2. While the Swift mission is primarily designed to follow gamma-ray bursts, the random distribution of bursts in the sky means that these survey's sky coverage is relatively uniform with the exposure at any point varying between about 6 to 16 megaseconds. The survey limits for source detection are about 10-11 ergs/s/cm2 over about half the sky and 1.3x10-11 ergs/s/cm2 over 90%.
These data replace the 9-month BAT datasets which we have retired. If you wish access to the older data please let us know. Note that for the 9-month data we provided access through the web page to the flux data and gave links to the signal-to-noise maps. Since the existence of sources is most easily seen in the SNR maps, we decided to invert that for this release.
For the 8 band data, the source data were provided by the BAT team as 6 FITS files. Each of these contained the 8 bands in separate image extensions for a region centered at l=0,b=+/-90 or l=0,90,180,270,b=0, the centers of 6 cubic facets. However these data are not the classical cube-faced projections, e.g., as used in COBE data. The data on the facets overlap, so that this is just a convenient way to tile the sky. SkyView separated each of the FITS image extensions into a separate file, but no other modifications were made to the data. The summed image was provided as six separate files. Provenance: NASA BAT Team. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=bat-flux-1&
TIMESTAMP = 1714845734177
ID = nasa.heasarc/skyview/cdfs-less
publisher_did = ivo://nasa.heasarc/skyview/cdfs-less
obs_collection = CDFS LESS
obs_title = LABOCA Extended Chandra Deep Field South Submillimetre Survey
obs_description = The LABOCA Extended Chandra Deep Field South (ECDFS) Submillimetre Survey (LESS) is a public legacy survey of the ECDFS at 870 ?m using the LABOCA camera (Siringo et al. 2009) on the APEX telescope.
The LABOCA data presented here were obtained between 2007 May and 2008 November in excellent conditions using time from both ESO and Max Planck allocations. The mapping pattern was designed to uniformly cover the 30'x30' extent of the ECDFS, centered on 03:32:29.0, -27:48:47.0 (J2000). The project used a total of 310 hrs of observations to achieve a beam-smoothed noise of 1.2 mJy/beam over 900 sq. arcmin (and <1.6mJy/beam over 1260 sq. arcmin). The flux calibration of the map came from observations of Mars, Uranus and Neptune (as well as secondary calibrators) and is accurate to within 8.5%. Provenance: Data downloaded from ESO archive. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=cdfs%20less&
TIMESTAMP = 1714845734569
ID = nasa.heasarc/skyview/cfhtls-d-u
publisher_did = ivo://nasa.heasarc/skyview/cfhtls-d-u
obs_collection = CFHTLS-D-u
obs_title = HIPS Survey:CFHTLS D u
obs_description = The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The Deep survey concerns 4 patchsof 1 square-degree. All will be observed in u,g,r,i and z, with very lon gexposure time
This survey description was generated automatically from the HiPS property file Provenance: CFHT
HiPS generated by CDS. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=cfhtls-d-u&
TIMESTAMP = 1714845734617
ID = nasa.heasarc/skyview/cfhtls-w-u
publisher_did = ivo://nasa.heasarc/skyview/cfhtls-w-u
obs_collection = CFHTLS-W-u
obs_title = HIPS Survey:CFHTLS W u
obs_description = The Canada-France-Hawaii Telescope Legacy Survey is a 5-year program carried out jointly by the Canadian and French agencies. It will use the Megaprime/Megacam instrument mounted at prime focus of the 3.6m CFH telescope during the period 2003-2008. The WIDE survey concerns 4 patchs, 3 of about 7x7 square-degrees each and 1 of about 4x4 square-degrees. All will be observed in u,g,r,i and z, with about 1 hr exposure time per filter
This survey description was generated automatically from the HiPS property file Provenance: CFHT
HiPS generated by CDS. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=cfhtls-w-u&
TIMESTAMP = 1714845734621
ID = nasa.heasarc/skyview/co
publisher_did = ivo://nasa.heasarc/skyview/co
obs_collection = CO
obs_title = CO Galactic Plane Survey
obs_description = New large-scale CO surveys of the first and second Galactic quadrants and the nearby molecular cloud complexes in Orion and Taurus, obtained with the Harvard-Smithsonian Center for Astrophysics 1.2 m telescope, have been combined with 31 other surveys obtained over the past two decades with that instrument and a similar telescope on Cerro Tololo in Chile, to produce a new composite CO survey of the entire Milky Way. The survey consists of 488,000 spectra that Nyquist or beamwidth (1/8 deg) sample the entire Galactic plane over a strip 4 deg-10 deg wide in latitude, and beamwidth or 1/4 deg sample nearly all large local clouds at higher latitudes. Compared with the previous composite CO survey of Dame et al. (1987), the new survey has 16 times more spectra, up to 3.4 times higher angular resolution, and up to 10 times higher sensitivity per unit solid angle.
Users should be aware that both the angular resolution and the sensitivity varies from region to region in the velocity-integrated map. The component surveys were integrated individually using clipping or moment masking in order to display nearly all statistically significant emission but little noise above a level of ~1.5 K km/s. See the reference below and the Millimeter-Wave Group site for more details Provenance: Data taken by two nearly-identical 1.2 m telescopes in Cambridge, MA and on Cerro Tololo, Chile combined into a complete survey of the Milky Way with CO integrated over all velocities.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=co&
TIMESTAMP = 1714845735157
ID = nasa.heasarc/skyview/cobe
publisher_did = ivo://nasa.heasarc/skyview/cobe
obs_collection = COBE
obs_title = Cosmic Background Explorer DIRBE Annual\ Average\ Map
obs_description = The DIRBE Project Data Sets cover the whole sky and provide photometric data in 10 bands ranging in wavelength from 1.25 to 240 microns. SkyView has supported three maps: an early averaged map including including zodiacal and Galactic components (COBE DIRBE (OLD)), a more recent cleaner version of that data (COBE DIRBE/AAM) and a map with the zodaical light subtracted out (COBE DIRBE/ZSMA). The early data is no longer supported. Please contact us if you want access to these data.
Detailed descriptions of the DIRBE, the data processing, and the data products are given in an Explanatory Supplement. A Small Source Spectral Energy Distribution Browser can be used to assess the visibility of an unresolved or small extended source in the DIRBE data and see its spectral energy distribution. As noted in section 5.6.6 of the Explanatory Supplement, the DIRBE Time-ordered Data are required to derive definitive point source fluxes.
These maps provide an estimate of the infrared intensity at each pixel and wavelength band based on an interpolation of the observations made at various times at solar elongations close to 90°;.
These COBE DIRBE maps are a combination original ten band passes with the following wavelengths:
- Band 1 - 1.25 µ;m
- Band 2 - 2.2 µ;m
- Band 3 - 3.5 µ;m
- Band 4 - 4.9 µ;m
- Band 5 - 12 µ;m
- Band 6 - 25 µ;m
- Band 7 - 60 µ;m
- Band 8 - 100 µ;m
- Band 9 - 140 µ;m
- Band 10 - 240 µ;m
The default two dimensional array uses Band 8 (100 µ;m).
The COBE DIRBE/Annual Average Maps (AAM) is the cumulative weighted average of the photometry. This average is calculated using the weighted number of observations from each Weekly Averaged Map ( WtNumObs from the Weekly Averaged Map) as the weight, such that annual_average =sum( weekly_average * weekly_weight )/ sum( weekly_weight )
COBE DIRBE/Zodi-Subtracted Mission Average (ZSMA) Skymap represents the extra-Solar system sky brightness. It is the average residual map that results after the modelled interplanetary dust (IPD) signal is subtracted from each of the DIRBE Weekly Skymaps from the cryogenic mission. Individual weekly residual maps can be reconstructed from the data supplied in the DIRBE Sky and Zodi Atlas (DSZA). Provenance: COBE Team. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=cobe&
TIMESTAMP = 1714845735161
ID = nasa.heasarc/skyview/comptel
publisher_did = ivo://nasa.heasarc/skyview/comptel
obs_collection = Comptel
obs_title = CGRO Compton Telescope: 3 channel data
obs_description = This survey is a maximum entropy solution to the data taken by the CompTel instrument on the Compton Gamma Ray Observatory. The data in this survey are intended only to give the general appearance of the MeV gamma-ray sky. Fluxes, flux limits and spectra should be derived using the Compass system for the analysis of CompTel data. Compass is available at the Compton Observatory Science Support Center .
The maps were originally generated by the CompTel Instrument Team as three separate maps in the bands:
- 1-3 MeV
- 3-10 MeV
- 10-30 MeV
All CompTel observations from phases 1, 2 and 3 were included in the maps (May 1991 through October 1994). These maps were combined into a single 3-D map at SkyView
Provenance: CompTel Instrument Team. Maps generated by Andrew Strong, Max-Planck Institute for Extraterrestrial Physics (Garching).. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = gamma-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=comptel&
TIMESTAMP = 1714845735177
ID = nasa.heasarc/skyview/dss
publisher_did = ivo://nasa.heasarc/skyview/dss
obs_collection = DSS
obs_title = Original Digitized Sky Survey
obs_description = This survey comprises the compressed digitization of the Southern Sky Survey and the Palomar Sky Survey E plates as distributed on CD ROM by the Space Telescope Science Institute. Coverage of the entire sky is included. This survey consists of the digititized Southern Sky Survey conducted at the UK Southern Schmidt Survey Group by the Royal Observatory, Edinburgh (prior to 1988) and the Anglo-Australian Observatory (since 1988) Additional plates covering regions with bright objects are also included. The plates were digitized at the Space Telescope Science Institute and compressed using algorithms developed by R.White. These data are distributed on a set of 101 CD-ROMs.
The following data are included:
- Southern hemisphere
- SERC Southern Sky Survey and the SERC J Equatorial extension. These are typically deep, 3600s, IIIa-J exposures with a GG395 filter. Also included are 94 short (1200s) V exposures typically at Galactic latitudes below 15°;. Special exposures are included in the regions of the Magellenic clouds.
- Northern hemisphere
- The northern hemisphere is covered by 644 plates from the POSS E survey. A special exposure of the M31 region that is distributed on the CD ROMs is not used in SkyView .
Provenance: Data taken by ROE and AAO, CalTech, Compression and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=dss&
TIMESTAMP = 1714845735557
ID = nasa.heasarc/skyview/dss1b
publisher_did = ivo://nasa.heasarc/skyview/dss1b
obs_collection = DSS1B
obs_title = First Digitized Sky Survey: Blue Plates
obs_description = This survey uses the POSS1 Blue plates. Provenance: Data taken by CalTech, Compression and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=dss1b&
TIMESTAMP = 1714845735561
ID = nasa.heasarc/skyview/dss1r
publisher_did = ivo://nasa.heasarc/skyview/dss1r
obs_collection = DSS1R
obs_title = First Digitized Sky Survey: Red Plates
obs_description = This survey is the POSS1 Red plates from the original POSS survey. It covers the sky north of -30 degrees declination. Provenance: Data taken by CalTech Compression and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=dss1r&
TIMESTAMP = 1714845735565
ID = nasa.heasarc/skyview/dss2
publisher_did = ivo://nasa.heasarc/skyview/dss2
obs_collection = DSS2
obs_title = 2nd Digitized Sky Survey (Blue)
obs_description = The native projection of these data is described as a high-order polynomial distortion of a gnomonic projection using the same terms as the DSS. Provenance: Data taken by ROE, AAO, and CalTech, Compression and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=dss2&
TIMESTAMP = 1714845735569
ID = nasa.heasarc/skyview/ebhis
publisher_did = ivo://nasa.heasarc/skyview/ebhis
obs_collection = EBHIS
obs_title = Effelsberg-Bonn HI Survey
obs_description = The Effelsberg-Bonn HI Survey (EBHIS) is a 21-cm survey performed with the 100-m telescope at Effelsberg. It covers the whole northern sky out to a redshift of z ~ 0.07 and comprises HI line emission from the Milky Way and the Local Volume. This dataset is the atomic neutral hydrogen (HI) column density map derived from the Milky-Way part of EBHIS (|Vlsr| < 600 km/s). Provenance: Argelander-Institut für Astronomie (AIfA) and Max-Planck-Institut für Radioastronomie (MPIfR); data provided by B. Winkel. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=ebhis&
TIMESTAMP = 1714845735609
ID = nasa.heasarc/skyview/egret
publisher_did = ivo://nasa.heasarc/skyview/egret
obs_collection = EGRET
obs_title = Energetic Gamma-Ray Event Telescope: Hard
obs_description = These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-100000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels.
The EGRET 3D map is comprised of ten channels with the following energy ranges:
- Channel 1 30-50 MeV
- Channel 2 50-70 MeV
- Channel 3 70-100 MeV
- Channel 4 100-150 MeV
- Channel 5 150-300 MeV
- Channel 6 300-500 MeV
- Channel 7 500-1000 MeV
- Channel 8 1000-2000 MeV
- Channel 9 2000-4000 MeV
- Channel 10 4000-10000 MeV
The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = gamma-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=egret&
TIMESTAMP = 1714845735621
ID = nasa.heasarc/skyview/egret3d
publisher_did = ivo://nasa.heasarc/skyview/egret3d
obs_collection = EGRET3D
obs_title = Energetic Gamma-Ray Event Telescope: 10 channel data
obs_description = These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-10000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels.
The EGRET 3D map is comprised of ten channels with the following energy ranges:
- Channel 1 30-50 MeV
- Channel 2 50-70 MeV
- Channel 3 70-100 MeV
- Channel 4 100-150 MeV
- Channel 5 150-300 MeV
- Channel 6 300-500 MeV
- Channel 7 500-1000 MeV
- Channel 8 1000-2000 MeV
- Channel 9 2000-4000 MeV
- Channel 10 4000-10000 MeV
The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = gamma-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=egret3d&
TIMESTAMP = 1714845735625
ID = nasa.heasarc/skyview/euve
publisher_did = ivo://nasa.heasarc/skyview/euve
obs_collection = EUVE
obs_title = Extreme Ultraviolet Explorer: 83 A
obs_description = The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include:
- Lexan/Boron filter: peak at 83A (full range 50-180)
- Aluminium/Carbon/Titanium : 171A (160-240)
- Aluminium/Titanium/Antimony: 405A (345-605)
- Tin/SiO: 555A (500-740)
The data currently in SkyView is direct from the Center for EUVE. Provenance: Center for Extreme UV Astronomy, UCB. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = uv
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=euve&
TIMESTAMP = 1714845735717
ID = nasa.heasarc/skyview/fermi
publisher_did = ivo://nasa.heasarc/skyview/fermi
obs_collection = FERMI
obs_title = Fermi Map: Band 1
obs_description = This survey sums all data observed by the Fermi mission up to week 396. This version of the Fermi survey are intensity maps where the summed counts data are divided by the exposure for each pixel (in cm^2 s) and the area of the pixel. Data is broken into 5 energy bands
- 30-100 MeV Band 1
- 100-300 MeV Band 2
- 300-1000 MeV Band 3
- 1-3 GeV Band 4
- 3-300 GeV Band 5
The SkyView data are based upon a Cartesian projection of the counts divided by the exposure maps. In the Cartesian projection pixels near the pole have a much smaller area than pixels on the equator, so these pixels have smaller integrated flux. When creating large scale images in other projections users may wish to make sure to compensate for this effect the flux conserving clip-resampling option. Provenance: Fermi LAT instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = gamma-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=fermi&
TIMESTAMP = 1714845735809
ID = nasa.heasarc/skyview/first
publisher_did = ivo://nasa.heasarc/skyview/first
obs_collection = FIRST
obs_title = FIRST
obs_description = The VLA FIRST (Faint Images of the Radio Sky at Twenty-centimeters) is a project designed to produce the radio equivalent of the Palomar Observatory Sky Survey over 10,000 square degrees of the North Galactic Cap. The FIRST home page has details of the instrumentation, status of the project, and data available. Currently about 5000 images of approximately .775x.58 degrees are available. These FIRST data have been retrieved from the FIRST FTP archive at the Space Telescope Science Institute.
The FIRST survey is included on the SkyView High Resolution Radio Coverage map. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. Provenance: The FIRST project team: R.J. Becker, D.H. Helfand, R.L. White
obs_description = M.D. Gregg. S.A. Laurent-Muehleisen.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=first&
TIMESTAMP = 1714845735905
ID = nasa.heasarc/skyview/galex
publisher_did = ivo://nasa.heasarc/skyview/galex
obs_collection = GALEX
obs_title = Galaxy Explorer All Sky Survey: Near UV
obs_description = The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682.
The SkyView GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image.
As of February 10, 2011, SkyView uses the GALEX GR6 data release. Provenance: All data is downloaded from the MAST GALEX archive.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = uv
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=galex&
TIMESTAMP = 1714845735981
ID = nasa.heasarc/skyview/gleam1
publisher_did = ivo://nasa.heasarc/skyview/gleam1
obs_collection = GLEAM1
obs_title = GLEAM 72-103: GaLactic and Extragalactic Allsky MWA Survey
obs_description = GLEAM, the GaLactic and Extragalactic All-sky MWA survey, is a survey of the entire radio sky south of declination 30 degrees at frequencies between 72 and 231 MHz. It was made with the Murchison Widefield Array (MWA) using a drift scan method that makes efficient use of the MWA's very large field-of-view. The survey is described in Wayth et al. (2015) and the website at https://www.mwatelescope.org/gleam.
The data presented here are from the first year of GLEAM observing, published in:
-
obs_description = Hurley-Walker et al. (2017): 25,000 square degrees of extragalactic sky
-
obs_description = For et al. (2018): the Large and Small Magellanic Clouds
-
obs_description = Hurley-Walker et al. (2019c): 8,000 square degrees of the Galactic plane
A region around Centaurus A, a few other small regions described by Hurley-Walker et al. (2017), and the Galactic plane between 180 < l < 345 degrees, are not available. The most sensitive and highest-resolution image is the 170-231MHz image which was used for all source-finding in generating the catalogue. It has a resolution of approximately 2.2 x 2.2/cos (dec + 26.7) arcmin at this frequency. However, due to ionospheric distortions, the final resolution of the survey varies by ~10% over the sky, with a direction-dependent PSF.
The SkyView data for the GLEAM surveys was extracted using the team's cutout server, into small (3 degree) raw cutouts over the region covered by the GLEAM survey. These cutouts have somewhat variable size and resolution. The default scale (i.e., pixel size) used for SkyView images is given in the table below. Since the GLEAM cutout server will not create an appropriately sized tile for the Sourth Pole, a larger tile offset from the pole is used.
SkyView resamples the cutouts retreived from the GLEAM website into the image geometry requested by the user. Only four wide-band datasets are included. The table below gives the frequency range, central frequency and a typical pixel scale for each of these bands.
| GLEAM Bands In SkyView |
|---|
| Band | fmin (MHz) | fmax (MHz) | fC (MHz) | Pixel scale (") |
|---|
| 1 | 72 | 103 | 88 | 56 |
| 2 | 103 | 134 | 118 | 44 |
| 3 | 138 | 170 | 155 | 34 |
| 4 | 170 | 231 | 200 | 28 |
These data and 20 narrower bands are available through the team website. To minimize resampling artifacts, this survey defaults to the Lanczos third order resampler. SkyView tracks the size and orientation of the beam as given in each of the tiles and includes the averaged value (i.e., the average of the input images weighted by the output pixels sampled from each input) in the BMAJ, BMIN, and BPA keywords of any result FITS file. Provenance: Source data extracted as cutouts from GLEAM cutout server in March 2020 with updates in July 2020.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=gleam1&
TIMESTAMP = 1714845736069
ID = nasa.heasarc/skyview/gns
publisher_did = ivo://nasa.heasarc/skyview/gns
obs_collection = GNS
obs_title = GOODS NICMOS Survey
obs_description = The GOODS NICMOS Survey (GNS) is a 180 orbit Hubble Space Telescope survey consisting of 60 pointings with the NICMOS-3 near-infrared camera. Each pointing is centred on a massive galaxy (M* > 1011 Msun) in the redshift range 1.7 < z < 3, selected by their optical-to-infrared colours (Papovich+06,Yan+04,Daddi+07) from the GOODS (Great Observatories Origins Deep Survey) fields.
The positions of the 60 GNS pointings were optimised to contain as many massive galaxies as possible and are partly overlapping, covering a total area of about 45 arcmin2. The field of view of the NICMOS-3 camera is 51.2 × 51.2 arcsec with a resolution of about 0.1 arcsec/pixel. The PSF has a width of about 0.3 arcsec FWHM. The limiting magnitude in H band reached at 5? is HAB = 26.8, about 2 magnitudes fainter than in available ground based data of the GOODS fields. [Taken from reference website.] Provenance: University of Nottingham, GNS group.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=gns&
TIMESTAMP = 1714845736185
ID = nasa.heasarc/skyview/goods-acs-b
publisher_did = ivo://nasa.heasarc/skyview/goods-acs-b
obs_collection = GOODS ACS B
obs_title = GOODS HST ACS B Filter
obs_description = This is a SkyView rendering of the HST ACS data as described in the release document. This comprises four bands of observations of each both the north and south GOODS regions.
These data are stored in SkyView as a hierarchical image with 7 levels of pixels, each with a factor of 2 change in scale. Thus the coarsest sampling using pixels 64 times larger than the finest. As we go to coarser pixels, 4 adjacent pixels forming a square are averaged to create the pixel in the next level. The coarsest pixel scale that is at least the resolution requested is used.
The exposure times are given as:
| GOODS ACS exposure (s) |
|---|
| Band | North> | South |
|---|
| z850 | 24760 | 18232 |
| i775 | 8530 | 7028 |
| V606 | 5650 | 5450 |
| B435 |
7200| 7200 |
Provenance: Created by the GOODS team and distributed by MAST. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goods%20acs%20b&
TIMESTAMP = 1714845736169
ID = nasa.heasarc/skyview/goods-isaac-h
publisher_did = ivo://nasa.heasarc/skyview/goods-isaac-h
obs_collection = GOODS ISAAC H
obs_title = Southern GOODS Field: VLT ISAAC Observations, H band
obs_description = As part of the Great Observatories Origins Deep Survey (GOODS), near-infrared imaging observations of the Chandra Deep Field South (CDF-S) were carried out in J, H, Ks bands, using the ISAAC instrument mounted at the Antu Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile. These data were obtained as part of the ESO Large Programme 168.A-0485 (PI: C. Cesarsky). Data covering four ISAAC fields in J and Ks bands were also drawn from the ESO programmes 64.O-0643, 66.A-0572 and 68.A-0544 (PI: E.Giallongo), which were part of the previous data releases.
This data release covers 172.4, 159.6, and 173.1 arcmin2 of the GOODS/CDF-S region in J, H and Ks respectively. More than 50% of the images reach a 5-sigma depth for point sources of at least 25.2 mag (J), 24.7 mag (H and Ks) in the AB system ("median depth").
This final GOODS/ISAAC data release accumulates observational data which have been acquired in 12814 science integrations between October 1999 and January 2007 totaling 1.3 Msec integration time. [Above adapted from reference website.]
SkyView uses the mosaic files provided in this delivery. The Version 1.5 mosaic is used for the KS band. Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goods%20isaac%20h&
TIMESTAMP = 1714845736181
ID = nasa.heasarc/skyview/goods-vimos-r
publisher_did = ivo://nasa.heasarc/skyview/goods-vimos-r
obs_collection = GOODS VIMOS R
obs_title = Southern GOODS Field: VLT VIMOS Observations, R band
obs_description = As part of the Great Observatories Origins Deep Survey (GOODS), deep imaging in the Chandra Deep Field South (CDF-S) has been carried out, using the VIMOS instrument mounted at the Melipal Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile.
This data release contains the coadded images in U band from the ESO large programme 168.A-0485 (P.I. C. Cesarsky) which have been obtained in service mode observations between August 2004 and fall 2006. The 1-sigma depth for VIMOS U band in the area covered by the GOODS-ACS observations is ~30 AB (within an aperture of 1" radius, ranging from 29.5 and 30.2 AB). The PSF of the VIMOS U band mosaic is ~0.8" FWHM, but varies over the field.
Also included in this data release is a coadded image in R band obtained from data retrieved from the ESO archive. Due to the different observing strategies adopted in the programmes the resulting coverage of the GOODS-ACS area is more complex than for the U band. The depth of the VIMOS R band mosaic over the ACS area ranges from ~28 AB to 29 AB (1-sigma, 1" aperture radius). The PSF of the VIMOS R band mosaic is ~0".7 FWHM and varies over the field. [Adapted from reference website.] Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goods%20vimos%20r&
TIMESTAMP = 1714845736189
ID = nasa.heasarc/skyview/goodsacisfb
publisher_did = ivo://nasa.heasarc/skyview/goodsacisfb
obs_collection = GOODSACISFB
obs_title = GOODS Chandra ACIS: Full band (0\.5\-8 keV)
obs_description = This survey comprises the 2 Ms Chandra Deep Field North and 4 Ms Deep Field South ACIS observations. All observations are co-added into two fields in the north and south. Data are provided in three bands, the soft 0.5-2 keV band, the hard 2.0-8.0 keV and the full 0.5 to 8 keV band. Provenance: Taken from the Neil Brandt's PSU websites for the the north and south.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsacisfb&
TIMESTAMP = 1714845736165
ID = nasa.heasarc/skyview/goodsherschel1
publisher_did = ivo://nasa.heasarc/skyview/goodsherschel1
obs_collection = GOODSHerschel1
obs_title = GOODS Herschel 100 micron, DR1 data release
obs_description = GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the Herschel Database in Marseille. Release DR1.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsherschel1&
TIMESTAMP = 1714845736169
ID = nasa.heasarc/skyview/goodsherschel2
publisher_did = ivo://nasa.heasarc/skyview/goodsherschel2
obs_collection = GOODSHerschel2
obs_title = GOODS Herschel 160 micron, DR1 data release
obs_description = GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the Herschel Database in Marseille. Release DR1.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsherschel2&
TIMESTAMP = 1714845736173
ID = nasa.heasarc/skyview/goodsherschel3
publisher_did = ivo://nasa.heasarc/skyview/goodsherschel3
obs_collection = GOODSHerschel3
obs_title = GOODS Herschel 250 micron, DR1 data release
obs_description = GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the Herschel Database in Marseille. Release DR1.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsherschel3&
TIMESTAMP = 1714845736173
ID = nasa.heasarc/skyview/goodsherschel4
publisher_did = ivo://nasa.heasarc/skyview/goodsherschel4
obs_collection = GOODSHerschel4
obs_title = GOODS Herschel 350 micron, DR1 data release
obs_description = GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the Herschel Database in Marseille. Release DR1.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsherschel4&
TIMESTAMP = 1714845736177
ID = nasa.heasarc/skyview/goodsherschel5
publisher_did = ivo://nasa.heasarc/skyview/goodsherschel5
obs_collection = GOODSHerschel5
obs_title = GOODS Herschel 500 micron, DR1 data release
obs_description = GOODS-Herschel is an open time key program of more than 360 hours of observation with the Hershel, SPIRE and PACS, from 100 um and 500.
North and South GOODS data is available for 100 and 160 microns (using PACS) but only the northern field is available at 250, 350 and 500 microns (using SPIRE).
Note that the scale and resolution of the underlying pixels is different in each band. Provenance: Downloaded from the Herschel Database in Marseille. Release DR1.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsherschel5&
TIMESTAMP = 1714845736177
ID = nasa.heasarc/skyview/goodsirac-1
publisher_did = ivo://nasa.heasarc/skyview/goodsirac-1
obs_collection = GOODSIRAC 1
obs_title = Spitzer IRAC GOODS 3\.6 micron data, channel 1
obs_description = Spitzer IRAC medium infrared observations taken in all four IRAC channels in both the north and south GOODS fields. Provenance: IRAC Goods Team, IRSA data center. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsirac%201&
TIMESTAMP = 1714845736181
ID = nasa.heasarc/skyview/goodsmips
publisher_did = ivo://nasa.heasarc/skyview/goodsmips
obs_collection = GOODSMIPS
obs_title = Spitzer MIPS GOODS 24 Micron Data
obs_description = Spitzer MIPS observations of the GOODS North and South fields in the 24 micron channel. Provenance: IRSA, GOODS team. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsmips&
TIMESTAMP = 1714845736185
ID = nasa.heasarc/skyview/goodsnvla
publisher_did = ivo://nasa.heasarc/skyview/goodsnvla
obs_collection = GOODSNVLA
obs_title = GOODS North Observations with the VLA
obs_description = A combination of VLA measurements in all four configurations combined to generate a very deep image of the GOODS North region. A total of about 150 hours of VLA time was used. Data are sensitive to about 5 microJanskies in the central region. A total of 1230 discrete sources where found in the 40'x40' region. Provenance: VLA Observations taken by Morrison et al. as provided through their website.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=goodsnvla&
TIMESTAMP = 1714845736189
ID = nasa.heasarc/skyview/granat
publisher_did = ivo://nasa.heasarc/skyview/granat
obs_collection = GRANAT
obs_title = GRANAT/SIGMA Significance
obs_description = The Soviet orbital observatory GRANAT was launched in December 1989 and was operational till November 1998. One of the main instruments of the observatory was the French-Soviet hard X-ray coded mask telescope SIGMA (Paul et al.1 1991, Adv.Space Res., 11, 279). It was the first space telescope that used coded aperture technique for reconstruction of sky images in hard X-rays (35-1300 keV). The angular resolution of the telescope was approximately 12' and the accuracy of a source localization is approximately 2-3'.
SIGMA discovered numerous interesting hard X-ray sources including GRS 1758-258, which is located only 40' from bright soft X-ray source GX 5-1. It detected hard X-ray flux from X-ray burster A1742-294, which is very near to bright black hole binary 1E1740.7-2942. SIGMA set an upper limit on the hard X-ray flux of from the central supermassive black hole in our Galaxy.
During the period 1990-1998 SIGMA observed more that one quarter of the sky with sensitivity better than 100 mCrab. The Galactic Center region had the deepest exposure ( approximately 9 million sec), with the sensitivity to a source discovery (S/N > ~ 5) or approximately 10 mCrab.
A list of all detected sources with references to publications on them is presented in the paper of Revnivtsev et al. 2004, Astr. Lett. v.6. In these survey images (40-100 keV) all performed observations are averaged together. Transient sources that were discovered by SIGMA may not visible in the averaged image.
This survey has some features that users should keep in mind. The SIGMA telescope is a complicated instrument and is strongly dominated by the accuracy of the background subtraction. The presence of a very bright source in the field of view of the telescope sometimes cannot be fully accounted for and as a result of it some 'ghost' sources can appear. Such features can be seen in the regions near very bright sources like Crab Nebula, Cyg X-1, Nova Per 1992, Nova Mus 1991, Nova Oph 1993, and in the Galactic Center region. In addition to its nominal field of view (~17x17 deg) located around the optical axis of the telescope, SIGMA had another window of relatively high transparency of its shield, approximately 20-30°; apart from the optical axis. Becuase of this a very bright sources like Cyg X-1 can cause non zero illumination of the SIGMA detector if they are located approximately 20-30°; from the optical axis. The ring-like features caused by this effect, can be seen around Cyg X-1, and Nova Per 1992.
The count rate of detected sources (or upper limits) can be roughly translated into mCrab using the fact that that Crab nebula gives the count rate approximately 2.8e-3 cnts/s in the units, provided in 'flux' maps Provenance: High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; CEA, Centre d'Etudes de Saclay Orme des Merisiers, France; Centre d'Etude Spatiale des Rayonnements, Toulouse, France; Fédération de Recherche Astroparticule et Cosmologie Université de Paris, France. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=granat&
TIMESTAMP = 1714845736209
ID = nasa.heasarc/skyview/gtee
publisher_did = ivo://nasa.heasarc/skyview/gtee
obs_collection = GTEE
obs_title = GTEE 0035 MHz Radio survey
obs_description = This survey is a mosaic of data taken at the low frequency T-array near Gauribidanur, India. The data was distributed in the NRAO Images from the Radio Sky CD ROM.
The original 287x101 tiles had only 1 pixel overlap. To allow higher order resampling, the data were retiled into two hemisphere files of 1726x600 pixels with an overlap of 10 pixels.
The southernmost tiles were only 287x100 pixels. We assumed that bottom row of these tiles (as compared with the others) was truncated. Provenance: . This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=gtee&
TIMESTAMP = 1714845736309
ID = nasa.heasarc/skyview/halpha
publisher_did = ivo://nasa.heasarc/skyview/halpha
obs_collection = HAlpha
obs_title = H-alpha Full Sky Map
obs_description = The full-sky H-alpha map (6' FWHM resolution) is a composite of the Virginia Tech Spectral line Survey (VTSS) in the north and the Southern H-Alpha Sky Survey Atlas (SHASSA) in the south. Stellar artifacts and bleed trails have been carefully removed from these maps. The Wisconsin H-Alpha Mapper (WHAM) survey provides a stable zero-point over 3/4 of the sky on a one degree scale. This composite map can be used to provide limits on thermal bremsstrahlung (free-free emission) from ionized gas known to contaminate microwave-background data. The map (in Rayleighs; 1R=106/4pi photons/cm2/s/sr), an error map, and a bitmask are provided in 8640x4320 Cartesian projections as well as HEALPIX (Nside 256, 512, and 1024) projections on the H-Alpha Full-Sky Map website. Provenance: . This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=halpha&
TIMESTAMP = 1714845736329
ID = nasa.heasarc/skyview/hawaii-hdf-b
publisher_did = ivo://nasa.heasarc/skyview/hawaii-hdf-b
obs_collection = Hawaii HDF B
obs_title = The Hawaii Hubble Deep Field North: Band B
obs_description = The Hawaii-HDF-N is an intensive multi-color imaging survey of 0.2 sq. degrees centered on the HDF-N. Data were collected on the NOAO 4m Mayall telescope, the National Astronomical Observatory of Japan 8.2m Subaru telescope and the University of Hawaii 2.2m telescope. Deep U, B, V, R, I, and z' data were obtained over the whole field and deep HK' data over the Chandra Deep Field North. Details are available in the references. [Adapted from reference website.]
Two different images are given in the V band (V0201 and V0401) from observations separated by about a month that had substantial differences in seeing. Provenance: Data downloaded from the reference website. A formatting error in the FITS files was corrected.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=hawaii%20hdf%20b&
TIMESTAMP = 1714845736333
ID = nasa.heasarc/skyview/heao1a
publisher_did = ivo://nasa.heasarc/skyview/heao1a
obs_collection = HEAO1A
obs_title = HEAO 1A
obs_description = These data were generated at the HEASARC in 1994. Certain gaps and streaks in the image have been fixed by interpolating over the the gap. Typically these gaps are no more than a pixel or two wide. A brief description of the satellite and the data analysis follows. The map used in SkyView is the map designated 322_15_tot_ecl_samp.img in the HEASARC FTP area. Many other maps are available. These differ in epoch, resolution, energy band, coordinate system and projection, and sampling methods. Details are given in the README file in the archive.
See Allen, Jahoda, and Whitlock (1994) for full details about the available maps, their processing, and methods for converting the map intensities into familiar physical units. Provenance: NASA, HEASARC. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=heao1a&
TIMESTAMP = 1714845736401
ID = nasa.heasarc/skyview/herschel-spire
publisher_did = ivo://nasa.heasarc/skyview/herschel-spire
obs_collection = HERSCHEL SPIRE
obs_title = Herschel Space Observatory - SPIRE
obs_description = The Herschel SPIRE survey is Provenance: HERSCHEL Project. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=herschel%20spire&
TIMESTAMP = 1714845736417
ID = nasa.heasarc/skyview/hi4pi
publisher_did = ivo://nasa.heasarc/skyview/hi4pi
obs_collection = HI4PI
obs_title = The HI 4-PI Survey
obs_description = The HI 4-PI Survey (HI4PI) is a 21-cm all-sky survey of neutral atomic hydrogen. It is constructed from the Effelsberg-Bonn HI Survey (EBHIS), made with the 100-m radio telescope at Effelsberg/Germany, and the Galactic All-Sky Survey (GASS), observed with the Parkes 64-m dish in Australia. HI4PI comprises HI line emission from the Milky Way. This dataset is the atomic neutral hydrogen (HI) column density map derived from HI4PI (|Vlsr| < 600 km/s). Provenance: Argelander-Institut für Astronomie (AIfA), Max-Planck-Institut für Radioastronomie (MPIfR), and CSIRO/Australia; data provided by B. Winkel. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=hi4pi&
TIMESTAMP = 1714845736465
ID = nasa.heasarc/skyview/hri
publisher_did = ivo://nasa.heasarc/skyview/hri
obs_collection = HRI
obs_title = ROSAT High Resolution Image Pointed Observations Mosaic: Intensity
obs_description = This survey was generated from all available ROSAT HRI observations. Data were mosaicked into 1.1 degree tiles by SkyView. Exposure maps were generated for each HRI observation using the hriexpmap FTOOL. For each tile, all observations that might contribute to that tile were located and added to count and exposure map tiles. Exposures for each observation were calculated using a nearest neighbor interpolation of the center of the tile pixels to the exposure map pixels. Counts were computed by projecting the RA and Decs of each eligible photon into the appropriate tile pixel. Only photons with a PHA > 3 were included in the mosaic and within each observation only counts within the region where the exposure was greater than half the maximum exposure were included. Provenance: Data from GSFC and MPE. SkyView mosaic generated by SkyView.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=hri&
TIMESTAMP = 1714845736601
ID = nasa.heasarc/skyview/hudfisaac
publisher_did = ivo://nasa.heasarc/skyview/hudfisaac
obs_collection = HUDFISAAC
obs_title = VLT ISAAC Ks Observations of the Southern Hubble Ultradeep Field
obs_description = A very deep Ks observation of the Hubble Ultradeep Field. This observation is approximately 0.6 magnitudes deeper than the GOODS ISAAC Ks image but covers only small fraction of the area. Provenance: Data downloaded from VLT archive. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=hudfisaac&
TIMESTAMP = 1714845736633
ID = nasa.heasarc/skyview/integralspi_gc
publisher_did = ivo://nasa.heasarc/skyview/integralspi_gc
obs_collection = INTEGRALSPI_gc
obs_title = INTEGRAL/Spectral Imager Galactic Center Survey
obs_description = The INTEGRAL observatory (Winkler et al. 2003, A&A, 411, L1) was launched in October 2002. The spectrograph SPI (Vedrenne et al. 2003, A&A, 411, L63) consists of 19 Germanium detectors and is capable of imaging in the 20 - 8000 keV band because of a coded mask. Part of the core program of the INTEGRAL mission is a study of the Galactic Centre, the Galactic Centre Deep Exposure (GCDE).
The SPI significance map is based on the public GCDE data and uses data in the 20 - 40 keV energy range. The analysis of the data was done using the SPIROS software (Skinner & Connell 2003, A&A, 411, L123). This software uses the 'Iterative Removal of Sources' technique in order to find the most significant sources. In the output significance map the sources found in this process are put on top of the residual map as points with a FWHM of 1 degree.
Current data respresent the combination of all public observations as of September 1, 2004. Provenance: INTEGRAL Science Data Center, Geneva, Switzerland. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=integralspi_gc&
TIMESTAMP = 1714845736785
ID = nasa.heasarc/skyview/intgal1735e
publisher_did = ivo://nasa.heasarc/skyview/intgal1735e
obs_collection = INTGAL1735E
obs_title = Nine Year INTEGRAL IBIS 17\-35 keV Galactic Plane Survey: Exposure
obs_description = This survey combines 9 years of INTEGRAL IBIS observations from December 2002 through January 2011 into a single Galactic Plane image. A total of 135 megaseconds of exposure is included in the observations used. Survey data is generated for the Galactic plane in the region |b| <= 17.5. The original flux data has been convolved with 5' seeing kernel. To minimize loss of resolution in transformations, the Lanczos sampler is suggested as the default, but may be overriden by the user. Both the preconvolved and standard convolved maps are available at the Website.
The exposure and sensitivity vary considerably over the coverage region, but 90% of the field has a limiting sensitivity better than 2.2 x 10-11ergs s-1cm-2 or about 1.56 mCrab. Further details of the survey construction are given in the reference.
The flux and significance maps use the PSF convolved maps from the survey. The flux maps are in millicrab units. Exposure maps (with exposures in seconds) were from the exposure extension in the MAPDLD files and give the dead-time corrected exposure in seconds.
Links to the exposure and significance maps corresponding to the requested region will be given in the Web output. These maps can be generated directly in the CLI interface. For each waveband the flux, significance and exposure maps are available with just the end of the survey names distinguishing them (e.g., INT Gal 17-35 [Flux|Sig|Exp] or INTGal1735[F|S|E]) Provenance: Krivonos et al., 2012
Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=intgal1735e&
TIMESTAMP = 1714845736789
ID = nasa.heasarc/skyview/iras
publisher_did = ivo://nasa.heasarc/skyview/iras
obs_collection = IRAS
obs_title = IRAS Sky Survey Atlas: 12 micron
obs_description = The IRAS data include all data distributed as part of the IRAS Sky Survey Atlas. Data from the four IRAS bands are shown as individual surveys in SkyView. Users should be aware that IPAC does not encourage the use of data near the ecliptic plane as they feel that contribution from local cirrus emission is significant.
The data are distributed in sets of 430 maps. Each map covers approximately 12.5x12.5 degrees, and the map centers are offset by 5 degrees so that there is a 2.5 degree overlap. IPAC has processed to a uniform standard so that excellent mosaics of the maps can be made. Users should be cautious of data in saturated regions. Known problems in the analysis mean that data values are unlikely to be correct. Note that IPAC has optimized the processing of these data for features of 5' or more although the resolution of the data is closer to the 1.5' pixel size.
There are occasional pixels in the IRAS maps which are given as NULL values. Unless these are explicitly trapped by user software, these data will appear as large negative values. SkyView ignores these pixels when determining the color scale to display an image.
Essentially the entire sky is covered by the survey. However there are a few regions not surveyed and the data values in these regions are suspect. These are given to users as delivered from IPAC. Provenance: NASA IPAC/Jet Propulsion Laboratory. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=iras&
TIMESTAMP = 1714845736969
ID = nasa.heasarc/skyview/iris
publisher_did = ivo://nasa.heasarc/skyview/iris
obs_collection = IRIS
obs_title = Improved Reprocessing of the IRAS Survey: 12
obs_description = The IRIS data is a reprocessing of the IRAS data set and has the same geometry as the IRAS Sky Survey Atlas (ISSA, labeled as IRAS nnn micron in SkyView) surveys. This new generation of IRAS images, called IRIS, benefits from a better zodiacal light subtraction, from a calibration and zero level compatible with DIRBE, and from a better destriping. At 100 micron the IRIS product is also a significant improvement from the Schlegel et al. (1998) maps. IRIS keeps the full ISSA resolution, it includes well calibrated point sources and the diffuse emission calibration at scales smaller than 1 degree was corrected for the variation of the IRAS detector responsivity with scale and brightness. The uncertainty on the IRIS calibration and zero level are dominated by the uncertainty on the DIRBE calibration and on the accuracy of the zodiacal light model.
More information about the IRIS dataset is available at the IRIS website whence most of the preceding description came. Provenance: Original IRAS data: NASA/JPL IPAC,
IRIS Reprocessing: Canadian Institute for Theoretical Astrophysics/Institut d'Astrophysique Spatiale
See the IRIS website.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=iris&
TIMESTAMP = 1714845736993
ID = nasa.heasarc/skyview/mellinger
publisher_did = ivo://nasa.heasarc/skyview/mellinger
obs_collection = MELLINGER
obs_title = Mellinger All Sky Mosaic: Red
obs_description = This all sky mosaic was created by Axel Mellinger and is used in SkyView with his permission. A fuller description is available at the survey website.
Between October 2007 and August 2009 a digital all-sky mosaic was assembled from more than 3000 individual CCD frames. Using an SBIG STL-11000 camera, 70 fields (each covering 40x27 degrees) were imaged from dark-sky locations in South Africa, Texas and Michigan. In order to increase the dynamic range beyond the 16 bits of the camera's analog-to-digital converter (of which approximately 12 bits provide data above the noise leve) three different exposure times (240s, 15s and 0.5 s) were used. Five frames were taken for each exposure time and filter setting. The frames were photometrically calibrated using standard catalog stars and sky background data from the Pioneer 10 and 11 space probes. the panorama has an image scale of 36"/pixel and a limiting magnitude of approximately 14. The survey has an 18 bit dynamic range.
The processing of these data used a custom data pipeline built using IRAF, Source Extractor and SWarp.
The data used here were converted to three independent RGB color planes of 8 bits each and provided to SkyView as a single 36000x18000x3 Cartesian projection cube. To allow users to efficiently sample data in a region of the sky, this cube was broken up into 2100x2100 pixel regions with a 50 pixel overlap between adjacent images. Tiles at the poles were 2100x2050.
In SkyView each color plane comprises a survey. The individual planes may be sampled as surveys independently as Mellinger-R, Mellinger-G and Mellinger-B. The color mosaics can be regenerated by creating an RGB image of all three surveys. Since SkyView may stretch the intensity values within each color, linear scaling and a minimum of 0 and maximum of 255 should be specified to keep the original intensity scalings.
The full spatial resolution data is used for images of less than 30 degrees on a side. If a user requests a larger region, data are sampled from a lower resolution 3600x1800x3 data cube. Please contact the survey author if you need to use the higher resolution data for larger regions. The Mellinger survey is only available in SkyView through the website. SkyView-in-a-Jar cannot access the underlying data. Provenance: Axel Mellinger. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=mellinger&
TIMESTAMP = 1714845738085
ID = nasa.heasarc/skyview/nh
publisher_did = ivo://nasa.heasarc/skyview/nh
obs_collection = nH
obs_title = Dickey and Lockman HI map
obs_description = This survey is derived from the 21cm maps presented by Dickey and Lockman in the ARAA 28, p215. The nH is derived assuming optically thin emission. The nH given should be considered a lower limit when the nH is greater than several times 1020. Provenance: provided by S. Snowden from data by Dickey and Lockman. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=nh&
TIMESTAMP = 1714845738985
ID = nasa.heasarc/skyview/nvss
publisher_did = ivo://nasa.heasarc/skyview/nvss
obs_collection = NVSS
obs_title = NRA) VLA Sky Survey
obs_description = SkyView has copied the NVSS intensity data from the NRAO FTP site. The full NVSS survey data includes information on other Stokes parameters.
Observations for the 1.4 GHz NRAO VLA Sky Survey (NVSS) began in 1993 September and should cover the sky north of -40 deg declination (82% of the celestial sphere) before the end of 1996. The principal data products are:
- A set of 2326 continuum map "cubes," each covering 4 deg X 4 deg with three planes containing Stokes I, Q, and U images. These maps were made with a relatively large restoring beam (45 arcsec FWHM) to yield the high surface-brightness sensitivity needed for completeness and photometric accuracy. Their rms brightness fluctuations are about 0.45 mJy/beam = 0.14 K (Stokes I) and 0.29 mJy/beam = 0.09 K (Stokes Q and U). The rms uncertainties in right ascension and declination vary from 0.3 arcsec for strong (S > 30 mJy) point sources to 5 arcsec for the faintest (S = 2.5 mJy) detectable sources.
- Lists of discrete sources.
The NVSS is being made as a service to the astronomical community, and the data products are being released as soon as they are produced and verified. The NVSS survey is included on the SkyView High Resolution Radio Coverage map. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates.
Provenance: National Radio Astronomy Observatory. The NVSS project includes J. J. Condon, W. D. Cotton, E. W. Greisen, Q. F. Yin, R. A. Perley (NRAO), and J. J. Broderick (VPI).. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=nvss&
TIMESTAMP = 1714845739061
ID = nasa.heasarc/skyview/planck857i
publisher_did = ivo://nasa.heasarc/skyview/planck857i
obs_collection = Planck857I
obs_title = Planck 857 GHz Survey: I
obs_description = Planck is ESA's third generation space based cosmic microwave background experiment, operating at nine frequencies between 30 and 857 GHz and was launched May 2009. Planck provides all-sky survey data at all nine frequencies with higher resolution at the 6 higher frequencies. It provides substantially higher resolution and sensitivity than WMAP. Planck orbits in the L2 Lagrange point.
These data come from the legacy Release 3 of the Planck mission.
These products include polarization information available to visualize in several ways. The data contain Stokes parameters I, Q, and U, and in addition to these, it is possible to visualize the polarized intensity PI=sqrt(Q^2+U^2) and the polarization angle PA=1/2atan(U/Q). Note that at their native resolution of a few arcmin (depending on the frequency), these polarization data will appear very noisy. In order to visualize the polarization information, it is highly recommended that the data be resampled with the "Clip (intensive)" sampler and the result smoothed. That sampler will average all the data points within a given output pixel rather than the more common nearest neighbor. It will do this averaging before computing either PI or PA to reduce the effects of the noise. This sampler is set as the default for this survey. If the output pixel resolution is not significantly larger than the resolution, a smoothing of the output pixels will also be necessary.
Note also that Q and U are defined relative to a given co-ordinate system, in this case Galactic, and following the CMB convention (not the IAU); see https://lambda.gsfc.nasa.gov/product/about/pol_convention.cfm. This means that they will appear to vary rapidly near the pole of that coordinate system. The PI and PA will be computed correctly for any position on the sky.
The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the HEALPix data. Users of the SkyView Jar will be able to access this survey through the web but performance may be poor since the FITS files are 150 to 600 MB in size and must be completely read in. SkyView will not automatically cache these files on the user machine as is done for non-HEALPix surveys.
Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'. Provenance: Data split using skyview.survey.HealPixSplitter from the PR3 distriuted by the Planck Science team.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = millimeter
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=planck857i&
TIMESTAMP = 1714845739409
ID = nasa.heasarc/skyview/pmn
publisher_did = ivo://nasa.heasarc/skyview/pmn
obs_collection = PMN
obs_title = 4850 MHz Survey - GB6/PMN
obs_description = The 4850MHz data is a combination of data from three different surveys: Parkes-MIT-NRAO (PMN) Southern (-88°; to -37°; declination) and tropical surveys (-29°; to -9°; declination, and (86+87) Green Bank survey (0°; to +75°; declination). The data contains gaps between -27°; to -39°;, -9°; to 0°;, and +77°; to +90°; declination. The 4850MHz survey data were obtained by tape from J.J. Condon and are comprised of 576 images and are used by permission. Full information pertaining to these surveys are found in the references. Provenance: NRAO, generated by J.J. Condon, J.J. Broderick and G.A. Seielstad, Douglas, K., and Gregory, P.C.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=pmn&
TIMESTAMP = 1714845732397
ID = nasa.heasarc/skyview/pspc0.6int
publisher_did = ivo://nasa.heasarc/skyview/pspc0.6int
obs_collection = PSPC0.6Int
obs_title = PSPC summed pointed observations, 0.6 degree cutoff, Intensity
obs_description = The ROSAT PSPC surveys were generated by SkyView as mosaics from publically available PSPC observations. The surveys include all data available through March 1, 1997. This includes the vast majority of ROSAT PSPC observations. Filter observations and observations taken during the verification phase in 1991 were not included in either set. The details of the generation of the surveys are discussed in a companion document. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two.
The smaller cut-offs allow users to distinguish point sources in fields where a bright source may have been towards the edge of one observation and near the center of another. In these cases the source appears fuzzy due to the poor resolution of ROSAT near the edge of the field of view. This comes at the cost of a substantial reduction in the fraction of the sky covered. Counts and exposure maps are included for users who may need this information (e.g., to do statistical analysis).
The global organization of the surveys is similar to the IRAS survey. Each map covers an area of 2.5°;x2.5°; with a minimum overlap of 0.25°;. To cover the entire sky would require over 10,000 maps. However due to lack of coverage only approximately 4000-6000 maps are actually populated. Users asking for reqions where there is no ROSAT coverage may get a blank region returned.
Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=pspc0.6int&
TIMESTAMP = 1714845739621
ID = nasa.heasarc/skyview/pspc1
publisher_did = ivo://nasa.heasarc/skyview/pspc1
obs_collection = PSPC1
obs_title = PSPC summed pointed observations, 1 degree cutoff, Intensity
obs_description = The ROSAT PSPC surveys were generated by SkyView as mosaics from publically available PSPC observations. The surveys include all data available through March 1, 1997. This includes the vast majority of ROSAT PSPC observations. Filter observations and observations taken during the verification phase in 1991 were not included in either set. The details of the generation of the surveys are discussed in a companion document. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two.
The smaller cut-offs allow users to distinguish point sources in fields where a bright source may have been towards the edge of one observation and near the center of another. In these cases the source appears fuzzy due to the poor resolution of ROSAT near the edge of the field of view. This comes at the cost of a substantial reduction in the fraction of the sky covered. Counts and exposure maps are included for users who may need this information (e.g., to do statistical analysis).
The global organization of the surveys is similar to the IRAS survey. Each map covers an area of 2.5°;x2.5°; with a minimum overlap of 0.25°;. To cover the entire sky would require over 10,000 maps. However due to lack of coverage only approximately 4000-6000 maps are actually populated. Users asking for reqions where there is no ROSAT coverage may get a blank region returned.
Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=pspc1&
TIMESTAMP = 1714845739613
ID = nasa.heasarc/skyview/pspc2
publisher_did = ivo://nasa.heasarc/skyview/pspc2
obs_collection = PSPC2
obs_title = PSPC summed pointed observations, 2 degree cutoff, Intensity
obs_description = The ROSAT PSPC surveys were generated by SkyView as mosaics from publically available PSPC observations. The surveys include all data available through March 1, 1997. This includes the vast majority of ROSAT PSPC observations. Filter observations and observations taken during the verification phase in 1991 were not included in either set. The details of the generation of the surveys are discussed in a companion document. Basically the counts and exposure from all observations were added and then an intensity map was generated as the ratio of the two.
The smaller cut-offs allow users to distinguish point sources in fields where a bright source may have been towards the edge of one observation and near the center of another. In these cases the source appears fuzzy due to the poor resolution of ROSAT near the edge of the field of view. This comes at the cost of a substantial reduction in the fraction of the sky covered. Counts and exposure maps are included for users who may need this information (e.g., to do statistical analysis).
The global organization of the surveys is similar to the IRAS survey. Each map covers an area of 2.5°;x2.5°; with a minimum overlap of 0.25°;. To cover the entire sky would require over 10,000 maps. However due to lack of coverage only approximately 4000-6000 maps are actually populated. Users asking for reqions where there is no ROSAT coverage may get a blank region returned.
Detailed information regarding the creation of the ROSAT suveys can be found in the ROSAT PSPC Generation Document. Provenance: Observational data from NASA Goddard Space Flight Center, mosaicking of images done by SkyView.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=pspc2&
TIMESTAMP = 1714845739617
ID = nasa.heasarc/skyview/rass3
publisher_did = ivo://nasa.heasarc/skyview/rass3
obs_collection = RASS3
obs_title = ROSAT All-Sky X-ray Survey Broad Band: Intensity
obs_description = The ROSAT All-Sky X-ray Survey was obtained during 1990/1991 using the ROSAT Position Sensitive Proportional Counter (PSPC) in combination with the ROSAT X-ray Telescope (XRT). More than 60,000 X-ray sources were detected during this time.
SkyView has multiple surveys derived from the RASS data. The surveys whose RASS are counts and exposure maps from the survey. Previously The RASSBCK maps have had the point sources removed to show the diffuse X-ray background and are presended at lower resolution.
The full-resolution RASS surveys data are organized in 1378 fields each 6.4°; x 6.4°; covering the whole sky. Neighboring fields overlap by at least 0.23°;.
Three bands are available through SkyView
- broad band (0.1-2.4 keV)
- hard band (0.5-2.0 keV)
- soft band (0.1-0.4 keV)
Data was dowloaded from the MPE FTP site. The intensity maps are created from the exposure maps using the single exposure map available which is appropriate for the broad band images, so the intensities of the hard and soft bands are only approximate. Provenance: Max Planck Institute for Exterrestrial Physics (Garching FRG). This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=rass3&
TIMESTAMP = 1714845739717
ID = nasa.heasarc/skyview/rassback
publisher_did = ivo://nasa.heasarc/skyview/rassback
obs_collection = RASSBACK
obs_title = ROSAT All-Sky X-ray Background Survey: Band 1
obs_description = These maps present maps of ROSAT soft X-ray all-sky survey as presented in Snowden et al, ApJ 485, 125 (1997). The maps cover approximately 98% of the sky. These maps have had all point sources removed These surveys supercede the RASS0.25, RASS0.75 and RASS1.5 Kev surveys previously provided. Those surveys may still be invoked in SkyView using batch and jar tools but are not accessible on the Web page.
The seven maps correspond to ranges in the pulse height analysis of the photons detected. Since the energy resolution of the PSPC is poor, there is consider overlap between adjacent bands.
The energy range for the bands corresponds to:
| Band | Energy range (keV) |
|---|
| Band 1 | 0.11 - 0.284 |
| Band 2 | 0.14 - 0.284 |
| Band 3 | 0.2 - 0.83 |
| Band 4 | 0.44 - 1.01 |
| Band 5 | 0.56 - 1.21 |
| Band 6 | 0.73 - 1.56 |
| Band 7 | 1.05 - 2.04 |
Note the substantial overlap between bands. Each photon detected is assigned to a band based on the pulse height analysis for that photon, but the energy resolution of the detectors is relatively poor. Also note that Band 3 was not included in the reference paper due to poor statistics and background modeling. SkyView has several other sets of surveys derived from ROSAT data with substantially higher resolution and which include point sources. The RASS surveys are derived from the RASS all sky survey. These include count and intensity maps. The PSPC maps are dervived from the PSPC pointed observations which were combined by SkyView. The HRI survey is derived from a similar mosaicking of all HRI observations. Provenance: Max Planck Institute for Exterrestrial Physics (Garching FRG). This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=rassback&
TIMESTAMP = 1714845739765
ID = nasa.heasarc/skyview/rxte3_20k_flux
publisher_did = ivo://nasa.heasarc/skyview/rxte3_20k_flux
obs_collection = RXTE3_20k_flux
obs_title = RXTE Allsky 3\-20 keV Flux
obs_description = Rossi X-ray Timing Explorer was launched at the end of 1995 and up to now (2004) it has been successfully operating for more than 7 years. The mission was primarily designed to study the variability of X-ray sources on time scales from sub-milliseconds to years. The maneuvering capability of the satellite combined with the high photon throughput of its main detector (PCA) and high quality of background prediction (thanks to PCA intrumental group of LHEA, GSFC) has also made it possible to construct maps of the sky in energy band 3-20 keV. During its life time RXTE/PCA has collected a large amount of data from slew observations covering almost the entire sky.
We have utilized the slew parts of all RXTE/PCA observations performed from April 15, 1996-July 16, 2002 which amounts in total to approximately 50,000 observations. The exposure time at a given point in the map is typically between 200-500 seconds. The observational period before April 15, 1996 (High Voltage Epochs 1 and 2) was excluded from the analysis because during that time the PCA had significantly different gain and dependence of the effective area on energy. The data reduction was done using standard tools of the LHEASOFT with a set of packages written by M. Revnivtsev (HEAD/IKI, Moscow; MPA, Garching).
The survey has several features. It has strongly different exposure times at different points on the sky that lead to strong variability of the statistical noise on images. Because of that the only meaningful representation of images is the map in units of statistical significance. After the detection of a source flux can be determined from the map in the 'flux' units. Map resolution is determined mainly by the slew rate of the RXTE (<0.05-0.1°;/sec) and the time resolution of used data (16 sec, Std2 mode of the PCA). Sources can be detected down to the level of ~6e-12 erg/s/cm2, but at this level the confusion starts to play an important role. Details of the survey are presented in the paper of Revnivtsev et al. (2004). Provenance: High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=rxte3_20k_flux&
TIMESTAMP = 1714845740357
ID = nasa.heasarc/skyview/sdss
publisher_did = ivo://nasa.heasarc/skyview/sdss
obs_collection = SDSS
obs_title = Sloan Digital Sky Survey g-band
obs_description = The Sloan Digital Sky Survey is the deepest large scale survey of the sky currently available. SkyView dynamically queries the SDSS archive (currently release DR9) to retrieve information and resample it into the user requested frame. Further information on the SDSS and many additional services are available at the SDSS website. Provenance: Sloan Digital Sky Survey Team. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=sdss&
TIMESTAMP = 1714845740729
ID = nasa.heasarc/skyview/sdssdr7
publisher_did = ivo://nasa.heasarc/skyview/sdssdr7
obs_collection = SDSSDR7
obs_title = Sloan Digital Sky Survey g-band DR7
obs_description = The Sloan Digital Sky Survey is the deepest large scale survey of the sky currently available. SkyView dynamically queries the SDSS archive to retrieve information and resample it into the user requested frame. Further information on the SDSS and many additional services are available at the SDSS website. Provenance: Sloan Digital Sky Survey Team. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=sdssdr7&
TIMESTAMP = 1714845740769
ID = nasa.heasarc/skyview/sfd
publisher_did = ivo://nasa.heasarc/skyview/sfd
obs_collection = SFD
obs_title = Schlegel, Finkbeiner and Davis dust\ map survey
obs_description = The full sky 100 micron map is a reprocessed composite of the COBE/DIRBE and IRAS/ISSA maps, with the zodiacal foreground and confirmed point sources removed. Artifacts from the IRAS scan pattern were removed. The result of these manipulations is a map with DIRBE-quality calibration and IR AS resolution. Provenance: David J. Schlegel, Douglas P. Finkbeiner and Marc Davis, Princeton University and University of California, Berkeley. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=sfd&
TIMESTAMP = 1714845740993
ID = nasa.heasarc/skyview/shassa
publisher_did = ivo://nasa.heasarc/skyview/shassa
obs_collection = SHASSA
obs_title = The Southern H-Alpha Sky Survey Atlas: Continuum
obs_description = The Southern H-Alpha Sky Survey Atlas is the product of a wide-angle digital imaging survey of the H-alpha emission from the warm ionized interstellar gas of our Galaxy. This atlas covers the southern hemisphere sky (declinations less than +15 degrees). The observations were taken with a robotic camera operating at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The atlas consists of 2168 images covering 542 fields. There are four images available for each field: H-alpha, Continuum, Continuum-Corrected (the difference of the H-alpha and Continuum images), and Smoothed (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The SHASSA website has more details of the data and the status of this and related projects. Images can also be obtained from the Download Images section at the SHASSA site. Provenance: John E. Gaustad (Swarthmore College), Peter R. McCullough (University of Illinois), Wayne Rosing (Las Cumbres Observatory), and Dave Van Buren (Extrasolar Research Corporation). This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=shassa&
TIMESTAMP = 1714845741037
ID = nasa.heasarc/skyview/skyview
publisher_did = ivo://nasa.heasarc/skyview/skyview
obs_collection = SkyView
obs_title = SkyView Virtual Observatory
obs_description = SkyView is a Virtual Observatory on the Net. Astronomers can generate images of any portion of the sky at wavelengths in all regimes from radio to gamma-ray. Users tell SkyView the position, scale and orientation desired, and SkyView gives users an image made to their specification. The user need not worry about transforming between equinoxes or coordinate systesm, mosaicking submaps, rotating the image,.... SkyView handles these geometric issues and lets the user get started on astronomy.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
obs_regime = infrared
obs_regime = optical
obs_regime = uv
obs_regime = x-ray
obs_regime = gamma-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?
TIMESTAMP = 1714845744989
ID = nasa.heasarc/skyview/stripe82vla
publisher_did = ivo://nasa.heasarc/skyview/stripe82vla
obs_collection = Stripe82VLA
obs_title = VLA Survey of SDSS Stripe 82
obs_description = This survey is a deep, high resolution radio survey of a relatively small region that has particularly deep coverage in the Sloan Digital Sky Survey. As described in the reference abstract: This is a high-resolution radio survey of the Sloan Digital Sky Survey (SDSS) Southern Equatorial Stripe, a.k.a., Stripe 82. This 1.4 GHz survey was conducted from 2007 to 2009 with the Very Large Array primarily in the A-configuration, with supplemental B-configuration data to increase sensitivity to extended structure. The survey has an angular resolution of 1.8" and achieves a median rms noise of 53 microJy/beam over 92 square degrees. This is the deepest 1.4 GHz survey to achieve this large of an area filling in the phase space between small&deep and large&shallow surveys.
The astrometric accuracy of the data is excellent with errors in observed sources of 0.10" in both RA and declination. A comparison with the SDSS DR7 Quasar Catalog confirms that the astrometry is well tied to the optical reference frame with mean offsets of 0.02+/-0.01" in RA and 0.01+/-0.02 in declination. Provenance: TBD. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=stripe82vla&
TIMESTAMP = 1714845741469
ID = nasa.heasarc/skyview/sumss
publisher_did = ivo://nasa.heasarc/skyview/sumss
obs_collection = SUMSS
obs_title = Sydney University Molonglo Sky Survey
obs_description = The Sydney University Molonglo Sky Survey (SUMSS) is a deep radio survey at 843 MHz of the entire sky south of declination -30°;, made using the Molonglo Observatory Synthesis Telescope ( MOST ), located near Canberra, Australia. The images from the SUMSS are produced as 4 x 4 degree mosaics of up to seventeen individual observations, to ensure even sensitivity across the sky. The mosaics slightly overlap each other. Data were last updated on January 28, 2015.
Images can also be obtained from the SUMSS Postage Stamp Server.
The SUMSS is intended to complement the NRAO-VLA Sky Survey (NVSS) which covered the sky between +90 and -40 deg declination, at a frequency of 1400MHz.
Provenance: The SUMSS project team, University of Sydney. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=sumss&
TIMESTAMP = 1714845741485
ID = nasa.heasarc/skyview/swiftuvot
publisher_did = ivo://nasa.heasarc/skyview/swiftuvot
obs_collection = SWIFTUVOT
obs_title = Swift UVOT Combined V Intensity Images
obs_description = The Swift UVOT instrument is a 30 cm modified Ritchey-Chretien reflecting telescope launched on board the Swift satellite on November 20, 2004. The range of optical and UV filters can accomodate wavebands between 1700 and 6500 Angstroms. A full field image covers 17x17 arcminutes and at maximum spatial sampling is imaged onto 2048x2048 0.5" pixels. A 1000 second observation can detect point sources to m=22.3 when no filter is used. The Swift Serendipitous Source Catalog (Page et al., 2015) detects sources down to m=23-26 for the six filters in very deep observations, but the typical limits are substantially brighter (~20-23 magnitude).
These surveys are mosaics of all Swift UVOT observations released between the start of the mission and July 2017. Data were extracted from the HEASARC archive from the UVOT products directory. Mosaics are provided in six filters and also with no filter, i.e., WHITE. The table below gives the number of observations and bandpasses for each of the filters. For each UVOT observation standard processing generates a counts and exposure file as a single multi-extension FITS file with a separate extension for each filter. To aid processing, these extensions were copied into separate files in directory trees for each filter. Four observations in which the exposure and counts maps did not agree on the filters used were omitted from the processing.
Some observations were recorded with 0.5" pixels while others were binned to 1". All 0.5" observations (typically fewer than 10%) were rebinned to the larger pixels for the counts maps since the counts data scales with the pixel size. Since the exposure values are intensive and do not vary significantly based upon the resolution, these data were not generally rebinned unless it was needed to ensure that Order 9 Hips data were produced.
The CDS Hipsgen software was used to generate Order 9 HiPS data (~0.8" pixels) for both the Counts and Exposure images. The HiPS (Hierarchical Progressive Survey VO standard) supports multi-resolution mosaics. Any quantitative use of these images should note that the rebinning increases the total counts by a factor of ~(1.0/0.8)^2 ~ 1.56. This software uses a bilinear interpolation to generate HEALPix tiles of an appropriate order (18 in this case). SkyView developed software was used to divide the level 9 counts maps tiles by the corresponding exposure maps to create intensity tiles. Pixels where the exposure was less than 5 seconds were left as NaNs. The lower order (8 to 3) order intensity tiles were then generated by averaging 2x2 sets of the higher order maps treating any missing maps or pixels as NaNs. A HiPS all-sky image was generated by averaged the Order 3 tiles.
Only the Intensity HIPS files are presented in the SkyView web page directly, but intensity, counts and exposure maps are available for all seven filters. Note that unlike the XRT HiPS data, the exposure and counts maps have not been clipped. I.e., the source FITS files have been aligned with the coordinate system and thus contain large numbers of unexposed pixels with 0 values. These 0's are simply propogated to HiPS tiles. NaNs are returned in regions which lie outside any of the original source images. For the Intensity map, any pixel for which the exposure was less than 5s is returned as a NaN.
| Filter | Count | Central Wavelength (Å;) | Bandpass (Å;) | Central Frequency(THz) | Bandpass (THz) | Coverage |
|---|
| WHITE | 3,000 | 3600 | 1600-6000 | 832 | 500-1874 | 0.0017 |
|---|
| V | 30,557 | 5468 | 5083-5852 | < 548 | 512-590 | 0.0171 |
|---|
| B | 28,347 | 4392 | 3904-4880 | 683 | 614-768 | 0.0112 | |
|---|
| U | 49,954 | 3465 | 3072-3875 | 865 | 774-975 | 0.0287 |
|---|
| UVW1 | 60,690 | 2600 | 2253-2946 | 1154 | 1017-1330 | 0.0277 |
|---|
| UVM2 | 56,977 | 2246 | 1997-2495 | 1334 | 1201-1501 | >td>0.0314
|---|
| UVW2 | 54,590 | 1928 | 1600-2256 | 1554 | 1328-1874 | 0.0260 |
|---|
Observation counts and bandpasses for UVOT Filters Provenance: Data generated from public images at HEASARC archive. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = uv
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=swiftuvot&
TIMESTAMP = 1714845741749
ID = nasa.heasarc/skyview/swiftxrt
publisher_did = ivo://nasa.heasarc/skyview/swiftxrt
obs_collection = SWIFTXRT
obs_title = Swift XRT Combined Intensity Images
obs_description = The Swift XRT (Burrows et al 2005, SSRv, 120, 165) is a sensitive, broad-band (0.2 - 10 keV) X-ray imager with an effective area of about 125 cm**2 at 1.5 keV. The 600 x 600 pixel CCD at the focus provides a 23.6' x 23.6' field of view with a pixel scale of 2.36". The point spread function is 18" (HPD) at 1.5 keV.
These XRT surveys represent the data from the first 12.5 years of Swift X-ray observations. They include all data taken in photon counting mode. A total of just over 8% of the sky has some non-zero exposure. The fraction of sky exposed as a function of the exposure is given in the following table:
| Exposure | >0 | 10 | 30 | 100 | 300 | 1000 | 3000 | 1000 | 30000 | 100000 | 300000 |
|---|
| Coverage | 8.42 | 8.37 | 8.29 | 7.67 | 7.29 | 5.68 | 3.40 | 1.26 | 0.35 | 0.044 | 0.00118 |
|---|
The individual exposure and counts maps have been combined into a Hierarchical Progressive Survey (HiPS) where the data are stored in tiles in the HEALPix projection at a number of different resulutions. The highest resolution pixels (HEALPix order 17) have a size of roughly 1.6". Data are also stored at lower resolutions at factors of 1/2, 1/4, 1/8, 1/16, and 1/32, and in an all sky image with a resolution 1/256 of the higest resolution. An intensity map has been created as the ratio of the counts and exposure maps. These surveys combine the basic count and exposure maps provided as standard products in the Swift XRT archive in obsid/xrt/products/*xpc_(sk|ex).img.gz. The surveys were created as follows:
- All of the exposure maps available in the archive in mid-May 2017 were combined using the CDS-developed Hipsgen tool. This includes 129,063 observations for which both count and exposure files were found in PC mode. Three exposures where there was a counts map but no exposure map were ignored. A few exposure files had more than one exposure extension. 1,082 files had two extensions and 1 file had 3 extensions. The 1084 HDUs in extensions were extracted as separate files and included in the total exposure. The value of 0 was given to the Hipsgen software as the null value for the FITS files. This caused the CDS software to treat such pixels as missing rather than 0 exposure.
- The counts data was extracted from the counts maps for each observation using SkyView developed software. For any pixel in which a count was recorded, the corresponding exposure file was checked and if there was any exposure (in any of the associated extensions), then the count was retained. If there was no exposure in any of the extensions of the corresponding exposure file, the counts in the pixel were omitted. Once a count was accepted, the overlap between the counts map pixel and the pixels of the corresponding HiPS tile (or tiles) was computed. Each count was then assigned entirely to a single pixel in the HiPS tile randomly but with the destination pixel probabilities weighted by area of the overlap. Thus if several pixels were found in a given counts map pixel they might be assigned to different pixels in the output image. The HiPS pixels (~1.6") used were of substantially higher resolution than the XRT resolution of 18" and somewhat higher than the counts map resolution of 2.36".
A total of 183,750,428 photons were extracted from the counts maps while 15,226 were rejected as being from pixels with 0 exposure. There were 501 pixels which required special treatment as straddling the boundaries of the HEALPix projection.
- The resulting counts tiles were then clipped using the exposure tiles that had been previously generated. Basically this transferred the coverage of the exposure tiles to the counts tiles. Any counts pixel where the corresponding exposure pixel was a NaN was changed to a NaN to indicate that there was no coverage in this region.
During the clipping process 137,730 HiPS level 8 were clipped (of 786,432 over the entire sky). There were 12,236 tiles for which there was some exposure but no counts found. During the clipping process 2 photons were found on pixels where there was no corresponding exposure in the exposure tiles. This can happen when the pixel assignment process noted above shifts a photon just outside the exposed region but should be -- as it was -- rare. These photons were deleted.
- After creating the clipped level 8 counts maps, level 7 to 3 tiles and an all sky map where generated by averaging pixels 2x2 to decrease each level. When adding the four pixels in the level N map together only pixels whose value was not NaN were considered.
- Finally an intensity map was created by dividing the counts tiles by the exposure tiles. To eliminate gross fluctuations due to rare counts in regions with very low exposure, only regions with exposure > 1 second were retained. A total of 30 photons were deleted due to this criterion.
Note that while any sampler may in principle be used with these data, the Spline sampler may give unexpected results. The spline computation propogates NaNs thought the image and means that even occasional NaNs can corrupt the output image completely. NaNs are very common in this dataset. Also, if the region straddles a boundary in the HEALPix projection, the size of the requested input region is likely to exceed memory limits since the HiPS data are considered a single very large image. Provenance: Data generated from public images at HEASARC archive. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = x-ray
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=swiftxrt&
TIMESTAMP = 1714845741777
ID = nasa.heasarc/skyview/tess
publisher_did = ivo://nasa.heasarc/skyview/tess
obs_collection = TESS
obs_title = HIPS Survey:Transiting Exoplanet Survey Satellite
obs_description = This is the TESS 2yr sky map. The Transiting Exoplanet Survey Satellite (TESS) is the next step in the search for planets outside of our solar system, including those that could support life. The mission will find exoplanets that periodically block part of the light from their host stars, events called transits. TESS will survey 200,000 of the brightest stars near the sun to search for transiting exoplanets. TESS aims for 50 ppm photometric precision on stars with TESS magnitude 9-15. TESS launched on April 18, 2018, aboard a SpaceX Falcon 9 rocket. This dataset is made of observations made during the first 2 years of the mission. See https://ui.adsabs.harvard.edu/abs/2015JATIS...1a4003R/abstract for more information on the mission. Funding for the TESS mission is provided by NASA's Science Mission directorate. Provenance: TESS Data were obtained by using the code provided by Ethan Kruse at https://github.com/ethankruse/tess_fullsky. HiPS generated by CDS. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = optical
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=tess&
TIMESTAMP = 1714845743329
ID = nasa.heasarc/skyview/tgss
publisher_did = ivo://nasa.heasarc/skyview/tgss
obs_collection = TGSS
obs_title = GMRT 150 MHz All-sky Radio Survey: First Alternative Data Release
obs_description = The first full release of a survey of the 150 MHz radio sky observed with the Giant Metrewave Radio Telescope between April 2010 and March 2012 as part of the TGSS project. Aimed at producing a reliable compact source survey, the automated data reduction pipeline efficiently processed more than 2000 hours of observations with minimal human interaction. Through application of innovative techniques such as image-based flagging, direction-dependent calibration of ionospheric phase errors, correcting for systematic offsets in antenna pointing, and improving the primary beam model, good quality images were created for over 95 percent of the 5336 pointings. This data release covers 36,900 square degrees (or 3.6 pi steradians) of the sky between -53 deg and +90 deg DEC, which is 90 percent of the total sky. The majority of pointing images have a background RMS noise below 5 mJy/beam with an approximate resolution of 25" x 25" (or 25" x 25" / cos (DEC - 19 deg) for pointings south of 19 deg DEC). The associated catalog has 640 thousand radio sources derived from an initial, high reliability source extraction at the 7 sigma level. The measured overall astrometric accuracy is better than 2" in RA and DEC, while the flux density accuracy is estimated at ~10 percent. Data is stored as 5336 mosaic images (5 deg x 5 deg).
SkyView uses Lanczos resampling and Sqrt image scaling by default for this survey. Provenance: TGS ADR Team. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=tgss&
TIMESTAMP = 1714845743373
ID = nasa.heasarc/skyview/ukidss
publisher_did = ivo://nasa.heasarc/skyview/ukidss
obs_collection = UKIDSS
obs_title = UKIRT Infrared Deep Survey J-band
obs_description = The UKIDSS survey is the next generation infrared survey, a successor to 2MASS. It will ultimately cover 7000 square degrees in the northern sky at both high and low Galactic latitudes and goes about three magnitudes deeper than 2MASS in the coverage area. Most data is taken in the J, H and K bands. A Y band is available in some regions.
UKIDSS is comprised of several distinct surveys in different regions of the sky. Of primary interest to SkyView users (since they have the largest sky coverage) are the Large Area Survey, the Galactic Plane Survey, and the Galactic Clusters Survey. There are deep and ultadeep surveys which cover much smaller fractions of the sky. The planned coverage for the UKIDSS surveys may be seen at the UKIDSS survey page. All UKIDSS data products are published by the Wide-Field Astronomy Unit (WFAU) at the University of Edinburgh through the WFCAM Science Archive (WSA) which includes more detailed coverage information for each data release.
SkyView currently uses the DR11 data release. Many thanks to the WSA team at WFAU for providing an interface to make all the latest data easily accessed. Note that coverage is not uniform across the different bands so that at a given point there might be H and K band data, but nothing in the J band. Provenance: UKIDSS Project. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=ukidss&
TIMESTAMP = 1714845743505
ID = nasa.heasarc/skyview/ultravista-h
publisher_did = ivo://nasa.heasarc/skyview/ultravista-h
obs_collection = UltraVista-H
obs_title = HIPS Survey:Ultradeep survey using the ESO Vista surveys telescope: Band H
obs_description = UltraVISTA is an Ultra Deep, near-infrared survey with the new VISTA surveys telescope of the European Southern Observatory (ESO). Over the course of 5 years, UltraVISTA will repeatedly image the COSMOS field in 5 bands covering a 1.5deg^2 field.\n \nESO acknowledgment: Data products from observations made with ESO Telescopes at the La Silla Paranal Observatories under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
This survey description was generated automatically from the HiPS property file Provenance: Origin unknown. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=ultravista-h&
TIMESTAMP = 1714845743653
ID = nasa.heasarc/skyview/vlss
publisher_did = ivo://nasa.heasarc/skyview/vlss
obs_collection = VLSS
obs_title = VLA Low-frequency Sky Survey
obs_description = The VLA Low-Frequency Sky Survey (VLSS) is a 74 MHz continuum survey covering the entire sky north of -30 degrees declination. Using the VLA in BnA and B-configurations, it will map the entire survey region at a resolution of 80" and with an average rms noise of 0.1 Jy/beam.
This version include the data from the VLSS redux which increased the coverage region slightly and substantially improved the data reduction. Details are in the Lane et al. (2012) reference. Provenance: VLSS Team: R.A. Perley, J.J. Condon, W.D. Cotton (NRAO); A.S. Cohen, W.M. Lane (NRC/NRL), N.E. Kassim, T.J.W. Lazio (NRL), W.C. Erickson (UMd). This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=vlss&
TIMESTAMP = 1714845744009
ID = nasa.heasarc/skyview/wenss
publisher_did = ivo://nasa.heasarc/skyview/wenss
obs_collection = WENSS
obs_title = Westerbork Northern Sky Survey
obs_description = The Westerbork Northern Sky Survey (WENSS) is a low-frequency radio survey that covers the whole sky north of delta=30 degree at a wavelength of 92 cm to a limiting flux density of approximately 18 mJy (5 sigma). This survey has a resolution of 54" x 54" cosec (delta) and a positional accuracy for strong sources of 1.5''.
Further information on the survey including links to catalogs derived from the survey is available at the WENSS website.
The WENSS survey is included on the SkyView High Resolution Radio Coverage map. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates.
Provenance: WENSS Team. Data downloaded from WENSS FTP site 1999-03-18. The WENSS project is a collaboration between the Netherlands Foundation for Research in Astronomy (NFRA/ASTRON) and the Leiden Observatory.. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = radio
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wenss&
TIMESTAMP = 1714845744153
ID = nasa.heasarc/skyview/wfcf
publisher_did = ivo://nasa.heasarc/skyview/wfcf
obs_collection = WFCF
obs_title = ROSAT Wide Field Camera: F1
obs_description = This survey is a mosaic of images taken by the ROSAT Wide Field Camera and comprises of 12,743 seperates fields in each of two filters. Each field covers a region 2.6°; x 2.6°; with a 0.3°; overlap. Currently, this data is not a complete coverage of the sky; regions near the northern ecliptic pole are currently not included. Provenance: University of Leicester. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = uv
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wfcf&
TIMESTAMP = 1714845744169
ID = nasa.heasarc/skyview/wise
publisher_did = ivo://nasa.heasarc/skyview/wise
obs_collection = WISE
obs_title = WISE 3\.4 Micron All-Sky Survey>: All-WISE data release
obs_description = From the WISE mission site:.
NASA's Wide-field Infrared Survey Explorer (WISE) mapped the sky at 3.4, 4.6, 12 and 22 micrometers in 2010 with an angular resolution of 6.1", 6.4", 6.5" and 12.0" in the four bands. WISE achieved a 5 sigma point source sensitivities better and 0.08, 0.11 1 and 6 mJy in unconfused regions on the ecliptic in the four bands. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodaical background. The WISE All-WISE includes all data taking during the WISE full cryogenic phase, from January 7, 2010 to August 6, 2010, that were processed with improved calibrations and reduction algorithms and combines this with the NEOWISE postcryogenic survey to form the most comprehensive view of the full mid-infrared sky. bibcode=1995ApJ...451..564V,2010ApJ...713..912W
SkyView includes the four WISE bands as separate surveys. Many non-image data products are available at the WISE site. Note that WISE data is distributed in relatively large (>50 MB) image files. When SkyView generates an image for a part of the sky where it has not yet cached the data from the IPAC server there may be a delay as full tiles are downloaded even when only a small fraction of a tile is needed. Images in cached regions, are generated much faster. Access to the WISE data uses the VO SIA interface maintained at IPAC. Even when data is cached, the SIA service must still be available for successful queries. Provenance: WISE Archive (IRSA/IPAC). This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wise&
TIMESTAMP = 1714845744201
ID = nasa.heasarc/skyview/wmap
publisher_did = ivo://nasa.heasarc/skyview/wmap
obs_collection = WMAP
obs_title = WMAP Nine Year Galaxy Removed
obs_description = These survey represents a combination of the 9-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body.
The original data are available at the LAMBDA archive. The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data.
Provenance: WMAP Mission/LAMBDA archive. This is a service of NASA HEASARC.
obs_description_url = https://skyview.gsfc.nasa.gov
obs_regime = infrared
sia_service_url = https://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wmap&
TIMESTAMP = 1714845744229
ID = nasa.heasarc/smc1400mhz
publisher_did = ivo://nasa.heasarc/smc1400mhz
obs_collection = SMC1400MHZ
obs_title = Small Magellanic Cloud ATCA and Parkes 1400-MHz Source Catalog
obs_description = This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains 1560 radio-continuum sources detected at 1400 MHz (lambda = 20 cm) from a set of new high-resolution radio-continuum mosaic images of the SMC created by combining observations from ATCA and Parkes (Wong et al. 2011, SerAJ, 182, 43). The 20 cm mosaic image (Fig. 2 in above reference)was created by combining data from ATCA project C1288 (Mao et al. 2008, ApJ, 688, 1029) with data obtained for a Parkes radio-continuum study of the SMC (Filipovic et al. 1997, A&AS, 121, 321). This image had a beam size of 17.8 x 12.2 arcseconds and an rms noise of 0.7 mJy/beam. The MIRIAD task 'imsad' was used to detect sources in the 20-cm image, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they were genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/183.103/ file tablea2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smc1400mhz.html
bib_reference = 2011SerAJ.183..103W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smc1400mhz&
tap_tablename = smc1400mhz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741173
ID = nasa.heasarc/smc4800mhz
publisher_did = ivo://nasa.heasarc/smc4800mhz
obs_collection = SMC4800MHZ
obs_title = Small Magellanic Cloud ATCA 4800-MHz Source Catalog
obs_description = This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains sources found at 4800 MHz (lambda = 6 cm) by combining data from various Australia Telescope Compact Array (ATCA) projects that covered the SMC. Some 601 sources have been detected at 6 cm in the new high-sensitivity and resolution radio-continuum image of the SMC from Crawford et al. (2011, SerAJ, 183, 95). The 6 cm map has a resolution of 30 arcseconds, and a sensitivity of 0.7 mJy/beam. The field size of the image used in this study covered from 00<sup>h</sup> 26<sup>m</sup> to 01<sup>h</sup> 28<sup>m</sup> in RA (J2000.0) and from -70<sup>o</sup> 29' to -75<sup>o</sup> 29' in Dec (J2000.0). The MIRIAD task 'imsad' was used to detect sources in the 6 cm image, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they are genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/184.93/ file tablea2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smc4800mhz.html
bib_reference = 2012SerAJ.184...93W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smc4800mhz&
tap_tablename = smc4800mhz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741185
ID = nasa.heasarc/smc843mhz
publisher_did = ivo://nasa.heasarc/smc843mhz
obs_collection = SMC843MHZ
obs_title = Small Magellanic Cloud MOST 843-MHz Source Catalog
obs_description = This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains 1689 radio-continuum sources detected at 843 MHz (lambda = 36 cm) from a radio survey of 36 square degrees containing the SMC (Turtle et al. 1998, PASA, 15, 280) conducted using the Molonglo Observatory Synthesis Telescope (MOST). These observations had a beam size of ~ 45 arcseconds and an rms noise of 0.7 mJy/beam. The MIRIAD task 'imsad' was used to detect sources in the 36-cm images, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they were genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/183.103/ file tablea3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smc843mhz.html
bib_reference = 2011SerAJ.183..103W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smc843mhz&
tap_tablename = smc843mhz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741193
ID = nasa.heasarc/smc8640mhz
publisher_did = ivo://nasa.heasarc/smc8640mhz
obs_collection = SMC8640MHZ
obs_title = Small Magellanic Cloud ATCA 8640-MHz Source Catalog
obs_description = This table contains a new catalog of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalog contains sources found at 8640 MHz (lambda = 3 cm) by combining data from various Australia Telescope Compact Array (ATCA) projects that covered the SMC. Some 457 sources have been detected at 3 cm in the new high-sensitivity and resolution radio-continuum image of the SMC from Crawford et al. (2011, SerAJ, 183, 95). The 3 cm map has a resolution of 20 arcseconds, and a sensitivity of 0.8 mJy/beam. The field size of the image used in this study covered from 00<sup>h</sup> 26<sup>m</sup> to 01<sup>h</sup> 27<sup>m</sup> in RA (J2000.0) and from -70<sup>o</sup> 35' to -75<sup>o</sup> 21' in Dec (J2000.0). The MIRIAD task 'imsad' was used to detect sources in the 3 cm image, requiring a fitted Gaussian flux density > 5 sigma (3.5 mJy). All sources were then visually examined to confirm that they are genuine point sources, excluding extended emission, bright side lobes, etc. This table was created by the HEASARC in September 2014 based on CDS Catalog J_other/Ser/184.93/ file tablea1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smc8640mhz.html
bib_reference = 2012SerAJ.184...93W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smc8640mhz&
tap_tablename = smc8640mhz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741253
ID = nasa.heasarc/smcclustrs
publisher_did = ivo://nasa.heasarc/smcclustrs
obs_collection = SMC/Clust
obs_title = SMC&BridgeClustersCatalog
obs_description = This is the Small Magellanic Cloud (SMC) and Inter-Magellanic Cloud ('Bridge') portion of the 'Revised and Extended Catalog of Magellanic System Clusters, Associations, and Emission Nebulae' (Table 2 of Bica and Schmitt 1995). A survey of extended objects in the SMC and Bridge was carried out on the ESO/SERC R and J Sky Survey Atlases and 1188 such objects were identified, including 544 classified as star clusters, 343 as emissionless associations, and 291 as emission nebulae. Only those objects which could be detected on the ESO/SERC Schmidt films as non-stellar (typically larger than 15 arcseconds) are included in this catalog, note. The catalog also includes cross-identifications with previous catalogs, and 284 newly identified objects. Accurate positions, classification, homogeneous sizes, and position angles are provided, as well as information on cluster pairs and hierarchical relations for superimposed objects. This database table was created by the HEASARC in February 1998 based on a computer readable version of the catalog that was obtained from the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/101/41">CDS catalog J/ApJS/101/41</a>. Additional information for the help documentation was obtained from the published version of this catalog (Bica and Schmitt 1995). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcclustrs.html
bib_reference = 1995ApJS..101...41B
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcclustrs&
tap_tablename = smcclustrs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741269
ID = nasa.heasarc/smcdfscxo
publisher_did = ivo://nasa.heasarc/smcdfscxo
obs_collection = SMCDFSCXO
obs_title = Small Magellanic Cloud Deep Fields X-Ray Point Source Catalog
obs_description = This table contains the results of a pair of 100 ks Chandra observations of the Small Magellanic Cloud (SMC) to survey high-mass X-ray binaries (HMXBs), stars, and low-mass X-ray binaries (LMXBs)/cataclysmic variables down to L<sub>X</sub> = 4.3 x 10<sup>32</sup> erg s<sup>-1</sup>. The two SMC Deep Fields (DFs) are located in the most active star-forming region of the SMC bar, with Deep Field-1 positioned at the most pulsar-rich location identified from previous surveys. Two new pulsars were discovered in outburst, CXOU J004929.7-731058 (P = 892 s) and CXOU J005252.2-721715 (P = 326 s), and three new HMXB candidates were identified. Of the 15 Be-pulsars now known in the field, 13 were detected, with pulsations seen in 9 of them. Ephemerides demonstrate that 6 of the 10 pulsars known to exhibit regular outbursts were seen outside their periastron phase, and quiescent X-ray emission at L<sub>X</sub> = 10<sup>(33-34)</sup> erg s<sup>-1</sup> is shown to be common. Comparison with ROSAT, ASCA, and XMM-Newton catalogs resulted in positive identification of several previously ambiguous sources. Bright optical counterparts exist for 40 of the X-ray sources, of which 33 are consistent with early-type stars (M<sub>V</sub> < -2, B-V < 0.2), and are the subject of a companion paper to the reference paper. The results point to an underlying HMXB population density up to double that of active systems. The full catalog of 394 point sources is presented in this table; detailed analyses of the source timing and spectral properties are available in the reference paper. The aim-points for these Chandra observations were as follows: DF1 had J2000.0 coordinates of 00 53 34.50 -72 26 43.2 and DF2 had J2000.0 coordinates of 00 50 41.40 -73 16 10.3. This table was created by the HEASARC in August 2010 based on the electronic version of Table 2 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcdfscxo.html
bib_reference = 2010ApJ...716.1217L
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcdfscxo&
tap_tablename = smcdfscxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741281
ID = nasa.heasarc/smcpscxmm
publisher_did = ivo://nasa.heasarc/smcpscxmm
obs_collection = SMCPSCXMM
obs_title = Small Magellanic Cloud XMM-Newton Point Source Catalog
obs_description = The XMM-Newton survey of the Small Magellanic Cloud (SMC) yielded complete coverage of the bar and eastern wing in the 0.2-12.0 keV energy band. In addition to the main-field (5.58 deg<sup>2</sup>), available outer fields were included in the catalogue, yielding a total field area of 6.32 deg<sup>2</sup>. This catalog comprises 3,053 unique X-ray point sources and sources with moderate extent that have been reduced from 5,236 individual detections found in 100 observations between April 2000 and April 2010 (the details of these exposures are given in Table B.1 of the reference paper). For 927 sources, there were detections at multiple epochs, with some SMC fields observed up to 36 times. The detected sources have a median position uncertainty of 1.3 arcseconds (1 sigma) and limiting fluxes down to ~1 x 10<sup>-14</sup> erg/s/cm<sup>2</sup> in the 0.2-4.5 keV band, corresponding to X-ray luminosities of ~5 x 10<sup>33</sup> erg/s for sources located in the SMC. Sources have been classified using X-ray hardness ratios, X-ray variability, and their multi-wavelength properties. In their paper, the authors discuss the statistical properties of the detected X-ray sources, like the spatial distribution, X-ray color diagrams, luminosity functions, and time variability. They have identified 49 SMC high-mass X-ray binaries (HMXB), four super-soft X-ray sources (SSS), 34 foreground stars, and 72 active galactic nuclei (AGN) behind the SMC. In addition, they found candidates for SMC HMXBs (45) and faint SSSs (8) as well as AGN (2092) and galaxy clusters (13). Notice that X-ray sources with high extent (>40 arcseconds), e.g. supernova remnants and galaxy clusters, have been previously presented by Haberl et al. (2012, A&A, 545, A128) and are not included in this table. To investigate the spectral behavior of all sources, the authors used hardness ratios HR<sub>i</sub> (i = 1, 2, 3, 4), defined by HR<sub>i</sub> = (R<sub>i+1</sub> - R<sub>i</sub>)/(R<sub>i+1</sub> + R<sub>i</sub>), where R<sub>i</sub> is the count rate in energy band i as defined by: <pre> Band Energy Range 1 0.2-0.5 keV 2 0.5-1.0 keV 3 1.0-2.0 keV 4 2.0-4.5 keV 5 4.5-12. keV </pre> To increase statistics, the authors also calculated average HR_i<sub>s</sub>, combining all available instruments and observations. HR<sub>i</sub> is not given if both rates R<sub>i</sub> and R<sub>i+1</sub> are null or if the 1-sigma uncertainty of Delta(HR<sub>i</sub>) covers the complete HR interval from -1 to +1. To convert an individual count rate R<sub>i</sub> of an energy band i into a setup-independent, observed flux F<sub>i</sub>, the authors calculated energy conversion factors (ECFs) f<sub>i</sub> = R<sub>i</sub>/F<sub>i</sub> , as described in Sect. A.3 of the reference paper. For the calculation, they assumed a universal spectrum for all sources, described by a power-law model with a photon index of 1.7 and a photo-electric foreground absorption by the Galaxy of N<sub>H,Gal</sub> = 6 x 10<sup>20</sup> cm<sup>-2</sup> (average for the SMC main field in the H I map of Dickey & Lockman 1990, ARAA, 28, 215). In addition to the fluxes for each detection, the authors calculated flux upper limits F<sub>UL</sub> for each observation and source, if the source was observed but not detected in an individual observation. As for the initial source detection, they used the emldetect task to fit sources, but kept the source positions fixed at the master positions and accepted all detection likelihoods in order to get an upper limit for the flux. This table was created by the HEASARC in October 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/558/A3">CDS Catalog J/A+A/558/A3</a> file smc_src.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcpscxmm.html
bib_reference = 2013A&A...558A...3S
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcpscxmm&
tap_tablename = smcpscxmm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741289
ID = nasa.heasarc/smcradio
publisher_did = ivo://nasa.heasarc/smcradio
obs_collection = SMCRadio
obs_title = Small Magellanic Cloud ATCA Radio Continuum Sources
obs_description = This table contains the classification of 717 radio-continuum sources from the Australia Telescope Compact Array (ATCA) Catalog of the Small Magellanic Cloud (SMC). All 717 sources have been categorised into one of three groups: supernova remnants (SNRs), HII regions and background sources. In total, 71 sources are named as HII regions (or candidates) and 21 sources are named as SNRs (or candidates). Six sources are named as either HII regions or background sources and two are candidate radio planetary nebulae. One source is coincident with an X-ray binary. 616 objects are classified as background sources and their statistics are presented in the published paper II from which this table is taken. This table was created by the HEASARC in March 2005 based on CDS table J/MNRAS/355/44/table2.dat . This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcradio.html
bib_reference = 2004MNRAS.355...44P
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcradio&
tap_tablename = smcradio
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741305
ID = nasa.heasarc/smcrosxray
publisher_did = ivo://nasa.heasarc/smcrosxray
obs_collection = PSPC/SMC
obs_title = ROSAT PSPC Survey of the Small Magellanic Cloud
obs_description = This catalog presents the results of a systematic search for point-like and moderately extended soft (0.1-2.4 keV) X-ray sources in a raster of nine pointings covering a field of 8.95 square degrees which was performed with the ROSAT PSPC between October 1991 and October 1993 in the direction of the Small Magellanic Cloud (SMC). 248 objects were detected and are included in this first version of the SMC catalog of soft X-ray sources. The authors set up seven source classes defined by selections in the count rate, hardness ratio and source extent parameters. They found five high luminosity super-soft sources (1E 0035.4-7230, 1E 0056.8-7146, RX J0048.4-7332, RX J0058.6-7146 and RX J0103-7254), one low-luminosity super-soft source RX J0059.6-7138 correlating with the planetary nebula L357, 51 candidate hard X-ray binaries including eight bright hard X-ray binary candidates, 19 supernova remnants (SNRs), 19 candidate foreground stars and 53 candidate background active galactic nuclei (and quasars). Likely classifications are given for about 60% of the catalogued sources. The total count rate of the detected point-like and moderately extended sources in the catalog is 6.9 +/- 0.3 counts s<sup>-1</sup>, comparable to the background subtracted total rate from the integrated field of about 6.1 +/- 0.1 counts s<sup>-1</sup>. This online catalog was created by the HEASARC in July 1999 based on tables obtained from the ADC/CDS data centers. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcrosxray.html
bib_reference = 1999A&AS..136...81K
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcrosxray&
tap_tablename = smcrosxray
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741317
ID = nasa.heasarc/smcrosxry2
publisher_did = ivo://nasa.heasarc/smcrosxry2
obs_collection = PSPC/SMC2
obs_title = ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al.)
obs_description = This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl & Pietsch (1999, A&AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10<sup>36</sup> erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. This database was created at the HEASARC in June 2000 based on the ADC/<a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+AS/142/41">CDS Catalog J/A+AS/142/41</a>, and is derived from Table 2 of the reference. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcrosxry2.html
bib_reference = 2000A&AS..142...41H
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcrosxry2&
tap_tablename = smcrosxry2
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741325
ID = nasa.heasarc/smcstars
publisher_did = ivo://nasa.heasarc/smcstars
obs_collection = SMCStars
obs_title = SMC Probable Member Stars Catalog
obs_description = An objective prism survey was conducted to discover probable members of the Small Magellanic Cloud. Interference filters were used to restrict the wavelength range and, hence, decrease the background and crowding. The limiting absolute magnitude of the survey is about -4.5. The 1975 paper listed 506 stars that show high luminosity characteristics; 193 of them had been confirmed by other authors. The 1979 paper added 14 additional probable members and photometric observations of 11 stars from the earlier paper that confirmed their membership. For completeness, four new Wolf-Rayet stars detected by Azzopardi and Breysacher (1979) were included. The catalog contains a catalog number in order of right ascension with the suffixes "a" or "b" used for the newer stars interpolated in the original list. Also included are the 1975 position, the MK spectral classification, the V magnitude, the (B-V) and (U-B) color indices, the number of observations, the identification chart number, and remarks indicating previous identifications. A later catalog of the Small Magellanic Could star members is also published by Azzopardi and Vigneau (1982A&AS...50..291A). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcstars.html
bib_reference = 1975A&AS...22..285A
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcstars&
tap_tablename = smcstars
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741337
ID = nasa.heasarc/smcstars2
publisher_did = ivo://nasa.heasarc/smcstars2
obs_collection = SMCSTAR2
obs_title = SMC H-Alpha Emission Stars/Nebulae
obs_description = This database table contains a list of H-alpha emission-line stars and small nebulae in the Small Magellanic Cloud (SMC) that were discovered in an objective-prism survey. This survey was performed through an H-alpha + [N II] interference filter using the 0.90m Curtis Schmidt telescope at Cerro Tololo Inter-American Observatory (CTIO). 1898 emission-line objects were detected in the main body of the SMC, almost quadrupling the number of those discovered in previous objective-prism surveys of the same region. Among these 1898 objects are newly discovered planetary nebulae, compact H II regions, and late-type stars. Continuum intensities, the shapes and strengths of the H-alpha emission line, co-ordinates and (where available) cross-identifications are provided for the listed objects. This version of the SMC H-alpha Emission-Line Stars and Small Nebulae Catalog of Meyssonnier and Azzopardi was created by the HEASARC in November 1997 based on the ADC/CDS machine-readable catalog J/A+AS/102/451. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcstars2.html
bib_reference = 1993A&AS..102..451M
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcstars2&
tap_tablename = smcstars2
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741345
ID = nasa.heasarc/smcwingcxo
publisher_did = ivo://nasa.heasarc/smcwingcxo
obs_collection = SMCWINGCXO
obs_title = Small Magellanic Cloud Wing Survey Chandra X-Ray Point Source Catalog
obs_description = The authors have detected 523 X-ray sources in a survey of the Small Magellanic Cloud (SMC) Wing with the Chandra X-ray Observatory. By cross-correlating the X-ray data with optical and near-infrared catalogs, they have found 300 matches. Using a technique that combines X-ray colors and X-ray to optical flux ratios, they have been able to assign preliminary classifications to 265 of the objects. The identifications include 4 pulsars, 1 high-mass X-ray binary (HMXB) candidate, 34 stars and 185 active galactic nuclei (AGN). In addition, the authors have classified 32 sources as hard AGN which are likely absorbed by local gas and dust, and 9 soft AGN whose nature is still unclear. Considering the abundance of HMXBs discovered so far in the Bar of the SMC the number that have been detected in the Wing is low. Observations in the Wing of the SMC were made from 2005 July to 2006 March with Chandra. The survey consisted of 20 fields, with exposure times ranging from 8.6 - 10.3 ks. X-ray parameters for 523 sources detected in the Wing of the SMC with Chandra are presented. For each source equatorial coordinates, positional error, net counts (total counts minus background counts) in the 0.5 - 8.0 keV band, signal-to-noise of the detection and source flux in the 0.5 - 8.0 keV band are given. The median, compressed median and normalized quartile ratio of the photon energy distribution, determined using quantile analysis, are given for sources with three or more counts. For the sources that have optical counterparts the V- and R-band magnitudes, B-V color, X-ray to optical flux ratios based on the V- and R-band magnitudes, and a preliminary classification for the sources are given. This table was created by the HEASARC in June 2008 based on the CDS Catalog J/MNRAS/383/330 file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcwingcxo.html
bib_reference = 2008MNRAS.383..330M
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcwingcxo&
tap_tablename = smcwingcxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741357
ID = nasa.heasarc/smcxray
publisher_did = ivo://nasa.heasarc/smcxray
obs_collection = Einstein/SMC
obs_title = SMC X-Ray Discrete Sources
obs_description = This database contains the 70 `discrete' (i.e., more compact than a few arc minutes) Einstein IPC X-ray sources in the direction of the Small Magellanic Cloud (SMC) that are tabulated in Table 2A of Wang & Wu (1992, ApJS, 78, 391). For full details about the data processing and selection criteria used to create the original source catalog, the above reference should be consulted. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smcxray.html
bib_reference = 1992ApJS...78..391W
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=smcxray&
tap_tablename = smcxray
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741369
ID = nasa.heasarc/smmgrs
publisher_did = ivo://nasa.heasarc/smmgrs
obs_collection = SMMGRS
obs_title = GRS Gamma-Ray Bursts
obs_description = The Gamma-Ray Spectrometer (GRS) was one of two instruments on the Solar Maximum Mission (SMM) which independently monitored cosmic gamma-ray bursts from SMM's launch in February 1980 until the end of the mission in 1989. The GRS was designed for investigation of the gamma-ray spectrum of solar flares (Forrest, D.J. et al. 1980, Sol. Phys., 65, 15). The main detector was an array of seven gain-controlled 7.6 cm diameter X 7.6 cm thick NaI(Tl) detectors. A complete spectrum was obtained every 16.38 seconds in the energy range 0.3-9 MeV. The number of counts in three energy windows covering the 4.2-6.4 MeV range was read out every 2.048 seconds. In addition, the number of counts in an approximately 50 keV wide window near 300 keV was read out every 64 milliseconds. The spectrometer was shielded by a 2.5 cm thick CsI(Na) annulus and a 25 cm diameter X 7.6 cm thick CsI(Na) back detector. The shield elements defined a field of view of approximately 135 degrees (FWHM) in the solar direction. The CsI back detector and the seven NaI detectors together provided a high-energy spectrometer with approximately 100 cm^2 effective area and four energy channels from 10 to 100 MeV. The number of counts in those high-energy channels was read out every 2.048 seconds. The experiment was complemented by two 8 cm^2 X 0.6 cm thick NaI(Tl) detectors which measured the X-ray portion of the spectrum every 1.024 seconds in the range from 13 keV to 182 keV. This database table was created by the HEASARC in the early 1990s based on tables supplied by the SMM Project and was subsequently revised in February 2002. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/smmgrs.html
obs_regime = gamma-ray
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
tap_tablename = smmgrs
TIMESTAMP = 1714845741373
ID = nasa.heasarc/snrgreen
publisher_did = ivo://nasa.heasarc/snrgreen
obs_collection = SNR(Green)
obs_title = Green Catalog of Galactic SNRs (June 2017 Version)
obs_description = This catalog of known Galactic supernova remnants (SNRs) is an updated version of the catalogs of Galactic SNRs presented in detail in Green (1984, 1988), in summary form in Green (1991, 1996, 2004, 2009), and on the Web (versions of 1995-July, 1996-August, 1998-September, 2000-August, 2001-December, 2004-January, 2006-April, 2009-March, and 2014-May). [Note that the version published in Green (1996) was produced in 1993.] This June 2017 version of the catalog contains 295 SNRs, and is based on results published in the literature up to the end of 2016. The basic summary data included in this catalog for each SNR are its designation, position, angular size (in arcminutes), type, flux density at 1 GHz, spectral index, and any other names by which it is known. Notes on these parameters, on possible remnants not included, and on questionable SNRs that are listed in this catalog, are given in the full version of the catalog on the Web at <a href="http://www.mrao.cam.ac.uk/surveys/snrs/snrs.info.html">http://www.mrao.cam.ac.uk/surveys/snrs/snrs.info.html</a> It should be noted that there are serious selection effects which apply to the identification of Galactic SNRs (e.g., Green 1991, 2004, 2005, 2009, 2014), so that care should be taken if these data are used in any statistical studies. This version of the Green Catalog of Galactic Supernova Remnants was ingested at the HEASARC in July 2017. It is based on the Catalogue of Galactic Supernova Remnants, 2017 June version, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/278">CDS Catalog VII/278</a>, file snrs.dat, obtained from the CDS at <a href="http://cdsarc.u-strasbg.fr/ftp/cats/VII/278/">http://cdsarc.u-strasbg.fr/ftp/cats/VII/278/</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/snrgreen.html
bib_reference = 2017yCat.7278....0G
obs_regime = optical
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=snrgreen&
tap_tablename = snrgreen
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741381
ID = nasa.heasarc/spass2p3gh
publisher_did = ivo://nasa.heasarc/spass2p3gh
obs_collection = SPASS2P3GH
obs_title = S-PASS (S-Band Polarization All-Sky Survey) 2.3-GHz Source Catalog
obs_description = The S-band Polarization All-Sky Survey (S-PASS) has observed the entire southern sky using the 64-meter Parkes radio telescope at 2.3 GHz with an effective bandwidth of 184 MHz. The surveyed sky area covers all Declinations < 0 degrees. To analyze compact sources the survey data have been re-processed to produce a set of 107 Stokes I maps with 10.75-arcminute resolution and the large scale emission contribution filtered out. In this paper, the authors use these Stokes I images to create a total intensity southern-sky extragalactic source catalog at 2.3 GHz. The source catalog contains 23,389 sources and covers a sky area of 16,600 deg<sup>2</sup>, excluding the Galactic plane for latitudes |b| < 10 degrees. Approximately 8% of the catalogued sources are resolved. S-PASS source positions are typically accurate to within 35 arcseconds. At a flux density of 225 mJy, the S-PASS source catalog is more than 95% complete, and ~94% of S-PASS sources brighter than 500 mJy/beam have a counterpart at lower frequencies. The observations were carried out over the period from October 2007 to January 2010 using the Parkes S-band receiver. The S-band receiver is a package with: a system temperature T<sub>sys</sub> = 20K, a beam Full Width at Half Maximum (FWHM) of 8.9 arcminutes, and a circular polarization front-end that is ideal for linear polarization observations with single-dish telescopes. This table was ingested by the HEASARC in August 2017 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/other/PASA/34.13">CDS catalog J/other/PASA/34.13</a> file s-pass.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/spass2p3gh.html
bib_reference = 2017PASA...34...13M
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=spass2p3gh&
tap_tablename = spass2p3gh
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TIMESTAMP = 1714845741393
ID = nasa.heasarc/spicescxo
publisher_did = ivo://nasa.heasarc/spicescxo
obs_collection = SPICESCXO
obs_title = SPICES Lynx Field Chandra X-Ray Source Catalog
obs_description = This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10<sup>-16</sup> erg/cm<sup>2</sup>/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K<sub>s</sub> = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K<sub>s</sub> >= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting non-transient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s<sup>-1</sup> per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin<sup>2</sup>. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N<sub>H</sub> = 2 x 10<sup>20</sup> cm<sup>-2</sup>. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H<sub>0</sub> = 50 h<sub>50</sub> km s<sup>-1</sup> Mpc<sup>-1</sup>, Omega<sub>M</sub> = 1, and Omega<sub>Lambda</sub> = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H<sub>0</sub> = 65 km s<sup>-1</sup> Mpc<sup>-1</sup>, Omega<sub>M</sub> = 0.35, and Omega<sub>Lambda</sub> = 0.65). This table was created by the HEASARC in April 2007 based on CDS catalog J/AJ/123/2223 files table1.dat, table2.dat and table3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/spicescxo.html
bib_reference = 2002AJ....123.2223S
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=spicescxo&
tap_tablename = spicescxo
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TIMESTAMP = 1714845741405
ID = nasa.heasarc/spidersros
publisher_did = ivo://nasa.heasarc/spidersros
obs_collection = SPIDERSROS
obs_title = SDSS-IV/SPIDERS ROSAT-Based X-Ray Point Source Spectroscopic Catalog
obs_description = This catalog aims to provide a detailed description of the SPectroscopic IDentification of ERosita Sources (SPIDERS) survey, an SDSS-IV program aimed at obtaining spectroscopic classification and redshift measurements for complete samples of sufficiently bright X-ray sources. The authors describe the SPIDERS X-Ray Point Source Spectroscopic Catalog, considering its store of 11,092 observed spectra drawn from a parent sample of 14,759 ROSAT and XMM sources over an area of 5,129 deg<sup>2</sup> covered in SDSS-IV by the eBOSS survey. This catalog presents the SPIDERS ROSAT subsample of 21,288 sources which were drawn from the Second ROSAT All-Sky Survey (2RXS), provided by the HEASARC in <a href="/W3Browse/rosat/rass2rxs.html">RASS2RXS</a>. The accompanying <a href="/W3Browse/xmm-newton/spidersxmm.html">SPIDERSXMM</a> table contains the 3,196 sources drawn from the XMM Slew Survey Source Catalog, version 2 (XMMSL2), provided by the HEASARC in <a href="/W3Browse/xmm-newton/xmmslewful.html">XMMSLEWFUL</a>. This program represents the largest systematic spectroscopic observation of an X-ray selected sample. A total of 10,970 (98.9%) of the observed objects are classified and 10,849 (97.8%) have secure redshifts. The majority of the spectra (10,070 objects) are active galactic nuclei (AGN), 522 are cluster galaxies, and 294 are stars. The SDSS-IV/BOSS spectrographic observations are taken between 2014 and 2019. This table was created by the HEASARC in May 2020 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/636/A97">CDS Catalog J/A+A/636/A97</a> file vc2rxs.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/spidersros.html
bib_reference = 2020A&A...636A..97C
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=spidersros&
tap_tablename = spidersros
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
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TIMESTAMP = 1714845741413
ID = nasa.heasarc/spidersxmm
publisher_did = ivo://nasa.heasarc/spidersxmm
obs_collection = SPIDERSXMM
obs_title = SDSS-IV/SPIDERS XMM-Based X-Ray Point Source Spectroscopic Catalog
obs_description = This catalog aims to provide a detailed description of the SPectroscopic IDentification of ERosita Sources (SPIDERS) survey, an SDSS-IV program aimed at obtaining spectroscopic classification and redshift measurements for complete samples of sufficiently bright X-ray sources. The authors describe the SPIDERS X-Ray Point Source Spectroscopic Catalog, considering its store of 11,092 observed spectra drawn from a parent sample of 14,759 ROSAT and XMM sources over an area of 5,129 deg<sup>2</sup> covered in SDSS-IV by the eBOSS survey. This catalog presents the SPIDERS XMM subsample of 3,196 sources which were drawn from the XMM Slew Survey source catalog, version 2 (XMMSL2), provided by the HEASARC in <a href="/W3Browse/xmm-newton/xmmslewful.html">XMMSLEWFUL</a>. The accompanying <a href="/W3Browse/rosat/spidersros.html">SPIDERSROS</a> table contains the 21,288 sources drawn from the Second ROSAT All-Sky Survey (2RXS) Source Catalog, available from the HEASARC as <a href="/W3Browse/rosat/rass2rxs.html">RASS2RXS</a>. This program represents the largest systematic spectroscopic observation of an X-ray selected sample. A total of 10,970 (98.9%) of the observed objects are classified and 10,849 (97.8%) have secure redshifts. The majority of the spectra (10,070 objects) are active galactic nuclei (AGN), 522 are cluster galaxies, and 294 are stars. The SDSS-IV/BOSS spectrographic observations are taken between 2014 and 2019. This table was created by the HEASARC in May 2020 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/636/A97">CDS Catalog J/A+A/636/A97</a> file vcxmmsl2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/spidersxmm.html
bib_reference = 2020A&A...636A..97C
obs_regime = x-ray
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=spidersxmm&
tap_tablename = spidersxmm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741437
ID = nasa.heasarc/spitzmastr
publisher_did = ivo://nasa.heasarc/spitzmastr
obs_collection = Spitzer
obs_title = Spitzer Space Telescope Observation Log
obs_description = This database table contains the Spitzer Space Telescope (SST) log of executed and scheduled observations, and is updated on a weekly basis. Spitzer is the fourth and final element in NASA's family of Great Observatories and represents an important scientific and technical bridge to NASA's Astronomical Search for Origins program. The SST Observatory carries an 85-cm cryogenic telescope and 3 cryogenically cooled science instruments capable of performing imaging and spectroscopy in the 3.6 to 160 micron (µm) range. Spitzer was launched on a Delta 7920H from Cape Canaveral into an Earth-trailing heliocentric orbit in August 2003. While the Spitzer cryogenic lifetime requirements are 2.5 years, current estimates indicate that achieving a goal of a 5-year cryogenic mission is possible. For more overview information, refer to the Spitzer Science Center (SSC) Overview at <a href="http://ssc.spitzer.caltech.edu/spitzermission/">http://ssc.spitzer.caltech.edu/spitzermission/</a>. The purpose of this HEASARC table is to help users, particularly those in the high-energy astronomy community, learn about which targets Spitzer has observed or will shortly observe. This table does not at this time have links from table entries to Spitzer data products. Once a particular Spitzer dataset of interest is identified, the SSC Archives/Analysis web page at <a href="http://ssc.spitzer.caltech.edu/archanaly/">http://ssc.spitzer.caltech.edu/archanaly/</a> should be used to access the dataset. The information in this table has been derived from the following files obtained from the SSC website: <p> The schedule of Spitzer science observations as executed: <pre> <a href="http://irsa.ipac.caltech.edu/data/SPITZER/docs/files/spitzer/spitzer_obslog.txt">http://irsa.ipac.caltech.edu/data/SPITZER/docs/files/spitzer/spitzer_obslog.txt</a> </pre> The list of all approved Spitzer science programs: <pre> <a href="http://irsa.ipac.caltech.edu/data/SPITZER/docs/files/spitzer/spitzer_programs.txt">http://irsa.ipac.caltech.edu/data/SPITZER/docs/files/spitzer/spitzer_programs.txt</a> </pre> Notice that this table contains primarily observations (identified by their AOR key value) from the first URL above. A given observation should appear only once in this HEASARC table. The HEASARC checks these URLs for modifications periodically and updates the table whenever changes are detected. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/spitzmastr.html
obs_regime = infrared
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=spitzmastr&
tap_tablename = spitzmastr
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741445
ID = nasa.heasarc/sporiabyso
publisher_did = ivo://nasa.heasarc/sporiabyso
obs_collection = SPORIABYSO
obs_title = Spitzer Survey of Orion A and B Molecular Clouds YSOs Catalog
obs_description = This table contains results from a survey of the Orion A and B molecular clouds undertaken with the IRAC and MIPS instruments on board Spitzer. In total, five distinct fields were mapped, covering 9 deg<sup>2</sup> in five mid-IR bands spanning 3 - 24 microns (um). The survey includes the Orion Nebula Cluster, the Lynds 1641, 1630, and 1622 dark clouds, and the NGC 2023, 2024, 2068, and 2071 nebulae. These data are merged with the Two Micron All Sky Survey point source catalog to generate a catalog of eight-band photometry. The authors identify 3479 dusty young stellar objects (YSOs) in the Orion molecular clouds by searching for point sources with mid-IR colors indicative of reprocessed light from dusty disks or in-falling envelopes. The YSOs are subsequently classified on the basis of their mid-IR colors and their spatial distributions are presented. The authors classify 2991 of the YSOs as pre-main-sequence stars with disks and 488 as likely protostars. Most of the sources were observed with IRAC in two to three epochs over six months; the authors search for variability between the epochs by looking for correlated variability in the 3.6 and 4.5 um bands. They find that 50% of the dusty YSOs show variability. The variations are typically small (~ 0.2 mag) with the protostars showing a higher incidence of variability and larger variations. The observed correlations between the 3.6, 4.5, 5.8, and 8 um variability suggests that we are observing variations in the heating of the inner disk due to changes in the accretion luminosity or rotating accretion hot spots. This table was created by the HEASARC in January 2013 based on an electronic version of Table 4 from the reference paper which was obtained from the AJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sporiabyso.html
bib_reference = 2012AJ....144..192M
obs_regime = infrared
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sporiabyso&
tap_tablename = sporiabyso
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741457
ID = nasa.heasarc/sptmm87sd
publisher_did = ivo://nasa.heasarc/sptmm87sd
obs_collection = SPTMM87SD
obs_title = South Pole Telescope 87-Square Degree Survey Millimeter Source Catalog
obs_description = This table contains the results of an 87 deg<sup>2</sup> point-source survey centered at RA = 5<sup>h</sup>30<sup>m</sup>, Dec = -55<sup>o</sup> (J2000.0) taken with the South Pole Telescope at 1.4 and 2.0 mm wavelengths with arcminute resolution and milli-Jansky (mJy) depth. Based on the ratio of flux in the two bands, the authors separate the detected sources into two populations, one consistent with synchrotron emission from active galactic nuclei (AGN) and the other consistent with thermal emission from dust. In the reference paper, the authors present source counts for each population from 11 to 640 mJy at 1.4 mm and from 4.4 to 800 mJy at 2.0 mm. The 2.0-mm counts are dominated by synchrotron-dominated sources across the reported flux range; the 1.4-mm counts are dominated by synchrotron-dominated sources above ~15 mJy and by dust-dominated sources below that flux level. The authors detect 141 synchrotron-dominated sources and 47 dust-dominated sources at signal-to-noise ratio S/N > 4.5 in at least one band. All of the most significantly detected members of the synchrotron-dominated population are associated with sources in previously published radio catalogs. Some of the dust-dominated sources are associated with nearby (z << 1) galaxies whose dust emission is also detected by the Infrared Astronomy Satellite (IRAS). However, most of the bright, dust-dominated sources have no counterparts in any existing catalogs. The authors argue that these sources represent the rarest and brightest members of the population commonly referred to as sub-millimeter galaxies (SMGs). During the 2008 observing season, the 960-element South Pole Telescope (SPT) camera included detectors sensitive to radiation within bands centered at approximately 1.4 mm, 2.0 mm, and 3.2 mm (220 GHz, 150 GHz, and 95 GHz). Result in this reference paper are based on 607 hr of observing time, using only the 1.4-mm and 2.0-mm data from the 87 deg<sup>2</sup> portion of the field that was mapped with near-uniform coverage. Main-lobe beams were measured using the brightest sources in the field and were adequately fit by two-dimensional Gaussians with FWHM equal to 1.05 and 1.15 arcminutes at 1.4 mm and 2.0 mm, respectively. The typical rms of the filtered 2.0-mm and 1.4-mm maps used for source candidate identification (shown in Figures 1 and 2, respectively, of the reference paper) is 1.3 mJy at 2.0 mm and 3.4 mJy at 1.4 mm. Detections in both bands are listed in the final catalog as a single source if they are offset <30 arcseconds between the two bands. For sources detected in both bands, the authors adopt the position of the more significant detection. The argue that they are far enough above the confusion limit that this simple and intuitive method is adequate. For sources detected in only one band, the authors use the flux in the cleaned map for the second band at the position of the detection. This table lists all 3,496 sources above 3 sigma in either map. This table was created by the HEASARC in October 2017 based on an electronic version of Table 5 from the reference paper which was obtained from the CDS as their catalog J/ApJ/719/763 file table5.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sptmm87sd.html
bib_reference = 2010ApJ...719..763V
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sptmm87sd&
tap_tablename = sptmm87sd
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741465
ID = nasa.heasarc/sptszgalcl
publisher_did = ivo://nasa.heasarc/sptszgalcl
obs_collection = SPTSZGALCL
obs_title = South Pole Telescope-Sunyarv-Zeldovich (SPT-SZ) Survey Catalog
obs_description = This table contains a catalog of galaxy clusters selected via their Sunyaev-Zel'dovich (SZ) effect signature from 2500 deg<sup>2</sup> of South Pole Telescope (SPT) data. This work represents the complete sample of clusters detected at high significance in the 2500 deg<sup>2</sup> SPT-SZ survey, which was completed in 2011. A total of 677 (409) cluster candidates are identified above a signal-to-noise threshold xi of 4.5 (5.0). Ground- and space-based optical and near-infrared (NIR) imaging confirms overdensities of similarly colored galaxies in the direction of 516 (or 76%) of the xi > 4.5 candidates and 387 (or 95%) of the xi > 5 candidates; the measured purity is consistent with expectations from simulations. Of these confirmed clusters, 415 were first identified in SPT data, including 251 new discoveries reported in this work. The authors estimate photometric redshifts for all candidates with identified optical and/or NIR counterparts; they additionally report redshifts derived from spectroscopic observations for 141 of these systems. The mass threshold of the catalog is roughly independent of redshift above z ~ 0.25 leading to a sample of massive clusters that extends to high redshift. The median mass of the sample is M<sub>500c</sub>(rho<sub>crit</sub>) ~ 3.5x10<sup>14</sup> M<sub>sun</sub> h<sub>70</sub><sup>-1</sup>, the median redshift is z<sub>med</sub> = 0.55, and the highest-redshift systems are at z > 1.4. The combination of large redshift extent, clean selection, and high typical mass makes this cluster sample of particular interest for cosmological analyses and studies of cluster formation and evolution. The South Pole Telescope (SPT) is a 10m diameter telescope located at the National Science Foundation Amundsen-Scott South Pole station in Antarctica. From 2008 to 2011 the telescope was used to conduct the SPT-SZ survey, a survey of ~ 2500 deg<sup>2</sup> of the southern sky at 95, 150, and 220 GHz. The survey covers a contiguous region from 20h to 7h in Right Ascension and -65 to -40 degrees in Declination (see, e.g., Figure 1 in Story et al. 2013, ApJ, 779, 86) and was mapped to depths of approximately 40, 18, and 70 microK-arcmin at 95, 150, and 220 GHz, respectively. The authors use optical and in some cases NIR imaging (Blanco Telescope, Magellan/Baade, Magellan/Clay, Swope, MPG/ESO, New Technology Telescope, Spitzer, WISE) to confirm candidates as clusters and to obtain redshifts for confirmed systems (see section 4 of the reference paper for more details). They have also used a variety of facilities to obtain spectroscopic observations of the SPT clusters (including VLT/FORS2 & Gemini/GMOS-S). This HEASARC table contains the total of 677 cluster candidates which were identified above a signal-to-noise threshold of xi = 4.5 in the 2500 deg<sup>2</sup> SPT-SZ survey. This table was created by the HEASARC in March 2015 based on an electronic version of Table 4 from the reference paper which was obtained from the CDS as their catalog J/ApJS/216/27 file table4.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sptszgalcl.html
bib_reference = 2015ApJS..216...27B
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sptszgalcl&
tap_tablename = sptszgalcl
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
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ID = nasa.heasarc/sptszspsc
publisher_did = ivo://nasa.heasarc/sptszspsc
obs_collection = SPTSZSPSC
obs_title = South Pole Telescope Sunyaev-Zeldovich Survey Point Source Catalog (2020)
obs_description = This database table presents the catalog of emissive point-sources detected in the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey, which is a contiguous 2530 deg<sup>2</sup> area surveyed between 2008-2011 in three bands centered at 95, 150, and 220 GHz. The catalog contains 4845 sources measured at a significance of 4.5 sigma or greater in at least one band, corresponding to detections above approximately 9.8, 5.8, and 20.4 mJy in 95, 150, and 220 GHz, respectively. Spectral behavior in the SPT bands is used for source classification into two populations based on the underlying physical mechanisms of compact, emissive sources that are bright at millimeter wavelengths: synchrotron radiation from active galactic nuclei and thermal emission from dust. The latter population includes a component of high-redshift sources often referred to as submillimeter galaxies (SMGs). In the relatively bright flux ranges probed by the survey, these sources are expected to be magnified by strong gravitational lensing. The survey also contains sources consistent with protoclusters, groups of dusty galaxies at high redshift undergoing collapse. The authors cross-match the SPT-SZ catalog with external catalogs at radio, infrared, and X-ray wavelengths and identify available redshift information. The catalog splits into 3980 synchrotron-dominated and 865 dust-dominated sources and determines a list of 506 SMGs. 10 sources are identified as stars. The SPT is a 10-m telescope located at the Amundsen-Scott South Pole station in Antarctica. At 150 GHz (2 mm), the SPT has arcminute angular resolution and a 1 deg<sup>2</sup> diffraction-limited field of view. The SPT was designed for high-sensitivity millimeter/sub-millimeter observations of faint, low-contrast sources, such as CMB anisotropies. The first survey with the SPT, designated as the SPT-SZ survey, was completed in 2011 November and covers a ~2500 deg<sup>2</sup> region of the southern extragalactic sky in three frequency bands, 95, 150, and 220 GHz, corresponding to wavelengths of 3.2, 2.0, and 1.4 mm. The fields were surveyed to depths of approximately 40, 18, and 70 microK arcmin at 95, 150, and 220 GHz, respectively. This study uses data from 19 fields observed by the SPT between 2008 and 2011. The fields are referred to using the J2000 coordinates of their centers, Right Ascension in hours and Declination in degrees. Table 1 in the reference paper lists the positions and effective areas of these fields.The total effective area used for the catalog and analysis in this present work is 2530 deg<sup>2</sup>. The catalog is an extension of two previous works: Vieira et al. (2010, ApJ, 719, 763) and Mocanu et al. (2013, ApJ, 779, 61) and builds on the same analysis pipeline, adding 1759 deg<sup>2</sup> of newly analyzed data, and additional data for two fields which were re-observed in 2010 and 2011. This table was originally created by the HEASARC in January 2014. It was updated to the 2020 version of this catalog in July 2020, based on a machine-readable catalog which was obtained from the <a href="https://lambda.gsfc.nasa.gov/product/spt/spt_everett2020_ps_catalog_info.cfm">LAMBDA</a> website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sptszspsc.html
bib_reference = 2020arXiv200303431E
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sptszspsc&
tap_tablename = sptszspsc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741497
ID = nasa.heasarc/ssa22cxo
publisher_did = ivo://nasa.heasarc/ssa22cxo
obs_collection = SSA22CXO
obs_title = SSA22 Field Chandra X-Ray Point Source Catalog
obs_description = This table contains the main X-ray point-source catalog for a deep ~400-ks Chandra ACIS-I (Advanced CCD Imaging Spectrometer) exposure of the SSA22 field. The observations were centred on a z = 3.09 protocluster, which is populated by Lyman break galaxies (LBGs), Lyman-alpha emitters (LAEs) and extended Lyman-alpha-emitting blobs (LABs). The survey reached ultimate (3 count) sensitivity limits of ~5.7 x 10<sup>-17</sup> and ~3.0 x 10<sup>-16</sup> erg cm<sup>-2</sup> s<sup>-1</sup> for the 0.5-2 and 2-8 keV bands, respectively (corresponding to L(2-10 keV) ~ 5.7 x 10<sup>42</sup> erg s<sup>-1</sup> and L(10-30 keV) ~ 2.0 x 10<sup>43</sup> erg s<sup>-1</sup> at z = 3.09, respectively, for an assumed photon index of Gamma = 1.4). These limits make SSA22 the fourth deepest extragalactic Chandra survey yet conducted, and the only one focused on a known high-redshift structure. In total, the authors detect 297 X-ray point sources and identify one obvious bright extended X-ray source (not included in the current table) over a ~330 arcmin<sup>2</sup> region. In addition to the X-ray data, the authors provide all available optical spectroscopic redshifts and near-infrared and mid-infrared photometry available for their sources. The basic X-ray and infrared properties of their Chandra sources indicate a variety of source types, although absorbed active galactic nuclei (AGN) appear to dominate. In total, they have identified 12 X-ray sources (either via optical spectroscopic redshifts or LAE selection) at z = 3.06 - 3.12 that are likely to be associated with the SSA22 protocluster. These sources have X-ray and multiwavelength properties that suggest they are powered by AGN with 0.5 - 8 keV luminosities in the range of ~ 10<sup>43</sup> - 10<sup>45</sup> erg s<sup>-1</sup>. The authors have analysed the AGN fraction of sources in the protocluster as a function of local LAE source density and find suggestive evidence for a correlation between AGN fraction and local LAE source density (at the ~96 per cent confidence level), implying that supermassive black hole growth at z ~3 is strongest in the highest density regions. This table was created by the HEASARC in February 2010 based on the electronic version of Table 2 from the reference paper which was obtained from the Monthly Notices web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/ssa22cxo.html
bib_reference = 2009MNRAS.400..299L
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=ssa22cxo&
tap_tablename = ssa22cxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741509
ID = nasa.heasarc/sss
publisher_did = ivo://nasa.heasarc/sss
obs_collection = SSS
obs_title = Einstein SSS Spectra and Lightcurves
obs_description = This table is the Einstein Solid State Spectrometer catalog of observations and data products. It incorporates the most recent ice model that is described in the article on the SSS calibration by Christian, Swank, and White that appeared in the HEASARC journal, Legacy, No. 1. Also available as "associated" data products are the quasi-simultaneous observations made by the Einstein Monitor Proportional Counter. There are 634 distinct SSS observations in this database, 95% of which have associated MPC data products. The remaining SSS observations cover time intervals in which all MPC data was flagged as bad by the pCHIP program that was used to generate the MPC spectra and lightcurves. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sss.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sss&
tap_tablename = sss
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741517
ID = nasa.heasarc/sssraw
publisher_did = ivo://nasa.heasarc/sssraw
obs_collection = SSSRAW
obs_title = Einstein SSS and MPC Raw Data
obs_description = The Einstein Observatory (also known as HEAO-2 or HEAO-B) was operational from 1978 November 13 until 1981 April 25 when the attitude control system failed. The Solid State Spectrometer (SSS) was operated intermittently between 1978 December 1 and 1979 October 22. However, the cryogen cooling for the detector was used up by about 2 weeks prior to the date of this last observation, so that the last reliable observation of the SSS is considered to have occurred on 1979 October 03. The SSSRAW database accesses the raw SSS data (and the associated monitoring proportional counter, MPC, data), restored in FITS format at HEASARC from the original machine dependent format data set. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sssraw.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sssraw&
tap_tablename = sssraw
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741529
ID = nasa.heasarc/sterngrb
publisher_did = ivo://nasa.heasarc/sterngrb
obs_collection = Stern
obs_title = Stern et al. (2001) BATSE Gamma-Ray Burst Catalog
obs_description = The Stern et al. (2001) BATSE Gamma-Ray Burst (GRB) Catalog was constructed by scanning the archival BATSE daily records (DISCLA data) covering the entire 9.1 years of BATSE's operation. 3906 GRBs were detected, 2068 of which are previously known BATSE triggers while 1838 of them are new non-triggered bursts. All events were detected in the same kind of data with 1.024 seconds time resolution and were processed with the same procedure, and thus constitute a uniform sample. This scan lowers the BATSE detection threshold to ~0.1 photons/s/cm**2. This database table was created at the HEASARC in August 2001 using the file <a href="ftp://ftp.astro.su.se/pub/head/grb/catalogs/etable2.txt">ftp://ftp.astro.su.se/pub/head/grb/catalogs/etable2.txt</a> on the Stockholm Observatory ftp site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sterngrb.html
bib_reference = 2001ApJ...563...80S
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sterngrb&
tap_tablename = sterngrb
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741537
ID = nasa.heasarc/subpfclog
publisher_did = ivo://nasa.heasarc/subpfclog
obs_collection = SubaruPFC
obs_title = Subaru Prime Focus Camera (Suprime-Cam) Exposures Log
obs_description = This table contains the Subaru Prime Focus Camera (Suprime-Cam) log of exposures having observation type = 'OBJECT' (those with 'BIAS', 'FLAT' and other types are not included) which have been made since April 2001. Note that from the version of Nov. 2005 on, the number of rows has significantly increased because those data with worse position determination (up to 30 arcsec error) are now included. The data currently extend to November 2005 and it is anticipated that they will be regularly updated Suprime-Cam is an 80-mega pixels (10240 x 8192) mosaic CCD camera, for the wide-field prime focus of the 8.2m Subaru telescope. Suprime-Cam covers a field of view 34' x 27', a unique facility among the 8-10m class telescopes, with a resolution of 0.202 arcseconds per pixel. The focal plane consists of ten high-resistivity 2kx2k CCDs developed by MIT Lincoln Laboratory, which are cooled by a large Stirling-cycle cooler. The CCD readout electronics was designed to be scalable, which allows the multiple read-out of tens of CCDs. It takes 50 seconds to readout entire arrays. A filter-exchange mechanism of the jukebox type is designed that can hold up to ten large filters (205 x 170 x 15 mm<sup>3</sup>). The wide-field corrector is basically a three-lens Wynne-type, but has a new type of atmospheric dispersion corrector. The corrector provides a flat focal plane and an un-vignetted field of view of 30' in diameter. The achieved co-planarity of the focal array mosaic is smaller than 30 um peak-to-peak, which realizes mostly the seeing limited image over the entire field. The median seeing in the I_c-band, measured over one year and a half, is 0.61 arcseconds. The PSF anisotropy in Suprime-Cam images, estimated by stellar ellipticities, is about 2% under this median seeing condition. At the time of its commissioning, Suprime-Cam had the largest survey speed, which is defined as the field of view multiplied by the primary mirror area of the telescope, among those cameras built for sub-arcsecond imaging. For more details, see: Miyazaki et al., Publ. Astron. Soc. Japan 54, 833-853, 2002 (2002PASJ...54..833M). This table was created by the HEASARC in September 2007 based on CDS table B/subaru/suprimc.dat (the ReadMe file for the latter was tagged with a date of August 25th, 2007). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/subpfclog.html
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=subpfclog&
tap_tablename = subpfclog
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741549
ID = nasa.heasarc/sumss
publisher_did = ivo://nasa.heasarc/sumss
obs_collection = SUMSS
obs_title = Sydney University Molonglo Sky Survey (SUMSS) Source Catalog
obs_description = The Sydney University Molonglo Sky Survey (SUMSS) is a radio imaging survey of the sky south of declination, delta = -30 degrees (a total area of 8100 square degrees) carried out with the Molonglo Observatory Synthesis Telescope (MOST) operating at 843 MHz. The survey consists of 629 4.3 degrees by 4.3 degrees mosaic images with a resolution of 45" by 45" x cosec delta, and a limiting peak brightness of 6 mJy/beam at declinations delta <= 50 degrees, and 10 mJy/beam at delta > 50 degrees. The SUMSS is therefore similar in sensitivity and resolution to the northern NRAO VLA Sky Survey (NVSS). This table based on the latest version of the SUMSS Source Catalog of radio sources (which uses all of the released mosaics). Sources were found by fitting two-dimensional Gaussians to SUMSS mosaics. Positions in the catalog are accurate to within 1-2" for sources with peak brightness >= 20 mJy/beam, and are always better than 10". The internal flux density scale is accurate to within 3%. Image artifacts were classified using a decision tree, which correctly identified and rejected spurious sources in over 96% of cases. Analysis of the catalog shows that it is highly uniform and is complete to 8 mJy at delta <= -50 degrees, and to 18 mJy at delta > -50 degrees. This HEASARC table was initially created in August 2005. It is updated automatically within a week of any detected change to the SUMSS Source Catalog as obtained from the SUMSS Website at the following URL: <pre> <a href="http://www.astrop.physics.usyd.edu.au/sumsscat/update">http://www.astrop.physics.usyd.edu.au/sumsscat/update</a> </pre> This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sumss.html
bib_reference = 2003MNRAS.342.1117M
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sumss&
tap_tablename = sumss
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741561
ID = nasa.heasarc/suzakuwam
publisher_did = ivo://nasa.heasarc/suzakuwam
obs_collection = SUZAKUWAM
obs_title = Suzaku Wide-Band All-Sky Monitor (WAM) Catalog of Event Lightcurves
obs_description = This database table contains information of the events detected by the Wide-band All-sky Monitor (WAM) on Suzaku during its ~10 years of operation. Each event has associated data products. The lightcurves are derived from the on-board operating modes that collected the WAM data from each of the sub-detectors. The lightcurves are rates as a function of time in different energy bands, and they can be used with the general FITS tools within HEAsoft or XRONOS. Version 3 of the lightcurves were generated at HEASARC from the version 2 files, and they are now the final versions hosted at both HEASARC and DARTS. This database table reflects version 3 of the data products. <p> Version 2 of the FITS lightcurves and their plots were generated at Saitama University in Japan and a copy hosted at the DARTS archive, located at ISAS (<a href="http://www.darts.isas.ac.jp/pub/suzaku/wam-2.0/">http://www.darts.isas.ac.jp/pub/suzaku/wam-2.0/</a>). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/suzakuwam.html
bib_reference = 2010PASJ...62.1341E
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=suzakuwam&
tap_tablename = suzakuwam
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741569
ID = nasa.heasarc/suzamaster
publisher_did = ivo://nasa.heasarc/suzamaster
obs_collection = SUZAMASTER
obs_title = Suzaku Master Catalog
obs_description = This database table records high-level information for each Suzaku observation and provides access to the data archive. Each record is associated with a single observation. An observation contains data from all instruments on board Suzaku. This database table is generated at the Suzaku processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/suzamaster.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=suzamaster&
tap_tablename = suzamaster
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
sia_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=suzamaster&
sia2_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=suzamaster&
sia2_glutag = SIA2
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741589
ID = nasa.heasarc/suzaxislog
publisher_did = ivo://nasa.heasarc/suzaxislog
obs_collection = SUZAXISLOG
obs_title = Suzaku XIS Configuration Log
obs_description = The Suzaku XIS detector units can be configured differently depending on how the user chooses the observation to be carried out. This database table records for each Suzaku observation the different XIS configurations during an observation for all XIS units. The set of parameters that can be configured are: datamode (see also edit mode), window size, on-board window discriminator, on-board grading and event threshold. Each record lists for a given XIS the values set for these parameters in the time interval where they are valid within the observation. Therefore for a given XIS there will be as many records as many different configurations are present within an observation. This database table is generated at the Suzaku processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/suzaxislog.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=suzaxislog&
tap_tablename = suzaxislog
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741601
ID = nasa.heasarc/swbat105m
publisher_did = ivo://nasa.heasarc/swbat105m
obs_collection = SWBAT105M
obs_title = Swift-BAT 105-Month All-Sky Hard X-Ray Survey
obs_description = The catalog includes hard X-ray sources detected in the first 105-months of observations with the Burst Alert Telescope (BAT) coded-mask imager on board the Swift observatory. The 105-month Swift-BAT survey is a uniform hard X-ray all-sky survey with a sensitivity of 8.40x10<sup>-12</sup>erg/s/cm<sup>2</sup> over 90% of the sky and 7.24x10<sup>-12</sup>erg/s/cm<sup>2</sup> over 50% of the sky in the 14-195 keV band. The Swift-BAT 105-month catalog provides 1632 (422 new detections) hard X-ray sources in the 14-195 keV band above the 4.8 sigma significance level. Adding to the previously known hard X-ray sources, 34% (144/422) of the new detections are identified as Seyfert active galactic nuclei (AGNs) in nearby galaxies (z<0.2). The majority of the remaining identified sources are X-ray binaries (7%, 31) and blazars/BL Lac objects (10%, 43). As part of this new edition of the Swift-BAT catalog, the authors release eight-channel spectra and monthly sampled light curves for each object in the online journal and at the <a href="https://swift.gsfc.nasa.gov/results/bs105mon/">Swift-BAT 105-month website</a>. The data reduction, analysis, and catalog generation of the Swift-BAT 105-month survey (between 2004 December and 2013 August) are conducted following the same procedures as in the Swift-BAT 70-month survey (Baumgartner+ 2013, J/ApJS/207/19). The catalog includes 1632 hard X-ray sources detected across the entire sky. Of these 1632 sources, 422 are new detections with respect to the 70-month catalog, and 320 are reported as hard X-ray sources for the first time. The Swift-BAT 105-month survey catalog contains 947 non-beamed AGNs detected in the hard X-ray band. The authors inspected soft X-ray images provided by Swift-XRT (3-10keV), Chandra (2-10keV), ASCA (2-10keV), and XMM-Newton (4-10keV) for the newly detected sources when available using 15 arcmin of matching radius. See section 2.1 of the paper for further explanations. This table was created by the HEASARC in March 2020 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/235/4">CDS Catalog J/ApJS/235/4</a> file table3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swbat105m.html
bib_reference = 2018ApJS..235....4O
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swbat105m&
tap_tablename = swbat105m
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741613
ID = nasa.heasarc/swbatagn60
publisher_did = ivo://nasa.heasarc/swbatagn60
obs_collection = SWBATAGN60
obs_title = Swift BAT 60-Month Survey of Active Galactic Nuclei Catalog
obs_description = Surveys above 10 keV represent one of the best resources to provide an unbiased census of the population of active galactic nuclei (AGNs). The authors present the results of 60 months of observation from 2005 March to 2010 March of the hard X-ray sky with the Swift Burst Alert Telescope (BAT). In this time frame, BAT detected (in the 15 - 55 keV band) 720 sources with a signal-to-noise ratio of >= 5 sigma in an all-sky survey, of which 428 are associated with AGNs, most of which are nearby. This sample has negligible incompleteness and statistics which are a factor of ~ 2 larger over similarly complete sets of AGNs. The sample contains (at least) 15 bona fide Compton-thick AGNs and 3 likely candidates. Compton-thick AGNs represent ~ 5% of AGN samples detected above 15 keV. The authors use the BAT data set to refine the determination of the log N - log S of AGNs which is extremely important, now that NuSTAR prepares for launch, toward assessing the AGN contribution to the cosmic X-ray background. The authors show that the log N - log S of AGNs selected above 10 keV is now established to ~ 10% precision. They derive the luminosity function of Compton-thick AGNs and measure a space density of 7.9 (+4.1, -2.9) x 10<sup>-5</sup> Mpc<sup>-3</sup> for objects with a de-absorbed luminosity larger than 2 x 10<sup>42</sup> erg s<sup>-1</sup>. As the BAT AGNs are all mostly local, they allow us to investigate the spatial distribution of AGNs in the nearby universe regardless of absorption. The authors find concentrations of AGNs that coincide spatially with the largest congregations of matter in the local (<= 85 Mpc) universe. There is some evidence that the fraction of Seyfert 2 objects is larger than average in the direction of these dense regions. This table was created by the HEASARC in May 2012, based on an electronic version of Table 1 from the referenced paper, which was obtained from the ApJ website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swbatagn60.html
bib_reference = 2012ApJ...749...21A
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swbatagn60&
tap_tablename = swbatagn60
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741621
ID = nasa.heasarc/swbatmontr
publisher_did = ivo://nasa.heasarc/swbatmontr
obs_collection = SWBATMONTR
obs_title = Swift BAT Transient Monitoring Catalog
obs_description = The SWBATMONTR database table records high-level information of the lightcurves from the sources monitored with the Burst Alert Telescope (BAT) on board of Swift. The Swift/BAT Monitoring Program is aimed at (1) the discovery of new transient X-ray sources, (2) the detection of outbursts or other changes in the flux of known X-ray sources, and (3) the generation of lightcurves of more than 1000 sources spanning the entire Swift lifetime. Swift is a NASA mission with international participation dedicated to the gamma-ray burst study. It carries three instruments. The BAT is the large field of view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. The BAT monitoring the sky in the field of view and provides alerts when detecting a burst of flux coming from a source in the field of view. The BAT monitoring lightcurves are generated by the BAT team over the course of the Swift mission. The HEASARC ingests these data in the archive and generates this database table by collecting high-level information from the data. The lightcurves are renamed to use a consistent naming convention, and the FITS header is updated by adding standard FITS keywords. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swbatmontr.html
bib_reference = 2013ApJS..209...14K
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swbatmontr&
tap_tablename = swbatmontr
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741633
ID = nasa.heasarc/swbatsfxt
publisher_did = ivo://nasa.heasarc/swbatsfxt
obs_collection = SWBATSFXT
obs_title = Swift BAT 100-Month Supergiant Fast X-Ray Transient Catalog
obs_description = Supergiant Fast X-ray Transients (SFXTs) are High Mass X-ray Binaries (HMXBs) that are defined by their hard X-ray flaring behavior. During such flares they reach peak luminosities of 10<sup>36</sup> - 10<sup>37</sup> erg/s for a few hours (in the hard X-ray), i.e., much shorter timescales than those characterizing Be/X-ray binaries. The authors have investigated the characteristics of bright flares (detections in excess of 5 sigma) for a sample of SFXTs and their relation to the orbital phase. They have retrieved all Swift/BAT Transient Monitor light curves, and collected all detections in excess of 5 sigma from both daily- and orbital-averaged light curves in the time range from 2005 February 12 to 2013 May 31 (MJD 53413 - 56443). The authors also considered all on-board detections as recorded in the same time span and selected those within 4 arcminutes of each source in their sample and in excess of 5 sigma. This table contains the catalog of over a thousand Burst Alert Telescope (BAT) flares from 11 SFXTs, down to 15-150 keV fluxes of ~6 x 10<sup>-10</sup>erg/cm<sup>2</sup>/s (daily timescale) and ~1.5 x 10<sup>-9</sup>erg/cm<sup>2</sup>/s (orbital timescale, averaging ~800s) and spanning 100 months. The great majority of these flares are unpublished. This population is characterized by short (a few hundred seconds) and relatively bright (in excess of 100 milliCrab, 15-50 keV) events. In the hard X-ray, these flares last in general much less than a day. Clustering of hard X-ray flares can be used to indirectly measure the length of an outburst, even when the low-level emission is not detected. In their paper, the authors construct the distributions of flares, of their significance (in terms of sigma) and their flux as a function of orbital phase, to infer the properties of these binary systems. In particular, they observe a trend of clustering of flares at some phases as P_orb increases, as consistent with a progression from tight, circular or mildly eccentric orbits at short periods, to wider and more eccentric orbits at longer orbital periods. Finally, the authors estimate the expected number of flares for a given source for their limiting flux and provide the recipe for calculating them for the limiting flux of future hard X-ray observatories. The BAT observes 88% of the sky daily, on average, so it is ideally suited to detect flaring in hard X-ray sources. Since 2005-02-12, the BAT Transient Monitor (Krimm et al. 2013, ApJS, 209, 14) has been providing near real-time light curves in the 15-50 keV energy range of more than 900 sources with a mean variance for one-day mosaics of 5.3 milliCrab. Several flares from SFXTs are regularly caught every year by the BAT Transient Monitor (BATTM). The catalog contains a total of 1117 flares from 11 SFXT sources (the only other confirmed SFXT, IGR J11215-5952, never triggered the BAT: see Section 2.2 of the reference paper for more information about this source). They are divided into 46 BAT triggers (bat_subsample_flag = 'T', 43 in outbursts), 126 daily-averaged BATTM light curves (bat_subsample_flag = 'D'), 267 orbital-averaged BATTM light curves (bat_subsample_flag = 'O'), and 678 on-board detections (bat_subsample_flag = 'B'). For each flare, the time of the occurrence, duration, flux, and significance are reported. Given the cut in sigma applied to the available BATTM and on-board detections, this catalog is a flux-limited sample of flares. Assuming a Crab-like spectrum (power-law of photon index 2.15), 5 sigma detections for one day and an average orbit typically correspond to fluxes of 5.98 x 10<sup>-10</sup> and 1.46 x 10<sup>-9</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, respectively, in the 15-150 keV band (or 3.38 x 10<sup>-10</sup> and 8.24 x 10<sup>-10</sup> erg cm<sup>-2</sup> s<sup>-1</sup> in the 15-50 keV band). This table was created by the HEASARC in August 2015 based on the union of <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/562/A2">CDS Catalog J/A+A/562/A2</a> files sample.dat (the properties of the confirmed SFXTs) and table4.dat (the catalog of the 1117 flares detected by the Swift BAT from 11 of the 12 confirmed SFXTs). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swbatsfxt.html
bib_reference = 2014A&A...562A...2R
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swbatsfxt&
tap_tablename = swbatsfxt
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741645
ID = nasa.heasarc/swif1swxrt
publisher_did = ivo://nasa.heasarc/swif1swxrt
obs_collection = SWIF1SWXRT
obs_title = The Seven-Year Swift-XRT Point Source Catalog (1SWXRT)
obs_description = This table contains the 1SWXRT catalog of point sources detected by X-ray Telescope (XRT) on board of the Swift satellite during the first seven years of operation (Jan 2005 - Dec 2011). Swift is a NASA mission with international participation dedicated to gamma-ray burst study. It carries three instruments. The BAT is the large field of view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. The seven-year Swift-XRT point source catalog (1SWXRT) was built using all the observations performed by Swift-XRT in PC observing mode with an exposure longer than 500 s. The total number of observations considered is 35011, for an overall exposure time of ~140 Ms. Different observations with same pointing were not merged, but analyzed separately, thus retaining information about the variability of the catalogued sources. Most of the observations have short exposures. In fact, ~18% have t<sub>exp</sub> < 1 ks and ~77% have t<sub>exp</sub> < 5 ks. Only 7% of the observations have an exposure time > 10 ks, which are mostly (but not exclusively) fields associated with GRBs. The catalog was generated by running the detection algorithm in the XIMAGE package version 4.4.1 that locates the point sources using a sliding-cell method. The average background intensity is estimated in several small square boxes uniformly located within the image. The position and intensity of each detected source are calculated in a box whose size maximizes the signal-to-noise ratio. For each detection the catalog reports three count rates in the 0.3-3 (Soft), and 2-10 (Hard), and 0.3-10 (Full) keV energy bands. Each are corrected for dead times and vignetting using exposure maps and for the PSF. Hardness ratios are calculated using the three energy band and defined as HR = (c<sub>H</sub> - c<sub>S</sub>)/(c<sub>H</sub> + c<sub>S</sub>) where c<sub>S</sub> and c<sub>H</sub> are the count rates in the S(oft) and H(ard) bands, respectively. The catalog was cleaned from spurious and extended sources by visual inspection of all the observations. Count rates in the three bands were converted to 0.5-10, 0.5-2, and 2-10 keV observed fluxes, respectively. For the fluxes these energy bands were adopted to easy comparison with other X-ray catalogs (Watson, M. G. et al. 2009, A&A, 493, 339; Evans, I. N. et al. 2010, ApJ, 189, 37). The count rate to flux conversion was made using an absorbed power-law. The absorption is the Galactic hydrogen column density in the direction of the source and the photon spectral index has been estimated through the hardness ratio. Each row in the catalog is a detection not a unique source since the analysis was done by observation. Since multiple observations have covered the same part of the sky, a source may be detected more than once. The total number of detections is 84979 with an estimated 36000 unique sources as reported in the D'Elia et al. paper. The number of unique sources is derived by considering as one source all detections that have their positions within 12 arcsec. However, the catalog does not have a marker to identify all detections of a unique source. This database table was created by the HEASARC in November 2021 based on the electronic version available from the ASI Data Center <a href="https://www.asdc.asi.it/1swxrt/">https://www.asdc.asi.it/1swxrt/</a> and published in the Astronomy and Astrophysics Journal. This catalog is also available as <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/551/A142">CDS catalog J/A+A/551/A142</a>. The HEASARC added the id_number parameter, a counter to numerically identify each detection in the catalog (since the names of the detections are not unique), . Note that there is a discrepancy in the number of detections in the electronic version which has 84979 records and the number of detections reported in the paper (84992). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swif1swxrt.html
bib_reference = 2013A&A...551A.142D
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swif1swxrt&
tap_tablename = swif1swxrt
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741673
ID = nasa.heasarc/swift2sxps
publisher_did = ivo://nasa.heasarc/swift2sxps
obs_collection = SWIFT2SXPS
obs_title = Swift-XRT Point Source Catalog (2SXPS)
obs_description = This table contains the second Swift X-ray Point Source (2SXPS) catalog of detections by the Swift X-ray Telescope (XRT) used in Photon Counting (PC) mode in the 0.3-10 keV energy range. Swift is a NASA mission with international participation dedicated to the gamma-ray burst study. It carries three instruments. The BAT is the large field-of-view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. The overall 2SXPS catalog characteristics are as follows: <pre> Data included 2005 Jan 01 - 2018 August 01 Sky coverage 3,790 square degrees Typical Sensitivity (0.3-10 keV) 2x10<sup>-13</sup> erg cm<sup>-2</sup> s<sup>-1</sup> (observations) 4x10<sup>-14</sup> erg cm<sup>-2</sup> s<sup>-1</sup> (stacked images) Typical position error 5.6" (90% confidence radius, including systematics) Detections 1,091,058 Unique sources 206,335 Variable sources 82,324 Uncatalogued sources 78,100 False positive rate Flag=Good 0.3% Flag=Good/Reasonable 1% Flag=Good/Reasonable/Poor <10% </pre> This catalog enhances the 1SXPS catalogue (Evans, P. A., et al. 2014, ApJS, 210, 8) in different ways. The 2SXPS catalog uses an improved Point Spread Function (PSF) and pile-up models, a better source detection pipeline that includes a technique to model the effects of stray light, and tests to automatically avoid diffuse emission and ~six years more data. The results are that the 2SXPS catalog contains 50% more temporal coverage than 1SXPS, a sky coverage of 3790 square deg almost double compare to the 1SXPS (1905 square Degree) and ~30% more sources compared to the 1SXPS. The Swift XRT observations were filtered to remove times when: a) data were contaminated by scattered light from the daylight side of the Earth; b) the on-board astrometry derived from the images obtained by the Swift UV/Optical telescope was unreliable; and c) observations with less than 100s of PC mode. The 127519 observations included in the catalog provide a total usable exposure is 266.5 Ms. A Swift observation is a collection of snapshots and the source detection algorithm was run on individual observation as well as on stacked images. The latter were generated on a grid of 2,300x2,300 pixels (~ 90'x90') to ensure that every overlap between observations is in at least one stacked image. A total of 14628 stacked images were generated. Each record corresponds to a unique source which characteristics are described with 230 parameters. The catalog reports for each source rates in four energy band (0.3-10.keV, 0.3-1. keV, 1-2 keV and 3-10 keV), background rates, variability for each energy band, two hardness ratio, peak rate and several spectral parameters. The hardness ratios are defined as follows: <pre> HR1 = (M-S)/(M+S) where M and S are the medium (1-2 keV) and soft (0.3-1 keV) band count rates HR2 = (H-M)/(H+M) where H and M are the hard (2-10 keV) and medium (1-2 keV) band count rates </pre> and they are calculated using all observations. The peak rate is determined using three different timescale: the count rate considering all the observations (see parameters rates in this database), the count rate in each observation (not reported in this database) and the count rate in each snapshot (not reported in this database). The peak rate is the rate +/- error from the timescale which has the highest 1-sigma lower-limit on the count rate. Spectral parameters and source flux are estimated using three different methods for two spectral models, a power-law and APEC (see Smith et al., 2001, ApJL, 556, L91). Not all sources have values for all three methods. The parameters starting with "fix" are defined for every source and uses fixed spectral model parameters: a photon index of 1.7 for a power-law model, a temperature of kT=1keV for the APEC model and for both models uses the Galactic absorption listed in the parameter "nh". The parameters starting "intr" have been inferred from the hardness ratio. Look-up tables containing (HR1, HR2, NH, photon index) and (HR1, HR2, NH, kT) are pre-calculated for the power-law and APEC models. If the source HR1 and HR2 are close to the values in the table, spectral parameters are derived by interpolating the HR1 and HR2 in the look-up tables that are close to the HR1 and HR2 of the source. The parameters starting with "fit" have been derived from fitting an actual source spectrum in XSPEC and they are only available for the brightest sources (>50 net counts, and at least one detection in a single observation). The parameters fields starting with "pow" and "apec" report the values from the 'best' of these methods. The parameters "which_pow" and "which_apec" indicates which of the three methods are reported. The catalog also includes flags derived from the cross-correlated with other source catalogs. The catalogs and their reference sources are as follows: <pre> * AllWISE: <a href="https://wise2.ipac.caltech.edu/docs/release/allwise/">https://wise2.ipac.caltech.edu/docs/release/allwise/</a> * ROSAT HRI: <a href="https://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html">https://heasarc.gsfc.nasa.gov/docs/rosat/rra/RRA.html</a> * SDSS Quasar Catalog DR14: Paris et al., 2018, A&A, 613, 51 (<a href="https://www.sdss.org/dr14/algorithms/qso_catalog/">https://www.sdss.org/dr14/algorithms/qso_catalog/</a>) * 2MASS: Skrutskie et al., 2006, AJ, 131, 1163 * 2CSC: accessed via the CSCView Tool at <a href="https://cxc.harvard.edu/csc/about.html">https://cxc.harvard.edu/csc/about.html</a> (1CSC paper: Evans et al., 2010, ApJS, 189, 37) * 1SWXRT: Evans et al., 2014, ApJS, 210,8 * 1SXPS: D'Elia et al., 2013, A&A, 551, 142 * 2RXS: Boller et al., 2016, A&A, 588, 103 * 3XMM-DR8: <a href="http://xmmssc.irap.omp.eu/Catalogue/3XMM-DR8/3XMM_DR8.html">http://xmmssc.irap.omp.eu/Catalogue/3XMM-DR8/3XMM_DR8.html</a> (3XMM paper: Rosen, Webb, Watson et al., 2016, A&A, 590, 1) * 3XMM Stack: Traulsen et al., 2019, A&A, 642, 77 * SwiftFT: Puccetti et al. 2011, A&A,528, A122 * XMM SL2: Saxton et al., 2008, A&A 480, 611 * XRTGRB: Evans et al, 2009, MNRAS, 397, 1177 (<a href="https://www.swift.ac.uk/xrt_positions">https://www.swift.ac.uk/xrt_positions</a>) * USNOB1: Monet et al., 2003, AJ, 125, 984 </pre> The 2SXPS paper (Evans et al. 2020 ApJS, 247,54) describes in detail the methodology of stacking images, background modeling, point spread function mapping, stray light detection and corrections, data filtering techniques and processing. The 2SXPS catalog has a dedicated website at <a href="https://www.swift.ac.uk/2SXPS">https://www.swift.ac.uk/2SXPS</a>. This database table was created by the HEASARC in November 20201 based on the electronic version delivered to the HEASARC by the Leicester University. The catalog has a dedicated website at <a href="https://www.swift.ac.uk/2SXPS">https://www.swift.ac.uk/2SXPS</a>. The version available from the HEASARC corresponds to the catalog designated as "All" on the Leicester website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swift2sxps.html
bib_reference = 2020ApJS..247...54E
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swift2sxps&
tap_tablename = swift2sxps
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741701
ID = nasa.heasarc/swiftbalog
publisher_did = ivo://nasa.heasarc/swiftbalog
obs_collection = SwiftBAT
obs_title = Swift BAT Instrument Log
obs_description = The BAT can operate several configuration modes simultaneously. Each of the simultaneous modes is listed in separate records within this table. For a given time interval, there are several records (partially overlapping in time), each describing a single configuration/mode. The BAT modes collect data for the entire FOV but also have the capability to record rates (tag mask rate) for up to a few specific sky positions (typically 3) that correspond to a pre-assigned target ID. It is possible that at least two or more of these positions do not coincide with the BAT or NFI pointing position and therefore the target ID does necessarily coincide with Target_ID of the BAT or NFI pointing position. This table records for the position (RA and Dec) and Target_ID parameters the correct values associated to each of the mask tag data. This database table is generated at the Swift processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swiftbalog.html
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swiftbalog&
tap_tablename = swiftbalog
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
ssa_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/ssa?table=swiftbalog&
sia_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=swiftbalog&
sia2_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=swiftbalog&
sia2_glutag = SIA2
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741773
ID = nasa.heasarc/swiftft
publisher_did = ivo://nasa.heasarc/swiftft
obs_collection = SWIFTFT
obs_title = Swift Serendipitous Survey in Deep XRT GRB Fields (SwiftFT)
obs_description = This table contains the SwiftFT catalog of point sources detected by the X-ray Telescope (XRT) on board the Swift satellite in observations centered on gamma-ray bursts (GRBs) during the first four years of operation (Jan 2005 - Dec 2008). Swift is a NASA mission with international participation dedicated to the gamma-ray burst study. It carries three instruments. The BAT is the large field of view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. The catalog was derived including pointing positions of the 374 fields centered on the GRBs covering a total area of ~32.55 square degrees. Since GRBs are distributed randomly in the sky, the survey covers totally unrelated parts of the sky, and is highly uniform courtesy of the XRT's stable point spread function and small vignetting correction factors. The observations for a particular field were merged together and the source search analysis was restricted to a circular area of 10 arcmin radius centered in the median of the individual observation aim points. The total exposure considering all the fields is of 36.8 Ms, with ~32% of the fields having more than 100 ks exposure time, and ~28% with exposure time in the range 50-100 ks. The catalog was generated by running the detection algorithm in the XIMAGE package version 4.4.1 that locates the point sources using a sliding-cell method. The average background intensity is estimated in several small square boxes uniformly located within the image. The position and intensity of each detected source are calculated in a box whose size maximizes the signal-to-noise ratio. The detect algorithm was run separately in the following three energy bands: 0.3-3 (Soft), 2-10 (Hard), and 0.3-10 (Full) keV. For each detections the three count rates in the soft, hard, and full bands are all corrected for dead times and vignetting using exposure maps and for the PSF. Hardness ratios are calculated using the three energy band and defined as HR = (c<sub>H</sub> - c<sub>S</sub>)/(c<sub>H</sub> + c<sub>S</sub>) where c<sub>S</sub> and c<sub>H</sub> are the count rates in the S(oft) and H(ard) bands, respectively. The catalog was cleaned of spurious and extended sources by visual inspection of all the observations. Count rates in the three bands were converted into flux in the 0.5-10, 0.5-2, and 2-10 keV energy bands, respectively. The flux was estimated using a power law spectrum with photon spectral index of 1.8 and a Galactic N<sub>H</sub> of 3.3 x 10<sup>20</sup> cm<sup>-2</sup>. Each row in the catalog is a unique source. The detections from the soft, hard, and full bands were merged into a single catalog using a matching radius of 6 arcsec and retaining detection with a significance level of being spurious <= 2 x 10<sup>-5</sup> in at least one band. There are 9387 total entries in the catalog. The SWIFTFT acronym honors both the Swift satellite and the memory of Francesca Tamburelli who made numerous crucial contributions to the development of the Swift-XRT data reduction software. This database table was created by the HEASARC in November 2021 based on the electronic version available from the ASI Data Center <a href="https://www.asdc.asi.it/xrtgrbdeep_cat/">https://www.asdc.asi.it/xrtgrbdeep_cat/</a> and published in the Astronomy and Astrophysics Journal. This catalog is also available as the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/528/A122">CDS catalog J/A+A/528/A122</a>. The HEASARC added the source_number parameter, a counter to numerically identify each source in the catalog, as well as Galactic coordinates and changed the source name from SWIFTFTJHHMMSS.s+DDMM.m to SWIFTFT JHHMMSS.s+DDMM.m, adding a space between the catalog prefix and the formatted J2000 coordinates. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swiftft.html
bib_reference = 2011A&A...528A.122P
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swiftft&
tap_tablename = swiftft
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741785
ID = nasa.heasarc/swiftgrb
publisher_did = ivo://nasa.heasarc/swiftgrb
obs_collection = SWIFTGRB
obs_title = Swift Gamma Ray Bursts Catalog
obs_description = This table contains the results of the Gamma Ray Bursts (GRBs) observed by Swift. The GRBs included are either triggered by Swift or follow-ups of GRBs discovered by other satellites. The table reports results and/or information, when possible, for each burst from all three instruments on board Swift, e.g. the Bursts Alert Telescope, BAT,the X-ray Telescope, XRT, and the Ultra-Violet Optical Telescope, UVOT. The results are obtained from a standard analysis processing of the Swift data which creates several data products available via this table. Additional information on the burst either from Gamma-ray and X-ray observations or results from ground-based telescopes are extracted from the GCN and the BAT Burst catalog. This table's data products are also available from the dedicated web pages <a href="http://heasarc.gsfc.nasa.gov/docs/swift/archive/grbsummary/">http://heasarc.gsfc.nasa.gov/docs/swift/archive/grbsummary/</a>. The current database contains all bursts observed by Swift from the beginning of the mission, 20 Nov 2004 up to 31 Dec 2012. The data products are available for Bursts detected after 15 Feb 2005. This online catalog was created by the HEASARC based on machine-readable tables compiled by the HEASARC staff. Details are published in Donato et al. (2012). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swiftgrb.html
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swiftgrb&
tap_tablename = swiftgrb
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741801
ID = nasa.heasarc/swiftguano
publisher_did = ivo://nasa.heasarc/swiftguano
obs_collection = SWIFTGUANO
obs_title = Swift Gamma-ray Urgent Archiver for Novel Opportunities (GUANO) Events
obs_description = The Swift Observatory provides event-level data from the Burst Alert Telescope (BAT) on demand in response to transients detected by other observatories/instruments. This capability, named "Gamma-ray Urgent Archiver for Novel Opportunities" (GUANO), was introduced in 2020. In normal operations, BAT records the arrival time (to 100-microsecond accuracy), location (in detector coordinates), and energy (in one of 80 bins from 15 to 350 keV) for each individual count that strikes the detector. These data, referred as event-by-event (or event), because of the large effective area of the BAT, produces a large data volume that cannot all be stored onboard or telemetered to the ground. For this reason, the BAT has relied on the performance of its onboard real-time detection algorithms, and only preserves event data and telemeters them to the ground around the time of events that trigger these onboard algorithms. The GUANO implementation allows to download BAT event data that did not trigger on board. Upon receiving an alert from different observatories, an autonomous spacecraft-commanding pipeline requests to download from the Swift satellite the BAT event data around the time of the GUANO event with a time window, typically around 200 seconds. The satellite does not slew; therefore, only BAT event data are available for the GUANO event and these data are tagged with a sequence number associated with the ongoing observation containing the GUANO time window. This table records the times of the GUANO events from different observatories from which Swift was able to download the BAT event data together with the directory and file names where the event are located in the archive. There is one record for each trigger by an external observatory that requested BAT event data; therefore, it is possible that multiple records are associated with the same event. This contents of this database table are generated at the Swift processing site. During operation, it is updated for any new GUANO trigger. These updates are then delivered to the HEASARC and ingested into the HEASARC database in a timely fashion. Note that some parameters (specifically, the galactic coordinates) have been added and are populated by the HEASARC. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swiftguano.html
bib_reference = 2020ApJ...900...35T
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swiftguano&
tap_tablename = swiftguano
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741813
ID = nasa.heasarc/swiftmastr
publisher_did = ivo://nasa.heasarc/swiftmastr
obs_collection = Swift
obs_title = Swift Master Catalog
obs_description = This table records high-level information for each Swift observation and provides access to the data archive. Each record is associated with a single observation that contains data from all instruments on board Swift. The BAT is the large field of view instrument and operates in the 10-300 keV energy band. The narrow field instruments, XRT and UVOT, operate in the X-ray and UV/optical regime, respectively. An observation is defined as a collection of snapshots, where a snapshot is defined as the time spent observing the same position continuously. Because of observing constraints, the length of a snapshot can be shorter than a single orbit and it can be interrupted because the satellite will point in a different direction of the sky or because the time allocated to that observation ends. The typical Swift observing strategy for a Gamma Ray Burst (GRB) and/or afterglow, consists of a serious of observations aimed at following the GRB and its afterglow evolution. This strategy is achieved with two different type of observations named Automatic Targets and Pre-Planned Targets. The Automatic Target is initiated on board soon after an event is triggered by the BAT. The Figure of Merit (FOM) algorithm, part of the observatory's autonomy, decides if it is worth requesting a slew maneuver to point the narrow field instruments (NFI) on Swift, XRT and UVOT, in the direction of the trigger. If the conditions to slew to the new position are satisfied, the Automatic Target observation takes place; all the instruments have a pre-set standard configuration of operating modes and filters and about 20000 seconds on source will be collected. The Pre-Planned Target observations instead are initiated from the ground once the trigger is known. These observations are planned on ground and uploaded onto the spacecraft. This database table is generated at the Swift processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swiftmastr.html
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swiftmastr&
tap_tablename = swiftmastr
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741821
ID = nasa.heasarc/swifttdrss
publisher_did = ivo://nasa.heasarc/swifttdrss
obs_collection = SWIFTTDRSS
obs_title = Swift TDRSS Messages
obs_description = This database table is derived from the Swift TDRSS messages sent on ground soon after a BAT trigger occurs on-board. For each trigger there are associated up to 14 messages, however not all are always generated and sent on ground. The messages are generated on board by the BAT, XRT and UVOT instruments and the Figure of Merit part of the observatory's autonomy. The BAT and XRT can each have five different message types. The UVOT and FOM can each have two different message types. These TDRSS messages are the results of the on-board data processing of the three instruments and some contain data products. They are first distributed via the GCN and later archived. The BAT messages are: alert, 'ack' containing the position, or 'nack' if the position could not be calculated, a lightcurve and scaled map. The XRT messages are: centroid containing the position, an image (if the position has been calculated), centroid error if the position could not be calculated, spectra in Low Rate Photodiode and Windowed Timing modes, a lightcurve. The UVOT messages are: finding chart containing star positions and a subimage centered on the XRT position. The FOM messages are used to indicate if the FOM will or will not observe the new target and if the spacecraft will (or will not) request a slew for the new target. The parameters in this database table are a collection of high level information taken from the following messages : the BAT alert, 'ack' or 'nack' message, the FOM messages, the XRT position and image. If the information is not available the fields are left blank. All messages are provided as data products within this database table. This database table is generated at the Swift processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swifttdrss.html
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swifttdrss&
tap_tablename = swifttdrss
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845741833
ID = nasa.heasarc/swiftuvlog
publisher_did = ivo://nasa.heasarc/swiftuvlog
obs_collection = SwiftUVOT
obs_title = Swift UVOT Instrument Log
obs_description = The UVOT runs only one type of configuration filter/mode/window in a given time interval. This database table, therefore, contains for a given time interval a single record that describes one configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swiftuvlog.html
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swiftuvlog&
tap_tablename = swiftuvlog
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
sia_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=swiftuvlog&
sia2_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=swiftuvlog&
sia2_glutag = SIA2
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845742085
ID = nasa.heasarc/swiftxrlog
publisher_did = ivo://nasa.heasarc/swiftxrlog
obs_collection = SwiftXRT
obs_title = Swift XRT Instrument Log
obs_description = The XRT runs only one type of configuration mode/window in a given time interval. The table therefore contains for a given time interval a single record that describes one configuration. A new record is generated when the following is changing within an observation: new operating mode , new pointing mode, or new window configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swiftxrlog.html
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swiftxrlog&
tap_tablename = swiftxrlog
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
ssa_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/ssa?table=swiftxrlog&
sia_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=swiftxrlog&
sia2_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=swiftxrlog&
sia2_glutag = SIA2
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743201
ID = nasa.heasarc/swirecxo
publisher_did = ivo://nasa.heasarc/swirecxo
obs_collection = SWIRECXO
obs_title = Spitzer Wide-Area IR Extra-Galactic Survey Chandra X-Ray Sources
obs_description = This table contains results from deep combined observations with Spitzer and Chandra of the Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE) in the ELAIS N1 region. This survey was used to investigate the nature of the faint X-ray and IR sources in common, to identify active galactic nucleus (AGN)/starburst diagnostics, and to study the sources of the X-ray and cosmic infrared backgrounds (XRB and CIRB). In the 17' x 17' area of the Chandra ACIS-I image there were approximately 3400 SWIRE near-IR sources with 4-sigma detections in at least two Infrared Array Camera (IRAC) bands and 988 sources detected at 24 micron (um) with the Multiband Imaging Photometer (MIPS) brighter than a 24-um flux S_24 ~ 0.1 mJy. Of these, 102 IRAC and 59 MIPS sources have Chandra counterparts, out of a total of 122 X-ray sources present in the area with 0.5 - 8 keV flux > 10-15 erg cm^-2 s^-1. The SWIRE ELAIS N1 field was imaged by the IRAC multiband camera on Spitzer in 2004 January and with MIPS in early 2004 February. The observations were centered at the position (16h 00m, +59d 01'). The X-ray observations were taken as part of the ELAIS Deep X-ray Survey (EDXS) and are described in detail in Manners et al. (2003, MNRAS, 343, 293). For this analysis, the Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of 75 ks centered on (16h 10m 20.11s, +54d 33' 22.3") (J2000.0) in the ELAIS N1 region. The aim point was focused on the ACIS-I chips, which consist of four CCDs arranged in a 2 x 2 array covering an area of 16.9' x 16.9' (286 square arcmin). Bad pixels and columns were removed, and data were filtered to eliminate high background times (due to strong solar flares), leaving 71.5 ks of good data after filtering. Counts-to-photon calibration assumed a standard power-law model spectrum with photon index Gamma = 1.7. Sources were detected to flux levels of 2.3 x 10^-15 erg s^-1 cm^-2 in the 0.5 - 8 keV band, 9.4 x 10^-16 erg s^-1 cm^-2 in the 0.5 - 2 keV band, and 5.2 x 10^-15 erg s^-1 cm^-2 in the 2 - 8 keV band. Sources are detectable to these flux limits over 90% of the nominal survey area. For this analysis, the authors used sources detected in the full band of ACIS-I only, of which there are 122 in the N1 region. Of the 102 sources in common between Chandra and SWIRE, 83 have significant detections in the separate soft X-ray band (0.5 - 2 keV) and 64 are detected in the hard (2 - 8 keV) band. A simple near-neighbor search was performed to cross-correlate the Spitzer and Chandra source catalogs within the Chandra ACIS-I chip image, using a d = 5" search radius (roughly the quadratic sum of the astrometric errors). All together, the authors found reliably associated counterparts for 102 of the 122 Chandra sources (84% in total). The vast majority of these were detected with the IRAC channels 1 and 2 (3.6 and 4.5 um): 100 of the 122 Chandra sources in each case. As many as 59 Chandra objects are reliably associated with MIPS 24 um sources (all of them having IRAC counterparts), and just 1 had a MIPS 70 um counterpart. Of the 102 Spitzer-identified Chandra sources, three turned out to correspond to Galactic stars on the basis of their position on color-magnitude plots and optical morphology and were excluded from the subsequent analysis (and this table). This table was created by the HEASARC in March 2007 based on CDS catalog J/AJ/129/2074 file table2.dat, This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swirecxo.html
bib_reference = 2005AJ....129.2074F
obs_regime = infrared
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swirecxo&
tap_tablename = swirecxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743225
ID = nasa.heasarc/swirelhcxo
publisher_did = ivo://nasa.heasarc/swirelhcxo
obs_collection = SWIRELHCXO
obs_title = SWIRE/Chandra Lockman Hole Field X-Ray Source Catalog
obs_description = The authors have carried out a moderate-depth (70 ks), contiguous 0.7 square degrees Chandra survey in the Lockman Hole Field of the Spitzer/SWIRE Legacy Survey coincident with a completed, ultra-deep VLA survey with deep optical and near-infrared imaging in-hand. The primary motivation is to distinguish starburst galaxies and active galactic nuclei (AGNs), including the significant, highly obscured (log N<sub>H</sub> > 23 cm<sup>-2</sup>) subset. Chandra has detected 775 X-ray sources to a limiting broadband (0.3 - 8 keV) flux of ~4 x 10<sup>-16</sup> erg cm<sup>-2</sup> s<sup>-1</sup>. This table contains the X-ray catalog, fluxes, hardness ratios, and multi-wavelength fluxes. The log N versus log S agrees with those of previous surveys covering similar flux ranges. The Chandra and Spitzer flux limits are well matched: 771 (99%) of the X-ray sources have infrared (IR) or optical counterparts, and 333 have MIPS 24-micron detections. There are four optical-only X-ray sources and four with no visible optical/IR counterpart. The very deep (~2.7 microJansky rms) VLA data yield 251 (> 4 sigma) radio counterparts, 44% of the X-ray sources in the field. The authors confirm that the tendency for lower X-ray flux sources to be harder is primarily due to absorption. As expected, there is no correlation between observed IR and X-ray fluxes. Optically bright, type 1, and red AGNs lie in distinct regions of the IR versus X-ray flux plots, demonstrating the wide range of spectral energy distributions in this sample and providing the potential for classification/source selection. Many optically bright sources, which lie outside the AGN region in the optical versus X-ray plots (f<sub>r</sub>/f<sub>x</sub> > 10), lie inside the region predicted for red AGNs in IR versus X-ray plots, consistent with the presence of an active nucleus. More than 40% of the X-ray sources in the VLA field are radio-loud using the classical definition of R<sub>L</sub>. The majority of these are red and relatively faint in the optical so that the use of R<sub>L</sub> to select those AGNs with the strongest radio emission becomes questionable. Using the 24-micron to radio flux ratio (q<sub>24</sub>) instead results in 13 of the 147 AGNs with sufficient data being classified as radio-loud, in good agreement with the ~10% expected for broad-lined AGNs based on optical surveys. The authors conclude that q<sub>24</sub> is a more reliable indicator of radio-loudness. Use of R<sub>L</sub> should be confined to the optically selected type 1 AGN. This table was created by the HEASARC in December 2009 based on the machine-readable versions of Tables 3, 4 and 7 from the reference paper which was obtained from the Astrophysical Journal web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swirelhcxo.html
bib_reference = 2009ApJS..185..433W
obs_regime = infrared
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swirelhcxo&
tap_tablename = swirelhcxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743241
ID = nasa.heasarc/swsdssqso
publisher_did = ivo://nasa.heasarc/swsdssqso
obs_collection = SWSDSSQSO
obs_title = Swift Simultaneous UV, Optical, and X-Ray Observed Quasar Catalog
obs_description = The authors have compiled a catalog of optically selected quasars with simultaneous observations in UV/optical and X-ray bands by the Swift Gamma-ray Burst Explorer. Objects in this catalog are identified by matching the Swift pointings with the Sloan Digital Sky Survey (SDSS) Data Release 5 (DR5) quasar catalog. The final catalog contains 843 objects, among which 637 have both Ultraviolet Optical Telescope (UVOT) and X-Ray Telescope (XRT) observations and 354 of which are detected by both instruments. The overall X-ray detection rate is ~ 60% which rises to ~ 85% among sources with at least 10 ks of XRT exposure time. The authors construct the time-averaged spectral energy distribution (SED) for each of the 354 quasars using UVOT photometric measurements and XRT spectra. From model fits to these SEDs, they find that the big blue bump contributes about ~ 0.3 dex to the quasar luminosity. The authors re-visit the alpha<sub>ox</sub> - L<sub>2500A</sub> relation by selecting a clean sample with only Type 1 radio-quiet quasars; the dispersion of this relation is reduced by at least 15% compared with studies that use non-simultaneous UV/optical and X-ray data. They find only a weak correlation between L<sub>bol</sub>/L<sub>Edd</sub> and alpha<sub>UV</sub>. They do not find significant correlations between alpha<sub>x</sub> and alpha<sub>ox</sub>, alpha<sub>ox</sub> and alpha<sub>UV</sub>, and alpha<sub>x</sub> and log L(0.3-10 keV). The correlations between alpha<sub>UV</sub> and alpha<sub>x</sub>, alpha<sub>ox</sub> and alpha<sub>x</sub>, alpha<sub>ox</sub> and alpha<sub>UV</sub>, L<sub>bol</sub>/L<sub>Edd</sub> and alpha<sub>x</sub>, and L<sub>bol</sub>/L<sub>Edd</sub> and alpha<sub>ox</sub> are stronger among low-redshift quasars, indicating that these correlations are likely driven by the changes of SED shape with accretion state. This quasar sample was compiled in the following steps: 1. Candidate objects for the catalog were selected as any SDSS DR5 quasar that lie within 20 arcminutes of the center of the Swift FOV in any pointing from launch through 2008 June. 2. XRT data were processed to obtain X-ray count rates, spectra, and spectral parameters. 3. UVOT data were processed to obtain UV and optical photometry. 4. UVOT photometry were supplemented with measurements at other wavelengths from published catalogs. 5. Quasar SEDs were constructed. 6. Additional parameters were calculated based on the SEDs of each quasar. The raw sample is constructed by matching 3.5 years Swift pointings and the SDSS DR5 quasar catalog and contains 1034 objects. This HEASARC version of this catalog contains all 1034 objects in the "raw" catalog. To select only the 843 objects in the "final" catalog, the user should specify catalog_flag = 1 in any searches of this table. This table was created by the HEASARC in August 2012 based on an electronic version of Table 8 from the reference paper which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swsdssqso.html
bib_reference = 2012ApJS..201...10W
obs_regime = optical
obs_regime = uv
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swsdssqso&
tap_tablename = swsdssqso
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743265
ID = nasa.heasarc/swuvotssc
publisher_did = ivo://nasa.heasarc/swuvotssc
obs_collection = SWUVOTSSC
obs_title = Swift/UVOT Serendipitous Source Catalog, v1.1
obs_description = The first version of the Swift UVOT Serendipitous Source Catalog (UVOTSSC) provides positions and magnitudes, as well as errors and upper limits of confirmed sources, for observations taken from the start of operations in 2005 until October 1st of 2010. The first version of the UVOTSSC has been produced by processing the image data obtained from the Swift Ultraviolet and Optical Telescope (UVOT). The data processing was performed at the Mullard Space Science Laboratory (MSSL, University College London, U.K.) using Swift FTOOLS from NASA's High Energy Astrophysics Software package (HEASoft-6.11), with some customizing of the UVOT packages in order to get more complete source detection and to properly apply quality flags to those sources that were detected within the UVOT image artifacts. The total number of observations with 17'x17' images used for version 1 of the catalog is 23,059, giving 6,200,016 sources in total, of which 2,027,265 have multiple entries in the source table because they have been detected in more than one observation. Some sources were only observed in one filter. The total number of entries in the source table is 13,860,568. The S/N ratio for all sources exceeds 5 in at least one UVOT filter, the rest of the filters having a S/N greater than 3. U, B, V, UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the UVOT Filterwheel section of the MSSL documentation at <a href="http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html">http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html</a>. The initially released version of the catalog (2015) was done with the source identifier "SWIFTUVOT" for each source, and was made available in that form. The decision was subsequently made to rename the catalog sources by including the catalog version number. In addition, in a few instances multiple source IDs shared the same name (IAUNAME). They will be distinguished by having a letter a,b,c,.. appended to their name. Sources brighter than 0.96 counts per frame have not been included because their coincidence loss is too large to correct for. This HEASARC table contains version 1.1 of the Swift UVOT source table and contains 13,860,568 entries for the individual detections of 6,200,016 sources. The HEASARC has changed the names of many of the parameters from those given in the original table. In such cases, we have listed the original names in parentheses at the end of the parameter descriptions given below. There is a second related table which gives a summary of the observations from which the UVOTSSC sources listed in this table have been detected and measured, which is available at the HEASARC as the SWUVOTSSOB table. This table was created by the HEASARC in May 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/339">CDS Catalog II/339</a> file uvotssc1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swuvotssc.html
bib_reference = 2014styd.confE..37P
obs_regime = optical
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swuvotssc&
tap_tablename = swuvotssc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743285
ID = nasa.heasarc/swuvotssob
publisher_did = ivo://nasa.heasarc/swuvotssob
obs_collection = SWUVOTSSOB
obs_title = Swift/UVOT Serendipitous Source Catalog, v1.1: Observations IDs
obs_description = The first version of the Swift UVOT Serendipitous Source Catalog (UVOTSSC) provides positions and magnitudes, as well as errors and upper limits of confirmed sources, for observations taken from the start of operations in 2005 until October 1st of 2010. The first version of the UVOTSSC has been produced by processing the image data obtained from the Swift Ultraviolet and Optical Telescope (UVOT). The data processing was performed at the Mullard Space Science Laboratory (MSSL, University College London, U.K.) using Swift FTOOLS from NASA's High Energy Astrophysics Software package (HEASoft-6.11), with some customizing of the UVOT packages in order to get more complete source detection and to properly apply quality flags to those sources that were detected within the UVOT image artifacts. The total number of observations with 17'x17' images used for version 1 of the catalog is 23,059, giving 6,200,016 sources in total, of which 2,027,265 have multiple entries in the source table because they have been detected in more than one observation. Some sources were only observed in one filter. The total number of entries in the source table is 13,860,568. The S/N ratio for all sources exceeds 5 in at least one UVOT filter, the rest of the filters having a S/N greater than 3. One Swift ObsID can consist of one or more images, which for this catalog have been summed, yielding the quoted total exposure times. The original UVOT images can be found in the on-line archives at MAST, and in the Swift archives at <a href="http://swift.ac.uk/">http://swift.ac.uk/</a> and at the HEASARC (<a href="http://heasarc.gsfc.nasa.gov/W3Browse/all/swiftmastr.html">http://heasarc.gsfc.nasa.gov/W3Browse/all/swiftmastr.html</a>), using the ObsID as the search key. For higher temporal resolution, the original images need to be used because the catalog data herein are summed over all of the individual images within an ObsID. The upper limits per filter for the summed images are constructed for each ObsID because the sensitivity hardly varies over the detector. Usually the images within one ObsID share the same pointing, however, whereas the quoted upper limits always apply for sources near the pointing direction given, if the images had small offsets in pointing they may not apply to sources near the edge of the summed image, which is typically about 8 arcminutes from the quoted pointing direction. U, B, V, UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the UVOT Filterwheel section of the MSSL documentation at <a href="http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html">http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html</a>. This HEASARC table contains version 1.1 of the Swift UVOT table of observations in which the sources in the source table were detected and contains the details of 23,059 Swift UVOT observations. The HEASARC has changed the names of many of the parameters from those given in the original table. In such cases, we have listed the original names in parentheses at the end of the parameter descriptions given below. There is a related table which lists the 13,860,568 source detections that is available at the HEASARC as the SWUVOTSSC table. This table was created by the HEASARC in May 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/339">CDS Catalog II/339</a> file summary.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swuvotssob.html
bib_reference = 2014styd.confE..37P
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swuvotssob&
tap_tablename = swuvotssob
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743305
ID = nasa.heasarc/swxcscat
publisher_did = ivo://nasa.heasarc/swxcscat
obs_collection = SWXCSCAT
obs_title = Swift X-Ray Telescope Cluster Survey Catalog
obs_description = This table contains the Swift X-ray Cluster Survey (SWXCS) catalog obtained using archival data from the X-ray telescope (XRT) on board the Swift satellite acquired from 2005 February to 2012 November, extending the first release of the SWXCS. The catalog provides positions and soft X-ray fluxes for a flux-limited sample of X-ray group and cluster candidates. In Table 3 of the reference paper (available at the HEASARC as the linked table SWXCSOXID), when possible, optical counterparts are given for these candidates. The authors consider the fields with Galactic latitude |b| > 20 degrees so as to avoid regions of high H I column density. They discard all of the observations targeted at groups or clusters of galaxies, as well as particular extragalactic fields not suitable for searching for faint extended sources. The authors finally select ~ 3000 useful fields covering a total solid angle of ~ 400 deg<sup>2</sup>. They identify extended source candidates in the soft-band (0.5-2 keV) images of these fields using the software EXSdetect, which is specifically calibrated for the XRT data. Extensive simulations are used to evaluate contamination and completeness as a function of the source signal, allowing the authors to minimize the number of spurious detections and to robustly assess the selection function. The final catalog includes 263 candidate galaxy clusters and groups down to a flux limit of 7 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s in the soft band (0.5 - 2.0 keV), and the log N - log S is in very good agreement with previous deep X-ray surveys. In the reference paper, the final list of sources is cross-correlated with published optical, X-ray, and Sunyaev-Zel'dovich catalogs of clusters. The authors find that 137 sources have been previously identified as clusters in the literature in independent surveys, while 126 are new detections. Currently, they have collected redshift information for 158 sources (60% of the entire sample). From the entire Swift XRT archive in the period 2005 February-2012 November, the authors have selected all the fields that can be used to build an unbiased, serendipitous X-ray cluster catalog. This table was created by the HEASARC in March 2015 based on an electronic version of Table 2 from the reference paper which was obtained from the CDS as their catalog J/ApJS/216/28 file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swxcscat.html
bib_reference = 2015ApJS..216...28L
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swxcscat&
tap_tablename = swxcscat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743317
ID = nasa.heasarc/swxcsoxid
publisher_did = ivo://nasa.heasarc/swxcsoxid
obs_collection = SWXCSOXID
obs_title = Swift X-Ray Telescope Cluster Survey Cross-Correlation Catalog
obs_description = This table contains the Swift X-ray Cluster Survey (SWXCS) table of cross-correlations of the X-ray galaxy cluster and group candidates with optical, X-ray and Sunyaev-Zel'dovich catalogs and optical follow-up. The SWXCS list of cluster candidates was obtained using archival data from the X-ray telescope (XRT) on board the Swift satellite acquired from 2005 February to 2012 November, extending the first release of the SWXCS. The main catalog (available at the HEASARC as the linked table SWXCSCAT) provides positions and soft X-ray fluxes for a flux-limited sample of X-ray group and cluster candidates. The table herein (based on Table 3 of the reference paper) contains when possible, optical and other counterparts for these candidates. The authors consider the fields with Galactic latitude |b| > 20 degrees so as to avoid regions of high H I column density. They discard all of the observations targeted at groups or clusters of galaxies, as well as particular extragalactic fields not suitable for searching for faint extended sources. The authors finally select ~ 3000 useful fields covering a total solid angle of ~ 400 deg<sup>2</sup>. They identify extended source candidates in the soft-band (0.5-2 keV) images of these fields using the software EXSdetect, which is specifically calibrated for the XRT data. Extensive simulations are used to evaluate contamination and completeness as a function of the source signal, allowing the authors to minimize the number of spurious detections and to robustly assess the selection function. The final catalog includes 263 candidate galaxy clusters and groups down to a flux limit of 7 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s in the soft band (0.5 - 2.0 keV), and the log N - log S is in very good agreement with previous deep X-ray surveys. In the reference paper, the final list of sources is cross-correlated with published optical, X-ray, and Sunyaev-Zel'dovich catalogs of clusters. The authors find that 137 sources have been previously identified as clusters in the literature in independent surveys, while 126 are new detections. Currently, they have collected redshift information for 158 sources (60% of the entire sample). The authors checked for counterparts in previous X-ray cluster surveys, in optical cluster surveys, and in the Planck SZ cluster survey. They simply assume a search radius of 2 arcminutes from the X-ray centroid, which has been shown to be an efficient criterion in Paper I. Nevertheless, they also inspected the area within 5 arcminutes from the X-ray centroid in order to investigate whether some possible identification is found at radii larger than 2 arcminutes. Counterparts at distances between 2 and 5 arcminutes are included when the optical or SZ corresponding source has a large uncertainty in its position. This is often the case for optical, sparse clusters, or for SZ cluster candidates. The authors list all of the counterparts associated with the SWXCS sources herein, and they include the measured redshift when available. In case of multiple counterparts, they list all of them. Except for a few cases where there are multiple counterparts with statistically inconsistent redshifts, the authors keep the counterpart with the smallest angular distance from the X-ray center. From optical surveys, the authors found 233 optical counterparts corresponding to 116 SWXCS sources. From X-ray surveys, they found 70 X-ray counterparts classified as clusters, corresponding to 36 SWXCS sources. Finally, for 15 SWXCS sources, they found 16 cluster counterparts detected via the SZ effect, 13 by Planck and 3 by the South Pole Telescope (SPT). The Planck sources are typically at larger distances from the X-ray centroid (between 1 and 3 arcminutes) because of the much larger position errors of Planck clusters. Overall, about half (137) of the 263 SWXCS sources were previously identified as groups or clusters of galaxies, while 126 SWXCS sources are new cluster and group candidates. The authors have collected spectroscopic or photometric redshifts for 130 of their sources. Moreover, to increase the number of available redshifts, they also searched in NED catalogs for single galaxies with published redshifts not associated with previously known clusters within a search radius of 7 arcseconds from the X-ray centroid of their sources. They find 50 galaxies with measured redshifts for 47 of their sources as a complement to the redshifts obtained from cluster counterparts. In 35 cases where the authors have both cluster and galaxy counterparts, the galaxy redshifts are consistent with those of clusters. In the 12 cases where no cluster counterpart is found, the authors tentatively assign the galaxy redshift to their X-ray source. This table was created by the HEASARC in March 2015 based on an electronic version of Table 3 from the reference paper which was obtained from the CDS as their catalog J/ApJS/216/28 file table3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swxcsoxid.html
bib_reference = 2015ApJS..216...28L
obs_regime = optical
obs_regime = x-ray
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
tap_tablename = swxcsoxid
TIMESTAMP = 1714845743325
ID = nasa.heasarc/swxrt1fgl
publisher_did = ivo://nasa.heasarc/swxrt1fgl
obs_collection = SWXRT1FGL
obs_title = Swift XRT Counterparts to Unidentified 1FGL Sources
obs_description = The authors have analyzed all the archival X-ray data of 134 unidentified (unID) gamma-ray sources listed in the first Fermi/LAT (1FGL) catalog and subsequently followed up by the Swift/XRT. They constructed the spectral energy distributions (SEDs) from radio to gamma-rays for each X-ray source detected, and tried to pick up unique objects that display anomalous spectral signatures. In these analyses, they target all the 1FGL unID sources, using updated data from the second Fermi/LAT (2FGL) catalog on the Large Area Telescope (LAT) position and spectra. In the reference paper, the authors discuss the X-ray identification results and the SEDs of all 134 sources observed with the Swift/XRT. The selection criteria for the Fermi sources were as follows: (1) categorized as unID sources in the 1FGL catalog, (2) localized at high Galactic latitude |b| > 10 degrees, (3) observational data were made public by October 2011, and (4) the positional center of the Swift FoV is within 12 arcminutes of the 1FGL sources. Among 630 unID sources listed in the 1FGL catalog, this selection yielded 134 sources which were analyzed in this study. This table contains the list of the positions and 0.3-10 keV count rates of 267 Swift XRT sources which were detected with a signal-to-noise ratio (SNR) of 3 or more within the Swift/XRT field of views (FoV) of 112 of the 134 1FGL unID gamma-ray sources, with 22 of the 1FGL sources having no detected Swift XRT sources in their FoVs. The Swift XRT images of all 134 unID gamma-ray sources, the positions of the significant XRT sources, and the 95% 1FGL and 2FGL error ellipses are shown in Figure 11 of the reference paper. This table was created by the HEASARC in September 2014 based on an electronic version of Table 4 from the reference paper which was obtained from the ApJS website. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/swxrt1fgl.html
bib_reference = 2013ApJS..208...25T
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=swxrt1fgl&
tap_tablename = swxrt1fgl
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743337
ID = nasa.heasarc/sxdscat
publisher_did = ivo://nasa.heasarc/sxdscat
obs_collection = SXDSCAT
obs_title = Subaru/XMM-Newton Deep Survey X-Ray Source List
obs_description = This table contains the X-ray source catalog in the Subaru/XMM-Newton Deep Survey (SXDS). A continuous area of 1.14 deg<sup>2</sup> centered at R.A.= 02h 18m and Dec =- 05 degrees is mapped by seven pointings with XMM-Newton covering the 0.2 - 10 keV band. From the combined images of the EPIC pn and MOS cameras, the authors have detected 866, 1114, 645, and 136 sources with sensitivity limits of 6 x 10<sup>-16</sup>, 8 x 10<sup>-16</sup>, 3 x 10<sup>-15</sup>, and 5 x 10<sup>-15</sup> ergs cm<sup>-2</sup> s<sup>-1</sup> in the 0.5 - 2, 0.5 - 4.5, 2 - 10, and 4.5 - 10 keV bands, respectively, with detection likelihood >=7 (corresponding to a confidence level of 99.91%). The catalog consists of 1245 sources in total, including 32 extended-source candidates. The averaged log N-log S relations are in good agreement with previous results, bridging the flux range between Chandra deep surveys and brighter surveys. The log N-log S relations show significant spatial variation among pointings on a scale of 0.2 deg<sup>2</sup>. Analyzing the autocorrelation function, the authors detect significant clustering signals from the 0.5 - 2 keV band sample, which can be fit with a power-law form (theta/theta<sub>c</sub>)<sup>(-0.8)</sup> with a correlation length of theta<sub>c</sub> of 5.9 (+1.0, -0.9) arcsec when the integral constraint term is included. In the 2 - 10 keV band, however, the clustering is not significant, with a 90% upper limit of theta<sub>c</sub> < 1.5 arcsec. This table was created by the HEASARC in November 2008 based on an electronic version of Table 2 of the reference paper obtained from the Astrophysical Journal website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sxdscat.html
bib_reference = 2008ApJS..179..124U
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sxdscat&
tap_tablename = sxdscat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743349
ID = nasa.heasarc/symbiotics
publisher_did = ivo://nasa.heasarc/symbiotics
obs_collection = Symbiotics
obs_title = Symbiotic Stars Catalog
obs_description = This database table contains a catalog of confirmed and suspected symbiotic stars. The list includes 188 symbiotic stars as well as 30 objects suspected of being symbiotic. For each star, basic observational material is presented: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radio observations. Also listed are the spectral type of the cool component, the maximum ionization potential observed, references to finding charts, spectra, classifications and recent (as of 2000) papers discussing the physical parameters and nature of each object. This table does NOT contain the information on orbital photometric ephemerides and orbital elements of known symbiotic binaries, pulsational periods for symbiotic Miras, Hipparcos parallaxes and information about outbursts and flickering that is contained in the printed version of the catalog (see Tables 3-7 in the paper for this material). This table was created by the HEASARC in November 2005 based on 4 CDS tables (table1.dat, table1b.dat, table2.dat, table2b.dat) from the directory J/A+AS/146/407/. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/symbiotics.html
bib_reference = 2000A&AS..146..407B
obs_regime = optical
obs_regime = radio
obs_regime = infrared
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=symbiotics&
tap_tablename = symbiotics
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743361
ID = nasa.heasarc/sza31ghz
publisher_did = ivo://nasa.heasarc/sza31ghz
obs_collection = SZA31GHZ
obs_title = Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog
obs_description = This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg<sup>2</sup> of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(>S) = (27.2 +/- 2.5) deg<sup>-2</sup> * (S<sub>mJy</sub>)<sup>(-1.18 +/- 0.12)</sup> over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg<sup>-2</sup>, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15. This table was created by the HEASARC in June 2102 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/716/521">CDS Catalog J/ApJ/716/521</a> file table3.dat. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/sza31ghz.html
bib_reference = 2010ApJ...716..521M
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=sza31ghz&
tap_tablename = sza31ghz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743369
ID = nasa.heasarc/tartarus
publisher_did = ivo://nasa.heasarc/tartarus
obs_collection = ASCA/AGN
obs_title = Tartarus: Reduced ASCA AGN Data (Version 3.1)
obs_description = The Tartarus database contains the results of a detailed but systematic analysis of ASCA observations of active galactic nuclei (AGN). It contains source and background events files, spectra, ancillary response files and response matrices, images, and assorted light curves for a large number of ASCA AGN observations. Spectral fit results are done by automatic XSPEC fitting. This database table allows easy access to reduced AGN data for the whole community, allowing the maximum scientific return from the data. Availability of publishable light curves, images, and spectra (which can also be readily re-fitted) should be particularly valuable to astronomers with little direct experience in the reduction of X-ray data. Version 3.1 has been created by analyzing all ASCA observing sequences with targets designated as AGN, as indicated by a leading "7" in the ASCA observing sequence number. Version 3.1 contains products for all 611 observing sequences designated as AGN observations. This is a significant improvement over Versions 1 and 2. Moreover, the 611 sequences for which products are available are complete in the sense that either the target object was not detected (in which case an upper limit on GIS2 source counts is given) or the intended AGN target was detected and the data were fully analyzed. In order to obtain the most accurate background subtraction and minimize contamination from any nearby sources, version 3.1 makes more use of custom extraction regions than previous versions. It is expected that version 3.1 will be replaced when the final ASCA calibration is completed. This database table has been created by the Tartarus Team, and they, rather than Imperial College London or the HEASARC, are responsible for the contents. It was ingested by the HEASARC in August, 2005. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/tartarus.html
bib_reference = 2001AIPC..599..991T
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=tartarus&
tap_tablename = tartarus
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
sia_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=tartarus&
sia2_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=tartarus&
sia2_glutag = SIA2
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743393
ID = nasa.heasarc/taurusxmm
publisher_did = ivo://nasa.heasarc/taurusxmm
obs_collection = TAURUSXMM
obs_title = Taurus Molecular Cloud XMM-Newton X-Ray Source Catalog
obs_description = The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST) surveys the most populated ~5 square degrees of the Taurus Molecular Cloud, using the XMM-Newton X-ray observatory to study the thermal structure, variability, and long-term evolution of hot plasma, to investigate the magnetic dynamo, and to search for new potential members of the association. The authors present overall correlations with fundamental stellar parameters that were derived from the previous literature. The present overview paper introduces the project and provides the basic results from the X-ray analysis of all sources detected in the XEST survey. Comprehensive tables in the published paper summarize the stellar properties of all the targets surveyed. The survey goes deeper than previous X-ray surveys of Taurus by about an order of magnitude and for the first time systematically accesses very faint and strongly absorbed TMC objects. The authors find a detection rate of 85% and 98% for classical and weak-line T Tauri stars (CTTS and WTTS), respectively, and identify about half of the surveyed protostars and brown dwarfs. Overall, 136 out of 169 surveyed stellar systems were detected. The authors describe an X-ray luminosity vs. mass correlation, discuss the distribution of X-ray-to-bolometric luminosity ratios, and show evidence for lower X-ray luminosities in CTTS compared to WTTS. The complete catalog of all X-ray sources (stellar and non-stellar) detected in the 28 XEST fields is presented in this table. The catalog provides X-ray coordinates, their uncertainties, X-ray count rates and their uncertainties, and X-ray hardness ratios for 2347 detected X-ray sources. If two XEST fields overlap, the same sources may have been identified twice, with different XEST IDs assigned, notice. This table was created by the HEASARC in July 2007 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/468/353">CDS Catalog J/A+A/468/353</a> file table14.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/taurusxmm.html
bib_reference = 2007A&A...468..353G
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=taurusxmm&
tap_tablename = taurusxmm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743405
ID = nasa.heasarc/td1
publisher_did = ivo://nasa.heasarc/td1
obs_collection = TD1
obs_title = TD1 Stellar Ultraviolet Fluxes Catalog
obs_description = The Belgian/UK Ultraviolet Sky Survey Telescope (S2/68) in the ESRO TD1 satellite carried out a controlled scan of the entire sky. It measured the absolute ultraviolet flux distribution between 2740A and 1350A of point sources down to 10th visual magnitude for unreddened early B stars. The S2/68 experiment has been described by Boksenberg et al. (1973MNRAS.163..291B), and the absolute calibration by Humphries et al. (1976A&A....49..389H). The TD1 Catalog of Stellar Ultraviolet Fluxes represents results from the sky-scan experiment on the TD1 satellite of the European Space Research Organization (ESRO), now part of ESA. It lists the absolute fluxes, in four passbands, for 31,215 stars: <pre> Passband Center: 274.0nm 236.5nm 196.5nm 156.5nm Effective Width: 31.0nm 33.0nm 33.0nm 33.0nm </pre> The stars have been selected subject to the constraint that the signal-to-noise ratio should be at least 10.0 in any one of the four passbands. Null values of a flux field and an error field indicate there are no valid data for the star. This usually arises with close pairs of stars whose spectra overlap. Five standard flux error values are greater than 99.99, and were too large for the format of the flux field in the original table. Thus, the flux error values which were greater than 99.99 are given as 99.99. Many of the fainter stars of spectral type later than A5 do not have significant signals in all of the spectrophotometric channels (particularly the 1565A channel). Consequently, after the removal of the background, they can randomly give rise to small negative values of flux. Those negative values were not suppressed, but are given together with their error, as they can be significant when considered as part of a statistical sample. Although the sky coverage is essentially complete, the catalog does not contain the fluxes for all stars that fall within the limit of the sensitivity of the instrument. If any star expected to be present is missing, then its signal is probably blended with that of a nearby star, in which case the data have been discarded. The original contents of the HEASARC's TD1 database table came from a magnetic tape sent to NASA/Goddard Space Flight Center by Dr. G.I. Thompson of the Royal Observatory in Edinburgh, Scotland. The HEASARC recreated this database table in August 2005, based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/59B">CDS Catalog II/59B</a> file catalog.dat.gz, in an effort to modernize its parameter names and documentation, as well as to add Galactic coordinates. The data in the CDS version originally came from "Selected Astronomical Catalogs" Vol. 1 CD-ROM released by the NASA Astronomical Data Center (ADC) in 1991. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/td1.html
bib_reference = 1978csuf.book.....T
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=td1&
tap_tablename = td1
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743417
ID = nasa.heasarc/tevcat
publisher_did = ivo://nasa.heasarc/tevcat
obs_collection = TEVCAT
obs_title = TeV Gamma-Ray Source Catalog
obs_description = TeVCat (<a href="http://tevcat.uchicago.edu/">http://tevcat.uchicago.edu/</a>) is an online, interactive catalog for very-high-energy (VHE: energies, E >~ 50 GeV) gamma-ray astronomy. As VHE astronomy continues to grow, the usefulness of a one-stop clearing house for information on new sources is increasingly evident. TeVCat is intended to be such a resource. With sky maps, scientific information, visibility plotters and linked references available at the website, it will help the wider gamma-ray community stay up-to-date and informed on this exciting and rapidly developing field. This HEASARC database table provides the TeVCat list of VHE sources as well as links to the TeV source resource pages on the TeVCat website. The catalog and <a href="http://tevcat.uchicago.edu/">the website at the University of Chicago</a> are maintained by Scott Wakely and Deirdre Horan. This table was first ingested by the HEASARC in July 2017 based on the catalog of VHE gamma-ray sources available at <a href="http://tevcat.uchicago.edu/">http://tevcat.uchicago.edu/</a>. It is updated automatically within a few days of the catalog being updated on the University of Chicago website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/tevcat.html
bib_reference = 2008ICRC....3.1341W
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=tevcat&
tap_tablename = tevcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743425
ID = nasa.heasarc/texas
publisher_did = ivo://nasa.heasarc/texas
obs_collection = Texas
obs_title = Texas Survey of Radio Sources at 365 MHz
obs_description = This catalog is from the Texas Survey of discrete radio sources between -35.5 degrees and +71.5 degrees declination (B1950), which was carried out at a frequency of 365 MHz (82 cm wavelength) with the Texas Interferometer during the period from 1974 to 1983. The Survey lists accurate positions with internal errors of about an arcsecond, flux densities (which for strong point sources have internal errors of about 1% and total errors of about 5%), simple structure models and indications of spectrum and variability for 66841 sources. Results of comparisons with other data show that the Survey is 90% complete at 0.4 Jy and 80% complete at 0.25 Jy, is nearly free from spurious sources, and has a lobeshift incidence which is reasonably described by quality flags associated with each source. The University of Texas Radio Astronomy Observatory (UTRAO) carried out, with the Texas Interferometer, this 365 MHz survey of the sky, which was intended to be complete to a flux density level of 0.25 Jy, to provide positions with an accuracy of about 1 arcsec in both coordinates, to give accurate flux densities and indication of source variability, and to give rough structure models for each source. The observations began in 1974 and were completed in 1983. A preliminary version of one declination strip was published (Douglas et al., Publ. Dept. Astron. Univ. Texas, No. 17, Oct. 1980), and a number of intermediate versions of the survey were privately circulated for various purposes, pending completion of the final analysis and adjustment of the data. This database was created by the HEASARC in February 2001, based on CDS/ADC catalog VIII/42. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/texas.html
bib_reference = 1996AJ....111.1945D
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=texas&
tap_tablename = texas
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743437
ID = nasa.heasarc/tgs
publisher_did = ivo://nasa.heasarc/tgs
obs_collection = TGS
obs_title = EXOSAT TGS L and R Orders
obs_description = Spectra obtained using the EXOSAT transmission grating spectrometer, TGS. There are two databases TGS and TGS2 as follows: <pre> * TGS - the grating spectra averaged over the positive and negative orders * TGS2 - the postive and negative orders kept separate </pre> TGS provides a better overview of the spectrum, and is quicker to use with a spectral fitting program. This is the default that most users will want to use. Once a user has become more expert and wants to see, for example, if a subtle feature is present in both halves of the grating spectra, the user can access TGS2. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/tgs.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=tgs&
tap_tablename = tgs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743449
ID = nasa.heasarc/tgs2
publisher_did = ivo://nasa.heasarc/tgs2
obs_collection = TGS2
obs_title = EXOSAT TGS Spectra and Lightcurves
obs_description = Spectra obtained using the EXOSAT transmission grating spectrometer, TGS. There are two databases TGS and TGS2 as follows: <pre> * TGS - the grating spectra averaged over the positive and negative orders * TGS2 - the postive and negative orders kept separate </pre> TGS provides a better overview of the spectrum, and is quicker to use with a spectral fitting program. This is the default that most users will want to use. Once a user has become more expert and want to see, for example, if a subtle feature is present in both halves of the grating spectra, the user can access TGS2. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/tgs2.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=tgs2&
tap_tablename = tgs2
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743457
ID = nasa.heasarc/tramisuboo
publisher_did = ivo://nasa.heasarc/tramisuboo
obs_collection = TRAMISUBOO
obs_title = Two-Meter Radio Mini Survey (T-RaMiSu) of the Bootes Field
obs_description = This table contains results from wide-area, deep, high-resolution 153-MHz GMRT observations of the NOAO Bootes field, adding to the extensive, multi-wavelength data of this region. The observations, data reduction, and catalog construction and description are described in the reference paper. The seven pointings (listed in Table 2 of the reference paper) produced a final mosaic covering 30 square degrees with a resolution of 25". The rms noise is 2 mJy/beam in the center of the image, rising to 4-5 mJy/beam at the edges, with an average of 3 mJy/beam. Seventy-five per cent of the area has an rms < 4 mJy/beam. The extracted source catalog contains 1289 sources detected at 5 sigma at flux densities between 4.1 mJy and 7.3 Jy, of which 453 are resolved. The authors estimate the catalogue to be 92% reliable and 95% complete at an integrated flux density limit of 14 mJy. The flux densities and astrometry have been corrected for systematic errors. In their paper, the authors calculate the differential source counts which are in good agreement with those in the literature and provide an important step forward in quantifying the source counts at these low frequencies and low flux densities. The GMRT 153-MHz sources have been matched to the 1.4-GHz NVSS and 327-MHz WENSS catalogs and spectral indices were derived. The source catalog presented here is derived from seven 4 hour pointings with the GMRT at 153 MHz, centered on the NOAO Bootes field. The resulting 30 square degree image has a central noise level of 2 mJy/beam and a resolution of 25". This table contains entries for all 1289 detected 153-MHz radio sources as well as for the 160 Gaussian components of the 77 sources (71 doubles and 3 triples) which could be fit by multiple Gaussian components, making a total of 1449 entries. This table was created by the HEASARC in January 2013 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/549/A55">CDS Catalog J/A+A/549/A55</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/tramisuboo.html
bib_reference = 2013A&A...549A..55W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=tramisuboo&
tap_tablename = tramisuboo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743469
ID = nasa.heasarc/trifidcxo
publisher_did = ivo://nasa.heasarc/trifidcxo
obs_collection = TRIFIDCXO
obs_title = Trifid Nebula (M 20) Chandra X-Ray Point Source Catalog
obs_description = This table contains a list of the Trifid Nebula (M 20) X-Ray point sources detected by the Chandra X-ray Observatory (CXO) in an observation carried out on 2002 June 13. The Trifid Nebula, a young star-forming H II region, was observed for 16 hr by the Advanced CCD Imaging Spectrometer imaging array, ACIS-I, detector. 304 X-ray sources were detected, 30% of which are hard sources (defined as those sources having a 0.5-2.0 keV to 2.0-8.0 keV hardness ratio > -0.2) and 70% of which have near-infrared counterparts. This table was created by the HEASARC in January 2007 based on CDS table J/ApJ/607/904/table1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/trifidcxo.html
bib_reference = 2004ApJ...607..904R
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=trifidcxo&
tap_tablename = trifidcxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743477
ID = nasa.heasarc/twodfqsoz
publisher_did = ivo://nasa.heasarc/twodfqsoz
obs_collection = TWODFQSOZ
obs_title = 2dF QSO Redshift (2QZ) Survey
obs_description = The final catalog of the 2dF QSO Redshift Survey (2QZ) is based on Anglo-Australian Telescope 2dF spectroscopic observations of 44,576 color-selected (u, b<sub>J</sub>, r) objects with 18.25 < b<sub>J</sub> < 20.85 selected from automated plate measurement scans of UK Schmidt Telescope (UKST) photographic plates. The 2QZ comprises 23,338 quasi-stellar objects (QSOs), 12,292 galactic stars (including 2,071 white dwarfs) and 4,558 compact narrow emission-line galaxies. The authors obtained a reliable spectroscopic identification for 86 per cent of objects observed with 2dF. They also report on the 6dF QSO Redshift Survey (6QZ), based on UKST 6dF observations of 1,564 brighter (16 < b<sub>J</sub> < 18.25) sources selected from the same photographic input catalog. In total, the authors identified 322 QSOs spectroscopically in the 6QZ. The completed 2QZ is, by more than a factor of 50, the largest homogeneous QSO catalog ever constructed at these faint limits (b<sub>J</sub> < 20.85) and high QSO surface densities (35 QSOs/deg<sup>2</sup>). As such, it represents an important resource in the study of the Universe at moderate-to-high redshifts. The survey area comprised 30 UKST fields, arranged in two 75 degrees by 5 degrees declination strips, one passing across the South Galactic Gap centered on Dec = -30 degrees (the SGP strip), and the other across the North Galactic Gap centered on Dec = 0 degrees (referred to in the reference paper as the equatorial strip, but also known as the NGP strip. The total survey area is 721.6 deg<sup>2</sup>, when allowance is made for regions of sky excised around bright stars. Spectroscopic observations of the input catalogue were made with the 2dF instrument at the Anglo-Australian Telescope (AAT; the 2QZ sample) and the 6dF instrument at the UKST (the 6QZ sample). 2dF spectroscopic observations began in January 1997 and were completed in April 2002. Six-degree Field observations were performed over the period 2001 March-2002 September. This online catalog was created by the HEASARC in October 2010 based on the machine-readable table 2qz.dat obtained from the CDS (their catalog VII/241). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/twodfqsoz.html
bib_reference = 2004MNRAS.349.1397C
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=twodfqsoz&
tap_tablename = twodfqsoz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743489
ID = nasa.heasarc/twomassrsc
publisher_did = ivo://nasa.heasarc/twomassrsc
obs_collection = TWOMASSRSC
obs_title = 2MASS Redshift Survey (2MRS) Catalog
obs_description = This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K<sub>s</sub> <= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K<sub>s</sub> <= 11.75 mag and |b| >= 5 degrees (>= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h<sup>-1</sup> Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K<sub>s</sub> <= 11.25 mag and |b| >= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: <pre> K<sub>s</sub> <= 11.75 mag and detected at H, E(B - V) <= 1 mag, |b| >= 5 degrees for 30 degrees < l < 330 degrees, |b| >= 8 degrees otherwise. </pre> They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented. This table was created by the HEASARC in April 2012 based on an electronic version of Table 3 of the reference paper which was obtained from the ApJS website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/twomassrsc.html
bib_reference = 2012ApJS..199...26H
obs_regime = infrared
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=twomassrsc&
tap_tablename = twomassrsc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743501
ID = nasa.heasarc/twosigma
publisher_did = ivo://nasa.heasarc/twosigma
obs_collection = Einstein/ETS
obs_title = Einstein Two-Sigma Catalog
obs_description = The X-ray sources from observations made with the Einstein Observatory (HEAO-2) Imaging Proportional Counter (IPC) that have intensities of 2-sigma or more above the background are compiled in this catalog. This catalog covers more sky at fainter flux levels than the Einstein Medium Sensitivity Survey. Fields with diffuse emission sources such as bright Abell clusters of galaxies and supernova remnants were excluded. Thus, data within 10 degrees of the galactic plane as well as fields within the boundaries of the Magellanic Clouds were excluded. Regions crowded with galactic sources such as the Orion and Pleiades fiels were also excluded. Excluding redundant fields, this catalog covers 1850 sq. degrees of the sky. The generation of the Einstein Two-Sigma Catalog was described in detail by Moran et al. (1996). Please read this article carefully to ensure responsible use of the Catalog. Detailed scientific and technical questions on the contents and methodology of this catalog should be addressed to the first author, Ed Moran (edhed@igpp.llnl.gov). In particular, it should be noted that, by design, this catalog contains a significant number of spurious sources: only 28%, or about 13,000 sources, out of the 46,000 source in the 2-sigma catalog are `real` astrophysical sources, with the remainder of the sources being spurious ones. Moran et al. show in their paper that performing cross-correlations of 2-sigma sources with other catalogs is an effective way of selecting sources in this catalog that are probably real. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/twosigma.html
bib_reference = 1996ApJ...461..127M
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=twosigma&
tap_tablename = twosigma
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743517
ID = nasa.heasarc/tycho2
publisher_did = ivo://nasa.heasarc/tycho2
obs_collection = Tycho-2
obs_title = Tycho-2 Catalog of the 2.5 Million Brightest Stars
obs_description = The Hipparcos and Tycho catalogs are the primary products of the European Space Agency's astrometric mission, Hipparcos. The satellite, which operated for four years, returned high quality scientific data from November 1989 to March 1993. The Tycho-2 catalog is an astrometric reference catalog containing positions and proper motions as well as two-color photometric data for the 2.5 million brightest stars in the sky. The Tycho-2 positions and magnitudes are based on precisely the same observations as the original Tycho catalog (hereafter Tycho-1; see <a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/239">CDS Cat. I/239</a>) collected by the star mapper of the ESA Hipparcos satellite, but Tycho-2 is much bigger and slightly more precise, owing to a more advanced reduction technique. Components of double stars with separations down to 0.8 arcsec are included. Proper motions precise to about 2.5 mas/yr are given as derived from a comparison with the Astrographic Catalogue and 143 other ground-based astrometric catalogs, all reduced to the Hipparcos celestial coordinate system. Tycho-2 supersedes in most applications Tycho-1, as well as the ACT (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/246">CDS Cat. I/246</a>) and the TRC (CDS Cat. I/250) catalogs based on Tycho-1. Supplement-1 (not part of this HEASARC database but available at <a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/259/suppl_1.dat.gz">https://cdsarc.cds.unistra.fr/ftp/cats/I/259/suppl_1.dat.gz</a>) lists stars from the Hipparcos and Tycho-1 catalogs which are not in Tycho-2. Supplement-2 (not part of this HEASARC database but available at <a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/259/suppl_2.dat.gz">https://cdsarc.cds.unistra.fr/ftp/cats/I/259/suppl_2.dat.gz</a>) lists 1146 Tycho-1 stars which are probably either false or heavily disturbed. The principal characteristics of the Tycho-2 catalog are summarized below. By means of proper motions the positions are transferred to the year 2000.0, the epoch of the catalog. The median values of internal standard errors are given: <pre> Mean satellite observation epoch ~J1991.5 Epoch of the Tycho-2 catalog J2000.0 Reference system ICRS coincidence with ICRS (1) +/-0.6 mas deviation from inertial (1) +/-0.25 mas/yr Number of entries 2,539,913 Astrometric standard errors (2) V_T < 9 mag 7 mas all stars, positions 60 mas all stars, proper motions 2.5 mas/yr Photometric std. errors (3) on V_T V_T < 9 mag 0.013 mag all stars 0.10 mag Star density b= 0 deg 150 stars/sq.deg. b= +/-30 deg 50 stars/sq.deg. b= +/-90 deg 25 stars/sq.deg. Completeness to 90 per cent V ~ 11.5 mag Completeness to 99 per cent V ~ 11.0 mag Number of Tycho observations ~300 10<sup>6</sup> Note (1): about all 3 axes Note (2): ratio of external to internal standard errors is ~1.0 for positions and for proper motions. Systematic errors are less than 1 mas and 0.5 mas/yr Note (3): ratio of photometric external to internal standard errors at V_T > 9 mag is below 1.5 </pre> For more information on the original catalog, please consult the Tycho-2 home page at <a href="http://www.astro.ku.dk/~erik/Tycho-2">http://www.astro.ku.dk/~erik/Tycho-2</a> For more information on the HEASARC implementation of the Tycho-2 catalog, please consult <a href="#heasarc_implementation">the "HEASARC Implementation" section</a> of this help. This database table was created at the HEASARC in June 2000 based on the ADC/<a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/259">CDS Catalog I/259</a>, using the file tyc2.dat. Galactic coordinates (calculated by converting the observed ICRS Equatorial positions) were added to this HEASARC database table in August 2005. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/tycho2.html
bib_reference = 2000A&A...355L..27H
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=tycho2&
tap_tablename = tycho2
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743525
ID = nasa.heasarc/uc7c151mhz
publisher_did = ivo://nasa.heasarc/uc7c151mhz
obs_collection = UC7C151MHZ
obs_title = 7C Catalog 151-MHz Survey Final Unified Source Catalog
obs_description = This table contains a final unified catalog for the 7C survey at 151 MHz with a spatial resolution of 70 x 70cosec(Dec) arcsec<sup>2</sup>. This has been constructed by amalgamating the existing catalogs derived from individual fields imaged at this resolution and eliminating redundancy in regions of mutual overlap. This was a non-trivial procedure because the flux in multiple-component sources may be fitted differently on alternative images, owing, for example, to differences in local noise and beam distortion. The final catalog as published thus produced contains 43683 sources. (Note that the HEASARC removed one duplicate source entry for '7C 083231.6+262635' since it had two entries, which were identical except that in one the beam-fitted flux density S<sub>bf</sub> was 834 mJy/beam, while, in the other entry now removed, S<sub>bf</sub> was 840 mJy/beam). Separate final catalogs have been previously published for the 7C Galactic Plane 7CG survey (available as the HEASARC table GP7C151MHZ), and the lower-resolution survey of the low-declination strip 9<sup>h</sup> < RA < 16<sup>h</sup>, 20<sup>o</sup> < Dec < 35<sup>o</sup> (available as the HEASARC table LD7C151MHZ). The individual catalogs for about 40 of the 96 regions contributing to the total have already been published, together with full details of the methodology, in MNRAS or A&AS: <pre> Reference Region Lacy et al. 1995, MNRAS, 276, 614 92 Visser et al. 1995, A&AS, 110, 419 93 Pooley et al. 1998, MNRAS, 298, 637 94-96 Riley et al. 1999, MNRAS, 306, 31 1-33 </pre> and these data are also available via the MRAO website: <a href="http://www.mrao.cam.ac.uk/surveys/7C/">http://www.mrao.cam.ac.uk/surveys/7C/</a> Individual catalogs for the remaining 58 regions by Riley et al. (regions 34-91) were released electronically via the MRAO website in November 2001. These include a re-analysis of data originally published in rather a different parametrization by McGilchrist et al. 1990, MNRAS, 246, 110. The regions re-analyzed are those numbered 41, 44, 59, 60, 62 and 63 and they supersede McGilchrist's 1990 publication. The RA x Dec coverage, the average rms noise, the flux density of the faintest source listed and the completeness limit for each of the individual regions contributing to the final catalog are given in the table <a href="http://cdsarc.u-strasbg.fr/ftp/cats/J_MNRAS/382/1639/regions.dat">http://cdsarc.u-strasbg.fr/ftp/cats/J_MNRAS/382/1639/regions.dat</a>. For further details of the surveys and data analysis procedures please refer to the published papers referenced above and other references contained therein. This table was created by the HEASARC in October 2010 based on CDS table J/MNRAS/382/1639 files 7c.dat and regions.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/uc7c151mhz.html
bib_reference = 2007MNRAS.382.1639H
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=uc7c151mhz&
tap_tablename = uc7c151mhz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743533
ID = nasa.heasarc/ugc
publisher_did = ivo://nasa.heasarc/ugc
obs_collection = UGC
obs_title = Uppsala General Catalog of Galaxies
obs_description = The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950.0 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted. This database table was first ingested by the HEASARC in September 2000 based on a machine-readable version of the UGC obtained from the ADC (ADC Catalog VII/26D). This latter version was a corrected and modified version of the original magnetic tape version of the UGC. A list of the types of changes and modifications made by the ADC is available at <a href="https://cdsarc.u-strasbg.fr/ftp/cats/VII/26D/ReadMe">https://cdsarc.u-strasbg.fr/ftp/cats/VII/26D/ReadMe</a>, while the list of the affected entries is available at <a href="https://cdsarc.u-strasbg.fr/ftp/cats/VII/26D/errors.dat.gz">https://cdsarc.u-strasbg.fr/ftp/cats/VII/26D/errors.dat.gz</a>. <p> The HEASARC last updated this database table in November 2021 upon reflection that the original catalog's coordinates were B1950 (instead of J1950, as originally assumed by the HEASARC). Due to the precision of the coordinates in this catalog, the difference is negligible. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/ugc.html
bib_reference = 1973UGC...C...0000N
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=ugc&
tap_tablename = ugc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743553
ID = nasa.heasarc/uhuru4
publisher_did = ivo://nasa.heasarc/uhuru4
obs_collection = UHURU4
obs_title = Uhuru Fourth (4U) Catalog
obs_description = The Fourth Uhuru (4U) Catalog lists 339 X-ray sources that were observed with the Uhuru (SAS A) X-ray observatory. It contains positional information in the form of 90% confidence level error boxes, 2-6 keV intensities, possible optical and radio counterparts, and alternative names for sources observed in earlier compilations. The major classes of identified objects include binary stellar systems, supernova remnants, Seyfert galaxies, clusters of galaxies, and possibly the new class of superclusters of galaxies. The Uhuru satellite was a scanning X-ray instrument with a narrow (1 by 10 degree FWFM) and a wide (10 by 10 degree FWFM) collimator (cf. Giacconi et al. 1971, ApJ, 165, L27). Typically, the scan rate was 0.5 degree/second, with the spin axis in one position for roughly one day. During the interval for which the spin axis was fixed, repeated scans were made of the same 10 by 360 degrees band of the sky. For this catalog, the individual scans were superposed using aspect data from an orthogonally mounted triad of magnetometers and a Sun sensor onboard the spacecraft, supplemented by observations of well-located X-ray sources. The observations employed in producing this catalog were obtained over a total of 429 days between 1970 December 12 and 1973 March 18, apart from a gap between 1972 July and December when the spacecraft's transmitter was operating improperly. This online catalog was created by the HEASARC in March 2003 based on a table obtained originally from the ADC website (<a href="https://heasarc.gsfc.nasa.gov/FTP/heasarc/dbase/misc_files/uhuru4/4u.dat">https://heasarc.gsfc.nasa.gov/FTP/heasarc/dbase/misc_files/uhuru4/4u.dat</a>), which was modified by the HEASARC to include some parameters that were in the published catalog (Table 1 in the reference) but were not in the ADC table. The HEASARC made a small number of other changes and corrections to the table which are listed in the HEASARC_Implementation section of this help. Notice that the ADC table itself differs in a number of respects from the published Table 1, e.g., the comments are sometimes abbreviated and/or different, some of the names are slightly different (usually by one digit in the RA minutes part), and three of the entries have differing names and positions. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/uhuru4.html
bib_reference = 1978ApJS...38..357F
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=uhuru4&
tap_tablename = uhuru4
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743601
ID = nasa.heasarc/uit
publisher_did = ivo://nasa.heasarc/uit
obs_collection = UIT
obs_title = Ultraviolet Imaging Telescope Near-UV Bright Objects Catalog
obs_description = The Ultraviolet Imaging Telescope (UIT) Near-UV Bright Objects Catalog is a photometric catalog of 2244 objects detected by the UIT in the near-ultraviolet (NUV; 1650A<lambda<2900A) during the Astro-1 Space Shuttle mission. Sources in the catalog are as faint as near-UV magnitude m_nuv of about 18.8, or near-UV flux f_nuv ~ 1.1x10^-16ergs/s/cm^2/A, but the survey is not complete to this level. Optical catalogs were used to cross identify sources and derive near-UV to Johnson V colors. A majority of the objects (88%) do indeed have proposed optical identifications from catalogs, and most are stars. The authors' purpose in creating the catalog was to form a database useful for identifying very blue objects and for performing Galactic UV stellar population studies. This database was created by the HEASARC in November 2000 based on a machine-readable version obtained from the CDS (Catalog J/ApJS/104/287). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/uit.html
bib_reference = 1996ApJS..104..287S
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=uit&
tap_tablename = uit
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743613
ID = nasa.heasarc/uitmaster
publisher_did = ivo://nasa.heasarc/uitmaster
obs_collection = UITMASTER
obs_title = Ultraviolet Imaging Telescope Master Catalog
obs_description = The Ultraviolet Imaging Telescope (UIT) was one of three ultraviolet telescopes on the ASTRO-1 mission flown on the Space Shuttle Columbia during the period of 2 - 10 December 1990. The same three instruments were later flown on the Space Shuttle Endeavour during 3 - 17 March 1995, as part of the ASTRO-2 mission. Exposures were obtained on 70-mm photographic film in the 1200-3300 Angstrom range using broadband filters and later digitized using a Perkin-Elmer microdensitometer. The image resolution was 3 arcseconds over a 40 arcminute field of view and images of targets as faint as 21st (ultraviolet) magnitude were recorded. Overall, the UIT-1 mission obtained 821 exposures of 66 targets (361 near-UV and 460 far-UV), and UIT-2 obtained 758 images of 193 targets (all far-UV), for a total of 1579 exposures. This table contains only 1481 rows, 777 UIT-1 exposures (347 near-UV and 430 far-UV) and 704 UIT-2 exposures (all far-UV), implying that 98 exposures are 'missing' from this table. This table was created by the HEASARC in April 2012 based on CDS Catalog VI/104 file uitlist.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/uitmaster.html
bib_reference = 1997PASP..109..584S
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=uitmaster&
tap_tablename = uitmaster
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743633
ID = nasa.heasarc/ulxngcat
publisher_did = ivo://nasa.heasarc/ulxngcat
obs_collection = ULXNGCAT
obs_title = Ultraluminous X-Ray Sources in Nearby Galaxies Catalog
obs_description = One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10<sup>39</sup> erg s<sup>-1</sup> are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 < log (M/M<sub>sun</sub>) < 11.4, and in star formation rate, 0.0002 < SFR(M<sub>sun</sub> yr<sup>-1</sup>) <= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10<sup>10</sup> M<sub>sun</sub>, one per ~0.5 M<sub>sun</sub> yr<sup>-1</sup> star formation rate, and one per 57 Mpc<sup>3</sup> corresponding to a luminosity density of ~2 x 10<sup>37</sup> erg s<sup>-1</sup> Mpc<sup>-3</sup>. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10<sup>39</sup> erg s<sup>-1</sup> with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L<sub>X</sub> ~ 10<sup>41</sup> erg s<sup>-1</sup>, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10<sup>41</sup> erg s<sup>-1</sup>, requiring a new population class to explain these extreme objects. This table was created by the HEASARC in November 2011 based on an electronic version of Table 1 from the reference paper that was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/ulxngcat.html
bib_reference = 2011ApJ...741...49S
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=ulxngcat&
tap_tablename = ulxngcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743641
ID = nasa.heasarc/ulxrbcat
publisher_did = ivo://nasa.heasarc/ulxrbcat
obs_collection = ULXRB
obs_title = Ultraluminous X-Ray Sources in External Galaxies Catalog
obs_description = This table is a catalog of ultraluminous X-ray sources (ULXs) in external galaxies, where ULXs have been defined as compact, off-nuclear X-ray sources with X-ray luminosities in the range of 10<sup>39</sup> - 10<sup>41</sup> erg/s. The aim of this catalog is to provide easy access to the properties of ULXs, their possible counterparts at other wavelengths (optical, IR, and radio), and the properties of their host galaxies. The catalog contains 229 ULXs found in 85 galaxies which had been reported in the astronomy literature as of April 2004. Most ULXs are stellar-mass-black hole X-ray binaries, but it cannot be excluded that some ULXs might be intermediate-mass black holes. A small fraction of the candidate ULXs might be background Active Galactic Nuclei (AGN) or Supernova Remnants (SNRs). ULXs with luminosity above 10<sup>40</sup> erg/s are found in both starburst galaxies and in the halos of early-type galaxies. Some notes on individual galaxies and/or ULXs in this catalog can be found in the file <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/429/1125/notes.dat">https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/429/1125/notes.dat</a> which is available at the CDS. This table was created by the HEASARC in January 2005, based on CDS tables J/A+A/429/1125/table1a.dat and table1b.dat. It was updated in September 2012 to correct an error in the declination signs of the NGC 253 objects. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/ulxrbcat.html
bib_reference = 2005A&A...429.1125L
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=ulxrbcat&
tap_tablename = ulxrbcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743661
ID = nasa.heasarc/upprscoxmm
publisher_did = ivo://nasa.heasarc/upprscoxmm
obs_collection = UPPRSCOXMM
obs_title = Upper Sco XMM-Newton X-Ray Point Source Catalog
obs_description = The authors studied the X-ray emission from young stars by analyzing the deep (a ~53 ks exposure centered at a J2000.0 RA and Dec of 16 14 00.0, -23 00 00 and a ~43 ks exposure at 15 56 25.0, -23 37 47) XMM-Newton observations of two regions of the Upper Scorpius (USco) subgroup of the Scorpius-Centaurus (Sco-Cen) association which is estimated to have an age of 5 Myr. Portions of the USco association were observed in the optical with the CTIO Curtis Schmidt telescope and the Danish 1.54m telescope. This table contains all the X-ray sources detected in the two XMM-Newton observations, as well as their near-IR counterparts from the 2MASS and DENIS catalogs, and their optical counterparts from the CTIO and Danish 1.54 m observations. Based on the near-infrared and optical photometry, 22 Upper Scorpius photometric members have been identified among the 224 detected X-ray sources. This table was created by the HEASARC in March 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/459/199">CDS catalog J/A+A/459/199</a> files tabled1.dat and table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/upprscoxmm.html
bib_reference = 2006A&A...459..199A
obs_regime = infrared
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=upprscoxmm&
tap_tablename = upprscoxmm
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TIMESTAMP = 1714845743673
ID = nasa.heasarc/uvotbscat
publisher_did = ivo://nasa.heasarc/uvotbscat
obs_collection = UVOTBSCAT
obs_title = UVOT Bright Star Catalog
obs_description = This catalog was compiled from 4 catalogs: Tycho-2, GVCS III, NGC, and the Yale Bright Star Catalog. All catalogs were preprocessed before compiling this catalog to achieve uniform columns and units. Next, they were merged into one catalogue before eliminating "red" objects and precessing all coordinates to epoch 2000.0. The catalog was then corrected for missing decimal points. Finally, the catalog was sorted by R.A. for ease of locating objects within the catalogue. The original catalog contained 239,853 objects brighter than 12.0 mags. This table was originally created by the HEASARC in July 2008 based on an input table supplied by the Swift Project which was compiled by Elizabeth Auden at MSSL. It was renamed to UVOTBSCAT in January 2009. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/uvotbscat.html
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=uvotbscat&
tap_tablename = uvotbscat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743681
ID = nasa.heasarc/uvqs
publisher_did = ivo://nasa.heasarc/uvqs
obs_collection = UVQS
obs_title = UV-Bright Quasar Survey (UVQS) DR1 Catalog
obs_description = This table contains data from the first data release (DR1) from the UV-bright Quasar Survey (UVQS) for new z ~ 1 active galactic nuclei (AGN) across the sky. Using simple GALEX UV and WISE near-IR color selection criteria, the authors generated a list of 1,450 primary candidates with FUV < 18.5 mag, that is contained in the HEASARC table (entries with source_sample = 'P'). They obtained discovery spectra, primarily on 3m-class telescopes, for 1,040 of these candidates and confirmed 86% as AGN, with redshifts generally at z > 0.5. Including a small set of observed secondary candidates, the authors report the discovery of 217 AGN with GALEX FUV magnitudes < 18 mag that previously had no reported spectroscopic redshifts. These are excellent potential targets for UV spectroscopy before the end of the Hubble Space Telescope mission. The main data products of UVQS are publicly available through the Mikulski Archive for Space Telescopes (MAST). The authors have performed an all-sky survey for z ~ 1, FUV-bright quasars selected from GALEX and WISE photometry. In several of the observing runs, conditions were unexpectedly favorable and we exhausted the primary candidates at certain right ascension ranges. To fill the remaining observing time, they generated a secondary candidate list. This secondary set of 2,010 candidates is also contained in this HEASARC table (entries with source_sample = 'S'). The authors proceeded to obtain discovery-quality long-slit spectra (i.e., low-dispersion, large-wavelength coverage, modest signal-to-noise ratio (S/N) of their UV-bright Quasar Survey (UVQS) candidates in one calendar year. The principal facilities were: (i) the dual Kast spectrometer on the 3m Shane telescope at the Lick Observatory; (ii) the Boller & Chivens (BCS) spectrometer on the Irenee du Pont 100-inch telescope at the Las Campanas Observatory; and (iii) the Calar Alto Faint Object Spectrograph on the CAHA 2.2-meter telescope at the Calar Alto Observatory (CAHA). They acquired an additional ~20 spectra on larger aperture telescopes (Keck/ESI, MMT/MBC, Magellan/MagE) during twilight or under poor observing conditions. Typical exposure times were limited to < ~200s, with adjustments for fainter sources or sub-optimal observing conditions. Table 3 in the reference paper provides a list of the details of the observations of these candidates. From the total candidates list of 3,460 objects, the authors measured high-quality redshifts (redshift quality flag values of 3 or greater) for 1,121 sources. They assumed that every source with a recessional velocity v<sub>r</sub> = z * c < 500 km s<sup>-1</sup> was "Galactic", which they associate with the Galaxy and members of the Local Group. This included sources where the eigenspectra fits were poor yet a low v<sub>r</sub> was indisputable (e.g., stars). Many of these were assigned z = 0 exactly. The remainder of the UVQS sources were assumed to be extragalactic AGN, and the derived redshift information for these sources (which was given in Table 4 of the reference paper) has been incorporated into this HEASARC representation of UVQS. Finally, there were 93 sources with good-quality spectra for which we cannot the authors could not recover a secure redshift. The majority of these have been previously cataloged as blazars (or BL Lac objects). Table 6 in the reference paper lists the sample of these unknown or insecure redshift objects. This table was created by the HEASARC in April 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/AJ/152/25">CDS Catalog J/AJ/152/25</a> files table1.dat, table2.dat, and table4.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/uvqs.html
bib_reference = 2016AJ....152...25M
obs_regime = optical
obs_regime = uv
obs_regime = infrared
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=uvqs&
tap_tablename = uvqs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743693
ID = nasa.heasarc/uzc
publisher_did = ivo://nasa.heasarc/uzc
obs_collection = UZC
obs_title = Updated Zwicky Catalog
obs_description = The Zwicky Catalog of Galaxies, with a magnitude limit m<sub>Zw</sub> <= 15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~<2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m<sub>Zw</sub> <= 15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr >= RA(1950) <= 4 hr and 8 hr <= RA(1950) <= 17 hr and the declination range -2.5 degrees <= Dec(1950) <= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999). This database was created by the HEASARC in October 2000 based on a machine-readable version obtained from the CDS (Catalog J/PASP/111/438). It was slightly revised in February 2001 (the 'redshift' parameters were renamed as 'radial velocity' parameters to conform with the usage in other similar HEASARC extragalactic catalogs). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/uzc.html
bib_reference = 1999PASP..111..438F
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=uzc&
tap_tablename = uzc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743705
ID = nasa.heasarc/vela5b
publisher_did = ivo://nasa.heasarc/vela5b
obs_collection = VELA5B
obs_title = Vela 5B All-Sky Monitor Lightcurves
obs_description = Data for these sources were obtained from the Vela 5B all-sky XC detector. The Vela 5B nuclear test detection satellite was part of a program run jointly by the Advanced Research Projects of the U.S. Department of Defense and the U.S.Atomic Energy Commission, managed by the U.S. Air Force. It was placed in a nearly circular orbit at a geocentric distance of ~118,000 km on 23 May 1969; the orbital period was ~112 hours. The satellite rotated about its spin axis with a ~64-sec period. The X-ray detector was located ~90 degrees from the spin axis, and so covered the celestial sphere twice per satellite orbit. Data were telemetered in 1-sec count accumulations. Vela 5B operated until 19 June 1979, although telemetry tracking was poor after mid-1976. The scintillation X-ray detector (XC) aboard Vela 5B consisted of two 1-mm-thick NaI(Tl) crystals mounted on photomultiplier tubes and covered by a 5-mil-thick beryllium window. Electronic thresholds provided two energy channels, 3-12 keV and 6-12 keV. In front of each crystal was a slat collimator providing a FWHM aperture of ~6.1x6.1 degrees. The effective detector area was ~26 sq-cm. Sensitivity to celestial sources was severely limited by the intrinsic detector background of ~36 cts/sec. The Vela 5B X-ray detector yielded ~40 cts/sec for the Crab, so 1 Vela ct/sec ~25 UFU~4.5E-10 ergs/sq-cm/sec in the 3-12 keV response band. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vela5b.html
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vela5b&
tap_tablename = vela5b
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743713
ID = nasa.heasarc/verimaster
publisher_did = ivo://nasa.heasarc/verimaster
obs_collection = VERIMASTER
obs_title = VERITAS Source Catalog
obs_description = The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is a major ground-based gamma-ray observatory operating at the Fred Lawrence Whipple Observatory (FLWO) in southern Arizona, USA. It is an array of four 12m optical telescopes for gamma-ray astronomy in the GeV - TeV energy range. VERITAS is an imaging air Cerenkov system. Gamma-rays from astrophysical sources create particle showers in the Earth's upper atmosphere that produce Cerenkov photons detected on the ground using the large optical telescopes. These telescopes are deployed such that they have the highest sensitivity in the VHE energy band (50 GeV - 50 TeV), with maximum sensitivity from 100 GeV to 10 TeV. The four telescope array is needed for stereoscopic observations that allow the reconstruction of the particle shower geometry, thus giving precise angular and energy resolution. This very high energy observatory, completed in 2007, effectively complements the Fermi Gamma-ray Space Telescope due to its large collection area as well as its higher energy bound and improved angular resolution. VERITAS started four-telescope operations in 2007 and collects about 1100 hours of good-weather data per year. The VERITAS collaboration has published over 100 journal articles since 2008 reporting on gamma-ray observations of a large variety of objects: Galactic sources like supernova remnants, pulsar wind nebulae, and binary systems; extragalactic sources like star forming galaxies, dwarf-spheroidal galaxies, and highly-variable active galactic nuclei. Additional details are available at the <a href="https://veritas.sao.arizona.edu/">VERITAS website</a>. The catalog lists the sources observed by VERITAS as of April 2022, including cross-matches with other gamma-ray observations and spectral fits. This catalog has associated high-level data products containing data from VERITAS publications. This database table was ingested by the HEASARC in December 2022 and is based upon data files provided by the VERITAS Team. A minor correction to one entry in the catalog was made in April 2024. <p> High-level data products were collected from VERITAS publications. Data and fit results were extracted from the published papers or from internal VERITAS analysis results used to produce the published figures and tables. In many cases, spectral and light curve data were obtained by digitizing published figures. This process was led by Gernot Maier at DESY with contributions from many members of the VERITAS collaboration. The primary archive can be accessed on <a href="https://github.com/VERITAS-Observatory/VERITAS-VTSCat">GitHub</a> or downloaded via Zenodo (doi:10.5281/zenodo.6163391). Translation to formats suitable for the HEASARC was led by Philip Kaaret with assistance by Sameer Patel at the University of Iowa and by the HEASARC Team. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/verimaster.html
bib_reference = 2023RNAAS...7....6A
obs_regime = gamma-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=verimaster&
tap_tablename = verimaster
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743725
ID = nasa.heasarc/veroncat
publisher_did = ivo://nasa.heasarc/veroncat
obs_collection = Veron
obs_title = VeronCatalogofQuasars&AGN,13thEdition
obs_description = This database table contains the 13th edition of the Catalog of Quasars and Active Galactic Nuclei by Veron-Cetty and Veron, and is an update of the previous versions. As in the previous editions, no information about absorption lines or X-ray properties is given, but absolute magnitides are provided, assuming a Hubble constant H<sub>0</sub> = 71 km/s/Mpc and a deceleration parameter q<sub>0</sub> = 0 (notice the change of cosmology from previous editions in which H<sub>0</sub> was assumed to be 50 km/s/Mpc). The present edition of this catalog contains 133336 quasars, 1374 BL Lac objects and 34231 active galaxies (including 15627 Seyfert 1 galaxies), for a grand total of 168941 objects, significantly more than the number of objects listed in the 12th edition (108080). The 13th edition includes positions and redshifts, as well as photometry (U, B, and V) and 6-cm and 20-cm flux densities, when available. 178 objects once proposed but now rejected as quasars are NOT included in the online version of this catalog: their names and positions are listed in the file <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/258/reject.dat">https://cdsarc.cds.unistra.fr/ftp/cats/VII/258/reject.dat</a>. This HEASARC table also does NOT contain the additional information on gravitationally lensed quasars and quasar pairs listed in Tables 3 and 4 of the published paper: these tables are available in electronic form at the CDS <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/248/">https://cdsarc.cds.unistra.fr/ftp/cats/VII/248/</a> files table2.dat and table3.dat (sic). The present edition of this catalog contains quasars with measured redshift known prior to July 1st, 2009. This online catalog was created by the HEASARC in April 2010 based on machine-readable tables obtained from the CDS (their catalog VII/258, files qso.dat, bllac.dat, and agn.dat). It was last updated in June 2012 to tweak some class values. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/veroncat.html
bib_reference = 2010A&A...518A..10V
obs_regime = optical
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=veroncat&
tap_tablename = veroncat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743737
ID = nasa.heasarc/vla23901p4
publisher_did = ivo://nasa.heasarc/vla23901p4
obs_collection = VLA23901P4
obs_title = VLA A2390 Cluster of Galaxies 1.4-GHz Source Catalog
obs_description = This table contains the 1.4-GHz source catalog for the field of the cluster of galaxies A2390 as observed with the Very Large Array (VLA). This is one of the deepest radio images of a cluster field ever taken. The image covers an area of 34' x 34' with a synthesized beam of ~1.4" and a noise level of ~5.6 µJy (µJy) near the field center. In the reference paper, the authors construct differential number counts for the central regions (radius < 16') of this cluster, and find that the faint (S<sub>1.4GHz</sub> < 3 mJy) counts of A2390 are roughly consistent with the lowest blank field number counts. Their analyses indicate that the number counts are primarily from field radio galaxies. The authors suggest that the disagreement of their number counts for this cluster with those from a similarly deep observation of A370 that was also presented in the reference paper can be largely attributed to cosmic variance. The authors observed the A2390 cluster field with the VLA in the A configuration for ~31.4hr on-source during 2008 October. The field center is located at 21:53:36 +17:41:52 (J2000). This table was created by the HEASARC in August 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/202/2/">CDS Catalog J/ApJS/202/2/</a> file table2.dat. This file contained 699 entries for sources detected at 1.4 GHz in the A370 field, as well as 524 entries for sources detected at 1.4 GHz in the A2390 field. Only the latter are included in this HEASARC table, while the former can be found in the HEASARC's <a href="vla3701p4.html">VLA3701P4</a> table. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vla23901p4.html
bib_reference = 2012ApJS..202....2W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vla23901p4&
tap_tablename = vla23901p4
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743745
ID = nasa.heasarc/vla3701p4
publisher_did = ivo://nasa.heasarc/vla3701p4
obs_collection = VLA3701P4
obs_title = VLA A370 Cluster of Galaxies 1.4-GHz Source Catalog
obs_description = This table contains the 1.4-GHz source catalog for the field of the cluster of galaxies A370 as observed with the Very Large Array (VLA). This is one of the deepest radio images of a cluster field ever taken. The image covers an area of 40' x 40' with a synthesized beam of ~1.7" and a noise level of ~5.7 µJy (µJy) near the field center. The authors have cataloged 200 redshifts for the A370 field. In the reference paper, they construct differential number counts for the central regions (radius < 16') of this cluster, and find that the faint (S<sub>1.4GHz</sub> < 3 mJy) counts of A370 are roughly consistent with the highest blank field number counts. Their analyses indicate that the number counts are primarily from field radio galaxies. The authors suggest that the disagreement of their number counts for this cluster with those from a similarly deep observation of A2390 that was also presented in the reference paper can be largely attributed to cosmic variance. The authors observed the A370 cluster field with the VLA in the A configuration for ~42.4hr on-source during 1999 August and September. K. S. Dwarakanath observed A370 in the B configuration for ~18.4hr on-source during 1994 August and September. The field center is located at 02:39:32 -01:35:07 (J2000). This is offset by approximately 5 arcminutes from the cluster center at 02:39:50.5 -01:35:08. The authors also targeted 58 radio sources, in A370, that had no existing optical spectral data using the Hydra fiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) telescope (spectral window of ~4500 - 9500 Angstrom). They preferentially targeted optically bright galaxies, obtaining these data in a single two-hour pointing on 2012 January 20. Of the 58 targets, the authors obtained high-confidence redshifts for 36. This table was created by the HEASARC in August 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/202/2/">CDS Catalog J/ApJS/202/2/</a> file table2.dat. This file contained 699 entries for sources detected at 1.4 GHz in the A370 field, as well as 524 entries for sources detected at 1.4 GHz in the A2390 field. Only the former are included in this HEASARC table, while the latter can be found in the HEASARC's <a href="vla23901p4.html">VLA23901P4</a> table. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vla3701p4.html
bib_reference = 2012ApJS..202....2W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vla3701p4&
tap_tablename = vla3701p4
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743757
ID = nasa.heasarc/vla74mhzdp
publisher_did = ivo://nasa.heasarc/vla74mhzdp
obs_collection = VLA74MHZDP
obs_title = VLA 74-MHz Deep High-Resolution Survey Source Catalog
obs_description = This table contains some of the results from a 74-MHz survey of a 165 deg<sup>2</sup> region located near the North Galactic Pole (NGP). This survey has an unprecedented combination of both spatial resolution (25" FWHM) and sensitivity (1-sigma as low as 24mJy/beam). The authors detect 949 sources at the 5-sigma level in this region, enough to begin exploring the nature of the 74-MHz source population. In their paper, they present differential source counts, spectral index measurements, and the size distribution as determined from counterparts in the high-resolution FIRST 1.4-GHz survey. They find a trend of steeper spectral indices for the brighter sources. Further, there is a clear correlation between spectral index and median source size, with the flat-spectrum sources being much smaller on average. Ultra-steep spectrum objects (power-law index alpha <= -1.2, where S_nu ~ nu<sup>alpha</sup>) are identified. These sources are excellent candidates for high-redshift radio galaxies. The data used to produce this survey come from observations taken on 1998 March 7 intended to map two normal galaxies at 74 MHz (NGC 4565 and NGC 4631). These two pointings were separated by 6.4 degrees, roughly the radius of the primary beam at 74 MHz, allowing them to be ideally combined to produce a single deep image roughly 17 x 10 degrees in size. The combination of VLA A-configuration resolution (25 arcsec), favorable ionospheric conditions, and pointings in directions near the NGP, where the background temperature is low, produced the deepest observation ever obtained below 100 MHz. The same algorithm that was used in the 1.4-GHz NVSS was used to identify and characterize sources in this 74-MHz survey. The source detection algorithm had a threshold such that sources must have both a peak and integrated flux density level of at least 5 times the local rms noise level. Since the rms noise level varied from 24 mJy/beam to 80 mJy mJy/beam at the chosen field edge, the absolute level of the source-detection threshold of 5-sigma likewise varied over the image. This table was created by the HEASARC in August 2010 based on CDS catalog J/ApJS/150/417/ file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vla74mhzdp.html
bib_reference = 2004ApJS..150..417C
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vla74mhzdp&
tap_tablename = vla74mhzdp
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743765
ID = nasa.heasarc/vlacdfscat
publisher_did = ivo://nasa.heasarc/vlacdfscat
obs_collection = VLACDFSCAT
obs_title = VLA Survey of Chandra Deep Field South
obs_description = This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and sub-millimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microJansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table. This table was created by the HEASARC in November 2008 based on the electronic version of Table 1 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlacdfscat.html
bib_reference = 2008ApJS..179...71K
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlacdfscat&
tap_tablename = vlacdfscat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743777
ID = nasa.heasarc/vlacomacat
publisher_did = ivo://nasa.heasarc/vlacomacat
obs_collection = VLACOMACAT
obs_title = VLA Coma Cluster of Galaxies 1.4-GHz Source Catalog
obs_description = This table contains results from deep 1.4-GHz Very Large Array (VLA) radio continuum observations of two ~0.5 deg<sup>2</sup> fields in the Coma cluster of galaxies. The two fields, "Coma 1" and "Coma 3", correspond to the cluster core and the southwest infall region, and were selected on account of abundant pre-existing multiwavelength data. In their most sensitive regions, the radio data reach 0.022 mJy (22 microJy) rms per 4.4" beam, sufficient to detect (at 5-sigma) Coma member galaxies with L<sub>1.4GHz</sub> = 1.3 x 10<sup>20</sup> W Hz<sup>-1</sup> (1.3 x 10<sup>27</sup> erg s<sup>-1</sup> Hz<sup>-1</sup>). The full catalog of radio detections at and above a 4.5-sigma significance threshold is presented herein; there are 1030 of these sources which are detected at >= 5 sigma, 628 of which are within the combined Coma 1 and Coma 3 area. The authors also provide optical identifications of the radio sources using data from the Sloan Digital Sky Survey (SDSS). The depth of the radio observations allows them to detect active galactic nuclei in cluster elliptical galaxies with M<sub>r</sub> < -20.5 (AB magnitudes), including radio detections for all cluster ellipticals with M<sub>r</sub> < -21.8. At fainter optical magnitudes (-20.5 < M<sub>r</sub> <~ -19), the radio sources are associated with star-forming galaxies with star formation rates as low as 0.1M_{sun}_ yr<sup>-1</sup>. The VLA observations were performed over five days in 2006 June as program code AM868. On each of the five days, the scheduled time was centered on the transit of Coma. This table was created by the HEASARC in December 2011 based on CDS catalog J/AJ/137/4436 files table2.dat ('The Radio Source Catalog') and table3.dat ('Optical Counterparts to the Radio Sources'). It does not include table4.dat ('Rejected Optical Counterparts to the Radio Sources'). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlacomacat.html
bib_reference = 2009AJ....137.4436M
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlacomacat&
tap_tablename = vlacomacat
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ID = nasa.heasarc/vlacos324m
publisher_did = ivo://nasa.heasarc/vlacos324m
obs_collection = VLACOS324M
obs_title = VLA-COSMOS Survey 324-MHz Continuum Source Catalog
obs_description = This table contains a source catalog based on 90-cm (324-MHz) Very Large Array (VLA) imaging of the COSMOS field, comprising a circular area of 3.14 square degrees centered on 10<sup>h</sup> 00<sup>m</sup> 28.6<sup>s</sup>, _02<sup>o</sup> 12' 21" (J2000.0 RA and Dec). The image from the merger of 3 nights of observations using all 27 VLA antennas had an effective total integration time of ~ 12 hours, an 8.0 arcsecond x 6.0 arcsecond angular resolution, and an average rms of 0.5 mJy beam<sup>-1</sup>. The extracted catalog contains 182 sources (down to 5.5 sigma), 30 of which are multi-component sources. Using Monte Carlo artificial source simulations, the authors derive the completeness of the catalog, and show that their 90-cm source counts agree very well with those from previous studies. In their paper, the authors use X-ray, NUV-NIR and radio COSMOS data to investigate the population mix of this 90-cm radio sample, and find that the sample is dominated by active galactic nuclei. The average 90-20 cm spectral index (S_nu_~ nu<sup>alpha</sup>, where S<sub>nu</sub> is the flux density at frequency nu and alpha the spectral index) of the 90-cm selected sources is -0.70, with an interquartile range from -0.90 to -0.53. Only a few ultra-steep-spectrum sources are present in this sample, consistent with results in the literature for similar fields. These data do not show clear steepening of the spectral index with redshift. Nevertheless, this sample suggests that sources with spectral indices steeper than -1 all lie at z >~ 1, in agreement with the idea that ultra-steep-spectrum radio sources may trace intermediate-redshift galaxies (z >~ 1). Using both the signal and rms maps (see Figs. 1 and 2 in the reference paper) as input data, the authors ran the AIPS task SAD to obtain a catalog of candidate components above a given local signal-to-noise ratio (S/N) threshold. The task SAD was run four times with search S/N levels of 10, 8, 6 and 5, using the resulting residual image each time. They recovered all the radio components with a local S/N > 5.00. Subsequently, all the selected components were visually inspected, in order to check their reliability, especially for the components near strong side-lobes. After a careful analysis, a S/N threshold of 5.50 was adopted as the best compromise between a deep and a reliable catalog. The procedure yielded a total of 246 components with a local S/N > 5.50. More than one component, identified in the 90-cm map sometimes belongs to a single radio source (e.g. large radio galaxies consist of multiple components). Using the 90-cm COSMOS radio map, the authors combined the various components into single sources based on visual inspection. The final catalog (contained in this HEASARC table) lists 182 radio sources, 30 of which have been classified as multiple, i.e. they are better described by more than a single component. Moreover, in order to ensure a more precise classification, all sources identified as multi-component sources have been also double-checked using the 20-cm radio map. The authors found that all the 26 multiple 90-cm radio sources within the 20-cm map have 20-cm counterpart sources already classified as multiple. The authors have made use of the VLA-COSMOS Large and Deep Projects over 2 square degrees, reaching down to an rms of ~15 microJy beam<sup>1</sup> ^ at 1.4 GHz and 1.5 arcsec resolution (Schinnerer et al. 2007, ApJS, 172, 46: the VLACOSMOS table in the HEASARC database). The 90-cm COSMOS radio catalog has, however, been extracted from a larger region of 3.14 square degrees (see Fig. 1 and Section 3.1 of the reference paper). This implies that a certain number of 90-cm sources (48) lie outside the area of the 20-cm COSMOS map used to select the radio catalog. Thus, to identify the 20-cm counterparts of the 90-cm radio sources, the authors used the joint VLA-COSMOS catalog (Schinnerer et al. 2010, ApJS, 188, 384: the VLACOSMJSC table in the HEASARC database) for the 134 sources within the 20-cm VLA-COSMOS area and the VLA- FIRST survey (White et al. 1997, ApJ, 475, 479: the FIRST table in the HEASARC database) for the remaining 48 sources. The 90-cm sources were cross-matched with the 20-cm VLA-COSMOS sources using a search radius of 2.5 arcseconds, while the cross-match with the VLA-FIRST sources has been done using a search radius of 4 arcseconds in order to take into account the larger synthesized beam of the VLA-FIRST survey of ~5 arcseconds. Finally, all the 90 cm - 20 cm associations were visually inspected in order to ensure also the association of the multiple 90-cm radio sources for which the value of the search radius used during the cross-match could be too restrictive. In summary, out of the total of 182 sources in the 90-cm catalog, 168 have counterparts at 20 cm. This table was created by the HEASARC in October 2014 based on an electronic version of Table 1 from the reference paper which was obtained from the COSMOS web site at IRSA, specifically the file vla-cosmos_327_sources_published_version.tbl at <a href="http://irsa.ipac.caltech.edu/data/COSMOS/tables/vla/">http://irsa.ipac.caltech.edu/data/COSMOS/tables/vla/</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlacos324m.html
bib_reference = 2014MNRAS.443.2590S
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlacos324m&
tap_tablename = vlacos324m
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ID = nasa.heasarc/vlacos3ghz
publisher_did = ivo://nasa.heasarc/vlacos3ghz
obs_collection = VLACOS3GHZ
obs_title = VLA-COSMOS 3-GHz Large Project Source Catalog
obs_description = This table contains some of the results from the VLA-COSMOS 3-GHz Large Project based on 384 hours of observations with the Karl G. Jansky Very Large Array (VLA) at 3 GHz (10 cm) toward the 2 square degree Cosmic Evolution Survey (COSMOS) field. The final mosaic reaches a median rms of 2.3 µJy (µJy) beam<sup>-1</sup> over the 2 square degrees at an angular resolution of 0.75 arcseconds. To fully account for the spectral shape and resolution variations across the broad (2-GHz) band, the authors imaged all the data with a multiscale, multifrequency synthesis algorithm. In this table, the catalog of 10,830 radio sources down to 5 sigma is presented, out of which 67 are combined from multiple components. Comparing the positions of these 3-GHz sources with those from the Very Long Baseline Array (VLBA)-COSMOS survey, the authors estimate that the astrometry is accurate to 0.01 arcseconds at the bright end (signal-to-noise ratio, S/N<sub>3GHz</sub> > 20). Survival analysis on these data combined with the VLA-COSMOS 1.4-GHz Joint Project catalog yields an expected median radio spectral index alpha = -0.7. The authors compute completeness corrections via Monte Carlo simulations to derive the corrected 3-GHz source counts. Their counts are in agreement with previously derived 3-GHz counts based on single-pointing (0.087 square degrees) VLA data. In summary, the VLA-COSMOS 3-GHz Large Project simultaneously provides the largest and deepest radio continuum survey at high (0.75") angular resolution to date, bridging the gap between last-generation and next-generation surveys. The catalog contains sources selected down to a 5-sigma (where sigma ~2.3 µJy/beam) threshold. This catalog can be used for statistical analyses, accompanied with the corrections given in the data & catalog release paper. All completeness and bias corrections and source counts presented in the paper were calculated using this sample. The total fraction of spurious sources in the COSMOS 2 sq.deg. field is below 2.7% within this catalog. However, an increase of spurious sources up to 24% at 5.0 < S/N < 5.5 is present (for details see Sec. 5.2., Fig. 17 and Table 3 of the reference paper). A subsample with a minimal spurious source fraction can be selected by requiring an additional cutoff S/N >= 5.5 for single component sources (MULTI=0). The total fraction of spurious sources in the COSMOS 2 sq.deg. field within such a selected sample is below 0.4%, and the fraction of spurious sources is below 3% even at the lowest S/N of 5.5. This table was created by the HEASARC in June 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/602/A1">CDS Catalog J/A+A/602/A1</a> file table1.dat, the VLA-COSMOS 3-GHz radio source catalog. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlacos3ghz.html
bib_reference = 2017A&A...602A...1S
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlacos3ghz&
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TIMESTAMP = 1714845743813
ID = nasa.heasarc/vlacosmjsc
publisher_did = ivo://nasa.heasarc/vlacosmjsc
obs_collection = VLACOSMJSC
obs_title = VLA-COSMOS Project 1.4-GHz Joint Source Catalog
obs_description = In the context of the VLA-COSMOS Deep project, additional VLA A array observations at 1.4 GHz were obtained for the central degree of the COSMOS field and combined with the existing data from the VLA-COSMOS Large project. A newly constructed Deep mosaic with a resolution of 2.5 arcseconds was used to search for sources down to 4 sigma with 1 sigma ~ 12 microJy beam^-1 in the central 50' x 50'. This new catalog is combined with the catalog from the Large project (obtained at 1.5" x 1.4" resolution) to construct a new Joint catalog. All sources listed in the new Joint catalog have peak flux densities of >= 5 sigma at 1.5" and/or 2.5" resolution to account for the fact that a significant fraction of sources at these low flux levels are expected to be slightly resolved at 1.5" resolution. All properties listed in the Joint catalog, such as peak flux density, integrated flux density, and source size, are determined in the 2.5" resolution Deep image. In addition, the Joint catalog contains 43 newly identified multi-component sources. This table was created by the HEASARC in June 2010 based on the electronic version of Table 3 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlacosmjsc.html
bib_reference = 2010ApJS..188..384S
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlacosmjsc&
tap_tablename = vlacosmjsc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743821
ID = nasa.heasarc/vlacosmos
publisher_did = ivo://nasa.heasarc/vlacosmos
obs_collection = VLACOSMOS
obs_title = VLA-COSMOS Large Project 1.4-GHz Source Catalog
obs_description = The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N >= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and < 55 mas, respectively. This table was created by the HEASARC in September 2007 based on the electronic version of Table 3 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlacosmos.html
bib_reference = 2007ApJS..172...46S
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlacosmos&
tap_tablename = vlacosmos
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743833
ID = nasa.heasarc/vlacosxoid
publisher_did = ivo://nasa.heasarc/vlacosxoid
obs_collection = VLACOSXOID
obs_title = VLA-COSMOS 3-GHz Large Project Multiwavelength Counterparts Catalog
obs_description = In the reference paper, the authors study the composition of the faint radio population selected from the VLA-COSMOS 3-GHz Large Project, a radio continuum survey performed at 10-cm wavelength. The survey covers a 2.6 square degree area with a mean rms of ~2.3 µJy/beam (µJy/beam), cataloguing 10,830 sources above 5 sigma, and enclosing the full 2 square degree COSMOS field. By combining these radio data with optical, near-infrared (UltraVISTA), and mid-infrared (Spitzer/IRAC) data, as well as X-ray data (Chandra), the authors find counterparts to radio sources for ~93% of the total radio sample in the unmasked areas of the COSMOS field, i.e., those not affected by saturated or bright sources in the optical to near-IR (NIR) bands, reaching out to z ~ 6. They further classify the sources as star-forming galaxies or AGN based on various criteria, such as X-ray luminosity, observed mid-infrare (MIR) color, UV-far-infrared (FIR) spectral-energy distribution (SED), rest-frame near-ultraviolet (NUV)-optical color corrected for dust extinction, and radio-excess relative to that expected from the the hosts' star-formation rate. The authors separate the AGN into sub-samples dominated by low-to-moderate and moderate-to-high radiative luminosity AGN, i.e., candidates for high-redshift analogs to local low- and high-excitation emission line AGN, respectively. They study the fractional contributions of these sub-populations down to radio flux levels of ~11 uJy at 3 GHz (or ~20 uJy at 1.4 GHz assuming a spectral index of -0.7), and find that the dominant fraction at 1.4 GHz flux densities above ~200 uJy is constituted of low-to-moderate radiative luminosity AGN MLAGN). Below densities of ~100 uJy the fraction of star-forming galaxies (SFG) increases to ~60%, followed by the moderate-to-high radiative luminosity AGN (HLAGN) with ~20%, and MLAGN with ~20%. Based on this observational evidence, the authors extrapolate the fractions down to sensitivities of the Square Kilometer Array (SKA). Their estimates suggest that at the faint flux limits to be reached by the (Wide, Deep, and UltraDeep) SKA1 surveys, a selection based only on radio flux limits can provide a simple tool to efficiently identify samples highly (>75%) dominated by star-forming galaxies. This table contains the full list of 9,161 optical-MIR counterparts collected over the largest unmasked area accessible to each catalog, being 1.77, 1.73, and 2.35 square degrees for COSMOS2015, i-band, and IRAC catalogs, respectively. The catalog lists the counterpart IDs, properties, as well as the individual criteria used in this work to classify these radio sources. The authors note that complete, non-overlapping samples within a well defined, effective area of 1.77 square degrees (COSMOS2015 masked area flag_C15 = 0, can be formed by combining (i) HLAGN, MLAGN, and clean SFG samples, or, alternatively, (ii) the radio-excess and no-radio-excess samples. This table was created by the HEASARC in July 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/602/A2">CDS Catalog J/A+A/602/A2</a> file table1.dat, the VLA-COSMOS 3-GHz Large Project multiwavelength counterpart catalog. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlacosxoid.html
bib_reference = 2017A&A...602A...2S
obs_regime = infrared
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlacosxoid&
tap_tablename = vlacosxoid
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
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TIMESTAMP = 1714845743841
ID = nasa.heasarc/vlaecdfs1p4
publisher_did = ivo://nasa.heasarc/vlaecdfs1p4
obs_collection = VLAECDFS1P4
obs_title = VLA Extended-Chandra Deep Field-South 1.4-GHz Source Catalog
obs_description = Deep radio observations at 1.4 GHz for the Extended Chandra Deep Field South were performed in 2007 June through September and presented in a first data release (Miller et al. 2008, ApJS, 179, 114). The survey was made using six separate pointings of the Very Large Array with over 40 hr of observation per pointing. In the current study, the authors improve on the data reduction to produce a second data release (DR2) mosaic image. This DR2 image covers an area of about a third of a square degree, reaches a best rms sensitivity of 6 microJy (uJy), and has a typical sensitivity of 7.4 uJy per 2.8" by 1.6" beam. The authors also present a more comprehensive catalog, including sources down to peak flux densities of five or more times the local rms noise, along with information on source sizes and relevant pointing data. In their paper, they discuss in some detail the consideration of whether sources are resolved under the complication of a radio image created as a mosaic of separate pointings, each suffering some degree of bandwidth smearing, and the accurate evaluation of the flux densities of such sources. Finally, the radio morphologies and optical/near-IR counterpart identifications are used to identify 17 likely multiple-component sources so as to arrive at a catalog of 883 radio sources (and also 49 individual components of the 17 multi-component sources), which is roughly double the number of sources contained in the first data release. In order to cover the full E-CDF-S area at near-uniform sensitivity, the authors pointed the VLA at six separate coordinate locations arranged in a hexagonal grid around the adopted center of the CDF-S, viz. RA, Dec (J2000) 03<sup>h</sup> 32<sup>m</sup> 28.00<sup>s</sup>, -27<sup>o</sup> 48' 30.0". The observations were spread over many days on account of the low declination of the field and typically amounted to 5 hr of time per calendar date. The details of the individual pointings are: <pre> Pointing ID R.A. (J2000) DE. (J2000) rms sensitivity for final image ECDFS 1 03:33:22.25 -27:48:30.0 10.5 uJy ECDFS 2 03:32:55.12 -27:38:03.0 9.4 uJy ECDFS 3 03:32:00.88 -27:38:03.0 9.7 uJy ECDFS 4 03:31:33.75 -27:48:30.0 9.5 uJy ECDFS 5 03:32:00.88 -27:58:57.0 10.0 uJy ECDFS 6 03:32:55.12 -27:58:57.0 9.3 uJy </pre> The images corresponding to the six individual pointings were combined to form the final mosaic image (shown in Figure 1 of the reference paper). This HEASARC table contains the catalog of 883 radio sources (Table 3 in the reference paper) and also the catalog of 49 individual components of the 17 multi-component sources (Table 4 in the reference paper), so that there are a total of 932 entries in the present table. To allow users to easily distinguish these types of entry, the HEASARC created a parameter type_flag which is set to 'S' for the 883 source entries and to 'C' for the 49 component entries. The HEASARC created names for the sources following the standard CDS and IAU recommendations for position-based names and using the prefix of '[MBF2013]' for Miller, Bonzini, Fomalont (2013), the first 3 authors and the date of publication of the reference paper. For the components, we have used the names based on the positions of the parent sources and the suffixes 'A', 'B', etc, in order of increasing J2000.0 RA. Thus, for the multi-component source [MBF2013] J033115.0-275518 which has 3 components, there are 4 entries in this table, one for the entire source, and one for each component, e.g.: <pre> Name | type_flag | RA (J2000.0) Dec (J2000.0) [MBF2013] J033115.0-275518 | S | 03 31 15.04 | -27 55 18.8 [MBF2013] J033115.0-275518 A| C | 03 31 13.99 | -27 55 19.9 [MBF2013] J033115.0-275518 B| C | 03 31 15.06 | -27 55 18.9 [MBF2013] J033115.0-275518 C| C | 03 31 17.05 | -27 55 15.2 </pre> The 17 sources thought to consist of multiple components associated with a single host object are each listed with a single aggregate integrated flux density. Gaussian fits to the individual components associated with these sources are separately listed for their components This table was created by the HEASARC in May 2013 based on CDS Catalog J/ApJS/205/13 files table3.dat and table4.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlaecdfs1p4.html
bib_reference = 2013ApJS..205...13M
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlaecdfs1p4&
tap_tablename = vlaecdfs1p4
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ID = nasa.heasarc/vlaecdfscls
publisher_did = ivo://nasa.heasarc/vlaecdfscls
obs_collection = VLAECDFSCLS
obs_title = VLA Extended-Chandra Deep Field-South Classification Catalog
obs_description = The sub-mJy radio population is a mixture of active systems, that is star-forming galaxies (SFGs) and active galactic nuclei (AGNs). In their paper, the authors study a sample of 883 radio sources detected at 1.4 GHz in a deep Very Large Array (VLA) survey of the Extended Chandra Deep Field-South (E-CDF-S) that reaches a best rms sensitivity of 6 microJansky (uJy). The authors have used a simple scheme to disentangle SFGs, radio-quiet (RQ), and radio-loud (RL) AGNs based on the combination of radio data with Chandra X-ray data and mid-infrared observations from Spitzer. They find that at flux densities between about 30 and 100 uJy, the radio population is dominated by SFGs (~60%) and that RQ AGNs become increasingly important over RL ones below 100 uJy. In the paper, the authors also compare the host galaxy properties of the three classes in terms of morphology, optical colors and stellar masses. Their results show that both SFG and RQ AGN host galaxies have blue colors and late-type morphology while RL AGNs tend to be hosted by massive red galaxies with early-type morphology. This supports the hypothesis that radio emission in SFGs and RQ AGNs mainly comes from the same physical process: star formation in the host galaxy. This table was created by the HEASARC in January 2014 based on the machine-readable version of Table 1 from the reference paper which was obtained from the MNRAS web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlaecdfscls.html
bib_reference = 2013MNRAS.436.3759B
obs_regime = infrared
obs_regime = radio
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlaecdfscls&
tap_tablename = vlaecdfscls
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743861
ID = nasa.heasarc/vlaecdfsoi
publisher_did = ivo://nasa.heasarc/vlaecdfsoi
obs_collection = VLAECDFSOI
obs_title = VLA Extended-Chandra Deep Field-South 1.4-GHz Sources Opt/IR Counterparts
obs_description = This table contains a sample of 883 sources detected in a deep Very Large Array (VLA) survey at 1.4 GHz in the Extended-Chandra Deep Field South (E-CDFS). The reference paper focuses on the identification of their optical and infrared (IR) counterparts. The authors use a likelihood-ratio technique that is particularly useful when dealing with deep optical images to minimize the number of spurious associations. They find a reliable counterpart for 95% of their radio sources. Most of the counterparts (74%) are detected at optical wavelengths, but there is a significant fraction (21%) that are only detectable in the IR. Combining newly acquired optical spectra with data from the literature, the authors are able to assign a redshift to 81% of the identified radio sources (37% spectroscopic). They also investigate the X-ray properties of the radio sources using the Chandra 4 Ms and 250 ks observations. In particular, the authors use a stacking technique to derive the average properties of radio objects undetected in the Chandra images. The results of their analysis are collected in this new catalog containing the position of the optical/IR counterpart, the redshift information, and the X-ray fluxes. It is the deepest multi-wavelength catalog of radio sources, which will be used for future study of this galaxy population. The E-CDFS was observed at 1.4 GHz with the VLA between 2007 June and September (Miller et al. 2008, ApJS, 179, 114). The mosaic image covered an area of about 34 by 34 arcminutes with near-uniform sensitivity. The typical rms is 7.4 microJy for a 2.8 by 1.6 arcseconds beam. The second data release (N. Miller et al. 2012, in preparation) provides a new source catalog with a 5-sigma point-source detection limit, for a total of 883 sources. The median value of the distribution is 58.5 microJy and the median signal-to-noise ratio (S/N) is 7.6. The authors note that ~ 90% of the sample has a flux density below 1 mJy, a regime where radio-quiet AGNs and star-forming galaxies (SFGs) become the dominant populations This table was created by the HEASARC in November 2012 based on the files table3.dat and table5.dat which were obtained from the ApJS web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlaecdfsoi.html
bib_reference = 2012ApJS..203...15B
obs_regime = infrared
obs_regime = optical
obs_regime = radio
obs_regime = x-ray
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TIMESTAMP = 1714845743873
ID = nasa.heasarc/vlaen20cm
publisher_did = ivo://nasa.heasarc/vlaen20cm
obs_collection = VLAEN20CM
obs_title = VLA ELAIS N1, N2, N3 Fields 20-cm Source Catalog
obs_description = The authors have used the Very Large Array (VLA) in C configuration to carry out a sensitive 20-cm radio survey of regions of the sky that have been surveyed in the far-infrared (FIR) over the wavelength range 5 -200 microns (um) with ISO (Infrared Space Observatory) as part of the European Large-Area ISO Survey (ELAIS). As usual in surveys based on a relatively small number of overlapping VLA pointings, the flux limit varies over the area surveyed: from a 5-sigma limit of 0.135 mJy over an area of 0.12 deg<sup>2</sup> to 1.15 mJy or better over the whole region covered of 4.22 deg<sup>2</sup>. In their paper, the authors present the complete radio catalog of 867 sources, 428 of which form a complete sample in the flux range 0.2 - 1.0 mJy. These regions of the sky have previously been surveyed to shallower flux limits at 20 cm with the VLA as part of the VLA D-configuration NVSS (full width at half-maximum, FWHM = 45arcseconds) and VLA-B configuration FIRST (FWHM = 5 arcseconds) surveys. This whole survey has a nominal 5-sigma flux limit a factor of 2 below that of the NVSS; 3.4 deg<sup>2</sup> of the survey reaches the nominal flux limit of the FIRST survey and 1.5 deg<sup>2</sup> reaches 0.25 mJy, a factor of 4 below the nominal FIRST survey limit. In addition, this survey is at a resolution intermediate between the two surveys and thus is well suited for a comparison of the reliability and resolution-dependent surface brightness effects that affect interferometric radio surveys. The authors have carried out a detailed comparison of their survey and these two independent surveys in order to assess the reliability and completeness of each. Considering the whole sample, they found that to the 5-sigma nominal limits of 2.3 and 1.0 mJy, respectively, the NVSS and FIRST surveys have a completeness of 96<sup>+2</sup><sub>-3</sub> and 89<sup>+2</sup><sub>-3</sub> % and a reliability of 99<sup>+1</sup><sub>-2</sub> and 94<sup>+2</sup><sub>-2</sub> %. The radio observations were obtained of three ISO ELAIS survey regions in the Northern celestial hemisphere (N1 1610+5430, N2 1636+4115 and N3 1429+3306) (see Table 1 of the reference paper for the details of the fields and the individual pointings). The observations are made with the Very Large Array (VLA) radio telescope at 1.4 GHz (20 cm) in the VLA C configuration (maximum baseline 3.4 km) with an angular resolution (FWHM) of ~15 arcseconds. The aim of these VLA observations was to obtain uniform coverage of the ELAIS regions with an rms noise limit of ~50 microJansky (uJy). This table contains the 921 components of 867 total sources detected at a level of >= 5 sigma (44 of which are multiple component sources as defined in Section 4.3 of the reference paper) over a total area of 4.222 deg<sup>2</sup>. There are also entries describing the properties of the total sources for the 44 multi-component sources (for which the positions have been computed as the flux-weighted average positions of their components), and thus this catalog contains 965 (921 + 44) entries. To filter out the latter, component_id values != 'T' should be selected when searching this table. This table was originally ingested by the HEASARC in August 2012, based on CDS Catalog J/MNRAS/302/222 file table3.dat. It was last updated in September 2013 to remove a duplicate entry for the source ELAISR J142743+331323. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlaen20cm.html
bib_reference = 1999MNRAS.302..222C
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlaen20cm&
tap_tablename = vlaen20cm
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TIMESTAMP = 1714845743881
ID = nasa.heasarc/vlagbsoph
publisher_did = ivo://nasa.heasarc/vlagbsoph
obs_collection = VLAGBSOPH
obs_title = VLA Goulds Belt Survey Ophiuchus Complex Source Catalog
obs_description = This table contains results from large-scale (~2000 arcmin<sup>2</sup>), deep (~20 microJy), high-resolution (~1") radio observations of the Ophiuchus star-forming complex obtained with the Karl G. Jansky Very Large Array (JVLA) at wavelengths of 4 and 6 cm (frequencies of 7.5 and 4.5 GHz). In total, 189 sources were detected, 56 of them associated with known young stellar objects (YSOs), and 4 with known extragalactic objects; the other 129 remain unclassified, but most of them are most probably background quasars. The vast majority of the young stars detected at radio wavelengths have spectral types K or M, although four objects of A/F/B types and two brown dwarf candidates are also detected. At least half of these young stars are non-thermal (gyrosynchrotron) sources, with active coronae characterized by high levels of variability, negative spectral indices, and (in some cases) significant circular polarization. As expected, there is a clear tendency for the fraction of non-thermal sources to increase from the younger (Class 0/I or flat spectrum) to the more evolved (Class III or weak-line T Tauri) stars. The young stars detected both in X-rays and at radio wavelengths broadly follow a Gudel-Benz relation, but with a different normalization than the most radio-active types of stars. Finally, the authors detected a ~70 mJy compact extragalactic source near the center of the Ophiuchus core, which should be used as gain calibrator for any future radio observations of this region. The observations were obtained with the JVLA of the National Radio Astronomy Observatory (NRAO). Two frequency sub-bands, each 1-GHz wide, and centered at 4.5 and 7.5 GHz, respectively, were recorded simultaneously. The observations were obtained on three different epochs (2011 February 17/19, April 3/4, and May 4/6) typically separated from one another by a month. The angular resolution of the observations is of the order of 1 arcsecond. To identify sources in their observations, the authors used the images corresponding to the concatenation of the three epochs, which provided the highest sensitivity. The criteria used to consider a detection as firm were: (1) sources with reported counterparts and a flux larger than four times the rms noise of the area, or (2) sources with a flux larger than five times the rms noise of the area and without reported counterparts. The authors searched the literature for previous radio detections, and for counterparts at X-ray, optical, near-infrared, and mid-infrared wavelengths. The search was done in SIMBAD, and accessed all the major catalogs (listed explicitly in the footnote of Table 3 in the reference paper). Note that the Spitzer c2d catalog includes cross-references to other major catalogs which were taken into account in their counterpart search. The authors considered a radio source associated with a counterpart at another wavelengths if the separation between the two was below the combined uncertainties of the two data sets. This was about 1.5 arcseconds for the optical and infrared catalogs, but could be significantly larger for some of the radio catalogs (for instance, the NVSS has a positional uncertainty of about 5 arcseconds). The authors found that only 76 of the sources detected here had previously been reported at radio wavelengths (matches are listed in the radio_name parameter in such cases), while the other 113 are new radio detections. On the other hand, they found a total of 100 counterparts at other wavelengths. Note that there are a significant number of sources that were previously known at radio wavelengths and have known counterparts at other frequencies. As a consequence, the number of sources that were previously known (at any frequency) is 134, while 55 of the sources in this sample are reported here for the first time. The authors argue that most of these 55 objects are likely background sources. They note, however, that 18 of the 129 unclassified objects (55 identified here for the first time and 74 previously known at radio wavelengths) are compact, have a positive spectral index, or exhibit high variability. Since these latter two properties are not expected of quasars (which are certainly variable, but usually not strongly on such short timescale), but would be natural characteristics of young stars, the authors argue that a small population of YSOs might be present among the unclassified sources. This population could account for, at most, 15% of the unclassified sources, and possibly significantly less. This table was created by the HEASARC in July 2015 based on electronic versions of Tables 1, 3 and 5 from the reference paper, which were obtained from the CDS (Catalog J/ApJ/775/63 files table1.dat, table3.dat and table5.dat). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlagbsoph.html
bib_reference = 2013ApJ...775...63D
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlagbsoph&
tap_tablename = vlagbsoph
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TIMESTAMP = 1714845743893
ID = nasa.heasarc/vlagbsori
publisher_did = ivo://nasa.heasarc/vlagbsori
obs_collection = VLAGBSORI
obs_title = VLA Goulds Belt Survey Orion Complex Source Catalog
obs_description = This table contains results from a high-sensitivity (60 microJy), large-scale (2.26 deg<sup>2</sup>) survey obtained with the Karl G. Jansky Very Large Array (JVLA) as part of the Gould's Belt Survey (GBS) program. The authors detected 374 and 354 sources at 4.5 and 7.5 GHz, respectively. Of these, 148 are associated with previously known young stellar objects (YSOs). Another 86 sources previously unclassified at either optical or infrared wavelengths exhibit radio properties that are consistent with those of young stars. The overall properties of these sources at radio wavelengths such as their variability and radio to X-ray luminosity relation are consistent with previous results from the GBS. These detections provide target lists for follow-up Very Long Baseline Array radio observations to determine their distances, as YSOs are located in regions of high nebulosity and extinction, making it difficult to measure their optical parallaxes. The observations were obtained with the JVLA of the National Radio Astronomy Observatory (NRAO) in its A configuration. The observations of the 210 fields in the Orion Molecular Clouds A and B were obtained in three different epochs (2011 June 25 to July 4, July 23 to 30, and August 25 to 29, as described in Table 1 of the reference paper) typically separated from one another by a month. The 210 individual fields have been split into 7 maps, with 30 fields being observed per map, as follows: 12 in the lambda Ori region, 3 in L1622, 27 are shared between NGC 2068 and NGC 2071, 14 are shared between NGC 2023 and NGC 2024, 11 in the sigma Ori region, 109 in the Orion Nebula Cluster (ONC), 16 in L1641-N, 8 in L1641-C, and 10 in L1641-S (see Figures 1 to 7 in the reference paper). Two frequency sub-bands, each 1-GHz wide, and centered at 4.5 and 7.5 GHz, respectively, were recorded simultaneously. The authors achieved a nearly uniform rms noise of 60 microJy beam<sup>-1</sup> at both frequencies in all the regions. The only exception to this is in the Trapezium region due to nebular emission; there the noise was 200 microJy beam<sup>-1</sup> after excluding baselines smaller than 150 kilo-lambda during imaging to remove extended emission. Sources were identified through a visual inspection of the individual fields at 4.5 GHz during the cleaning and imaging process since an automated source identification was deemed to be not sufficiently advanced and produced results that were too unreliable. In particularly clustered regions such as the Trapezium and NGC 2024, in addition to standard imaging, data from all three epochs were combined into a single image for source identification purposes only to improve statistical significance of each detection. The authors detected a combined total of 374 sources among the three epochs for all of the regions. All sources but one had fluxes greater than five times the rms noise in at least one epoch. The remaining source, 'GBS-VLA J053518.67-052033.1', was detected at two epochs with maximum detection probability of 4.9 sigma in a single epoch data. It is found in the Trapezium region, and has known counterparts in other wavelength regimes. The authors cross-referenced their catalog of sources with previous major radio, infrared, optical and X-ray surveys of the regions published in the literature. They have generally considered sources in these surveys to be counterparts if they had positional coincidences less than 1 arcsecond, but have allowed for larger offsets if the combined uncertainty between the databases was large. Of 374 detected sources, 261 have been previously found at another wavelength region, while 113 are new detections. 146 sources have been detected in X-rays, 94 at optical wavelengths, 218 at infrared, and 63 in previous radio surveys. Of the previously identified sources, 1 is extragalactic, while the other 148 as young stellar objects (YSOs). Of the YSOs, 106 have been placed on the standard class system based on the IRAC color-color classification of Allen et al. (2004, ApJS, 154, 363). There are 11 Class 0/I, 26 Class II, and 70 Class III type stars. A total of 225 sources are either new detections or, to the authors' knowledge, have not been previously classified in the literature. Of these remaining objects, they have identified 86 as exhibiting variability or high levels of circular polarization. While the authors cannot exclude the possibility that any of them are extragalactic in nature, quasars are not expected to vary as strongly on timescales of few weeks to few months, and exhibit very weak circular polarization, so these sources (listed in Table 5 of the reference paper) are likely YSO candidates. Using the same criteria of variability and circular polarization would identify only 107 of the 148 previously-known YSOs; thus we cannot tell which of the remaining 139 unidentified sources are YSOs or extragalactic objects. This table was created by the HEASARC in July 2015 based on electronic versions of Tables 2 and 4 from the reference paper, which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlagbsori.html
bib_reference = 2014ApJ...790...49K
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlagbsori&
tap_tablename = vlagbsori
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client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743901
ID = nasa.heasarc/vlagbsper
publisher_did = ivo://nasa.heasarc/vlagbsper
obs_collection = VLAGBSPER
obs_title = VLA Goulds Belt Survey Perseus Region Source Catalog
obs_description = This table contains a source catalog from multi-epoch, large-scale (~2,000 arcmin<sup>2</sup>), fairly deep (~16 microJansky or uJy), high-resolution (~1") radio observations of the Perseus star-forming complex that were obtained with the Karl G. Jansky Very Large Array (VLA) at frequencies of 4.5 and 7.5 GHz. These observations were mainly focused on the clouds NGC 1333 and IC 348, although the authors also observed several fields in other parts of the Perseus complex. They detect a total of 206 sources, 42 of which are associated with young stellar objects (YSOs). The radio properties of about 60% of the YSOs are compatible with a non-thermal radio emission origin. Based on their sample, the authors find a fairly clear relation between the prevalence of non-thermal radio emission and the evolutionary status of the YSOs. By comparing their results with previously reported X-ray observations, they show that YSOs in Perseus follow a Gudel-Benz relation with a value of the kappa parameter (L<sub>X</sub>/L<sub>rad</sub> = kappa x 10<sup>(15.5 +/- 1)</sup> [Hz]) of 0.03, consistent with other regions of star formation. The authors argue that most of the sources detected in their observations that are not associated with known YSOs are extragalactic, but provide a list in the reference paper Of 20 unidentified radio sources whose radio properties are consistent with them being YSO candidates. Finally, they also detect five sources with extended emission features that can clearly be associated with radio galaxies. The observations were collected with the VLA of the National Radio Astronomy Observatory in B and BnA configurations. Two frequency sub-bands, each 1 GHz wide and centered at 4.5 and 7.5 GHz, respectively, were recorded simultaneously. The observations were obtained in three observing sessions, on 2011 March 06/13, April 14/25, and May 01/02/10/19/22, typically separated from one another by a month. This dual-frequency, multi-epoch strategy was chosen to enable the characterization of the spectral index and variability of the detected sources, as well as to help with the identification of the emission mechanisms. The locations of the VLA observations are shown in Figure 1 of the reference paper. Other details of the observations are given in Table 1 of the reference paper. The approximate positions of the two main fields observed are: <pre> RA (ICRS) DE Designation(s) </pre> 03 28 55 +31 22.2 Ced 16 = NGC 1333 03 44 34 +32 09.8 NAME omi Per Cloud = IC 348 <pre> This HEASARC table contains the contents of Table 2 (74 radio sources detected in NGC 1333), Table 3 (91 radio sources detected in IC 348) and Table 4 (41 radio sources detected in single fields in Perseus) from the reference paper, totaling 206 radio sources. This table was created by the HEASARC in February 2018 based on an ASCII version of Table 2 from the reference paper that was obtained from the ApJ website and on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/818/116">CDS catalog J/ApJ/818/116</a> files table3.dat and table4.dat that contains Tables 3 and 4 from the reference paper. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlagbsper.html
bib_reference = 2016ApJ...818..116P
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlagbsper&
tap_tablename = vlagbsper
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client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743913
ID = nasa.heasarc/vlagbsser
publisher_did = ivo://nasa.heasarc/vlagbsser
obs_collection = VLAGBSSER
obs_title = VLA Goulds Belt Survey Serpens Region Source Catalog
obs_description = This table contains results from a deep (~17 µJy) radio continuum observations of the Serpens molecular cloud, the Serpens south cluster, and the W40 region that were obtained using the Jansky Very Large Array (JVLA) in its A configuration. The authors detected a total of 146 sources, 29 of which are young stellar objects (YSOs), 2 of which are BV stars, and 5 more of which are associated with phenomena related to YSOs. Based on their radio variability and spectral index, the authors propose that about 16 of the remaining 110 unclassified sources are also YSOs. For approximately 65% of the known YSOs detected here as radio sources, the emission is most likely non-thermal and related to stellar coronal activity. As also recently observed in Ophiuchus, this sample of YSOs with X-ray counterparts lies below the fiducial Guedel & Benz (1993, ApJ, 405, L63) relation. In the reference paper, the authors analyze the proper motions of nine sources in the W40 region, thus allowing them to better constrain the membership of the radio sources in the region. The Serpens molecular cloud and the Serpens South cluster were observed in the same observing sessions on three different epochs (2011 June 17, July 19, and September 12 UT), using 25 and 4 pointings, respectively, with the JVLA at 4.5 and 4.5GHz. The W40 region, on the other hand, was only observed on two epochs (2011 June 17 and July 16), using 13 pointings. The details of the observations are listed in Table 1 of the reference paper. The authors adopted the same criteria as Dzib et al. (2013, ApJ, 775, 63) to consider a detection as firm. For new sources, i.e., those without reported counterparts in the literature, they considered 5-sigma detections, where sigma is the rms noise of the area around the source. For known sources with counterparts in the literature, on the other hand, they included 4-sigma detections. According to these criteria, they detected 94 sources in the Serpens molecular cloud, 41 in the W40 region, and 8 in the Serpens South cluster, for a total of 143 detections. Out of the 143 sources, 69 are new detections (see Section 3.2 of the reference paper). GBS-VLA source positions were compared with source positions from X-ray, optical, near-IR, mid-IR, and radio catalogs. GBS-VLA sources were considered to have a counterpart at another wavelength when the positional coincidences were better than the combined uncertainties of the two data sets. These were about 1 arcsecond for the IR catalogs. For the X-ray and radio catalogs it depended on the instrument and its configuration. The search was done in SIMBAD and included all the major catalogs. The authors also accessed the lists with all YSOs in the c2d-GB clouds compiled by Dunham et al.(2013, AJ, 145, 94) and L.E. Allen et al. (2015, in preparation). In total, 354 c2d-GB sources lie inside the regions observed by the present survey. In order to find their radio counterparts, the authors imaged regions of 64 pixels in each dimension, centered in the c2d-GB positions, and combining accordingly with each region, the three or two epochs. For this search, they only used the field whose phase center was closest to the source. Three additional radio sources were found in Serpens South in this pursuit, increasing the number of the radio detections to 146. This table was created by the HEASARC in October 2015 based on electronic versions of Tables 2, 3 and 6 from the reference paper, which were obtained from the CDS (Catalog J/ApJ/805/9 files table2.dat, table3.dat and table6.dat). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlagbsser.html
bib_reference = 2015ApJ...805....9O
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlagbsser&
tap_tablename = vlagbsser
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client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743921
ID = nasa.heasarc/vlagbstau
publisher_did = ivo://nasa.heasarc/vlagbstau
obs_collection = VLAGBSTAU
obs_title = VLA Goulds Belt Survey Taurus-Auriga Complex Source Catalog
obs_description = This table contains results from a multi-epoch radio study of the Taurus-Auriga complex made with the Karl G. Jansky Very Large Array (JVLA) at frequencies of 4.5 GHz and 7.5 GHz. A total of 610 sources were detected, 59 of which are related to young stellar objects (YSOs) and 18 to field stars. The properties of 56% of the young stars are compatible with non-thermal radio emission. The authors also show that the radio emission of more evolved YSOs tends to be more non-thermal in origin and, in general, that their radio properties are compatible with those found in other star-forming regions. By comparing their results with previously reported X-ray observations, the authors noticed that YSOs in Taurus-Auriga follow a Guedel-Benz relation with a scaling factor, kappa, of 0.03, as they previously suggested for other regions of star formation. In general, YSOs in Taurus-Auriga and in all the previous studied regions seem to follow this relation with a dispersion of ~1 dex. Finally, the authors propose that most of the remaining sources are related with extragalactic objects but provide a list of 46 unidentified radio sources whose radio properties are compatible with a YSO nature (identified in this implementation of their catalog by values for the parameter radio_yso_flag of 'Y'). The observations were obtained with the JVLA of the National Radio Astronomy Observatory (NRAO) in its B and BnA configuration. Two frequency sub-bands, each 1 GHz wide, and centered at 4.5 and 7.5 GHz, respectively, were recorded simultaneously. The observations were obtained in three different time periods (February 25/26/28 to March 6, April 12/17/20/25, and April 30 to May 1/5/14/22, all in 2011) typically separated from one another by a month: see Table 1 of the reference paper for more details. For their study, the authors observed 127 different target fields distributed across the cloud complex (Figure 1 of the reference paper). The fields were chosen to cover previously known YSOs. In 33 of those fields, the authors could observe more than one YSO target, while in the remaining 94 fields, only one YSO was targeted. In most cases, the infrared evolutionary class (i.e., Classes I, II, or III) or T Tauri evolutionary status (classical or weak line) of the targeted sources was known from the literature. The final images covered circular areas of 8.8 and 14.3 arcminutes in diameter, for the 7.5 and 4.5 GHz sub-bands, respectively, and were corrected for the effects of the position-dependent primary beam response. The noise levels reached for each individual observation was about ~40 microJy and ~30 microJy, at 4.5 GHz and7.5 GHz, respectively. The visibilities of the three, or two, observations obtained for each field were concatenated to produce a new image with a lower noise level (of about ~25 microJy at 4.5 GHz and ~18 microJy at 7.5 GHz). The angular resolution of ~1 arcsecond (see the synthesized beam sizes in Table 1 of the reference paper) allows an uncertainty in position of ~0.1 arcseconds or better. In the observed area, there are a total of 196 known YSOs.The first step was the identification of radio sources in the observed fields. The authors follow the procedure and criteria presented by Dzib et al. (2013, ApJ, 775, 63) who consider a detection as firm if the sources have a flux larger than 4 times the noise level and there is a counterpart known at another wavelength, else they require a flux which is 5 times the noise level. The identification was done using the images corresponding to the concatenation of the observed epochs, which provides the highest sensitivity. From this, a total of 609 sources were detected. Of these sources, 215 were only detected in the 4.5 GHz sub-band, while six were only detected in the 7.5 GHz sub-band. The remaining 388 sources were detected in both sub-bands. The authors searched the literature for previous radio detections, and for counterparts at X-ray, optical, near-infrared, and mid-infrared wavelengths. The search was done using SIMBAD, and accessed all the major catalogs. They considered a radio source to be associated with a counterpart at another wavelength if the separation between the two was below the combined uncertainties of the two data sets. This was about 1.0 arcsecond for the optical and infrared catalogs, but could be significantly larger for some of the radio catalogs (for instance, the NVSS has a positional uncertainty of about 5 arcseconds). They found that only 120 of the sources detected here had previously been reported at radio wavelengths, while the other 491 are new radio detections. On the other hand, the authors found a total of 270 counterparts at other wavelengths. In the literature, 18 are classified as field stars, 49 as extragalactic, 1 is classified as either a star or an extragalactic source in different surveys, 49 are classified as YSOs, 11 are classified as either YSO and extragalactic, and the remaining 143 sources are unclassified. Note that 56 sources were previously known at radio wavelengths but do not have known counterparts at other frequencies. As a consequence, the number of sources that were previously known (at any frequency) is 327, while 284 of the sources in this sample are reported here for the first time. This table was created by the HEASARC in July 2015 based on electronic versions of Tables 1, 4 and 5 from the reference paper, which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlagbstau.html
bib_reference = 2015ApJ...801...91D
obs_regime = radio
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TIMESTAMP = 1714845743933
ID = nasa.heasarc/vlagoodsn
publisher_did = ivo://nasa.heasarc/vlagoodsn
obs_collection = VLAGOODSN
obs_title = VLA GOODS-North Field 1.4-GHz Source Catalog
obs_description = This table contains results from deep, new, wide-field radio continuum observations of the Great Observatories Origins Deep Survey-North (GOODS-North) field. (The GOODS-North field covers ~160 arcmin<sup>2</sup> centered on the Hubble Deep Field North (Williams et al. 1996, AJ, 112, 1335) and is unrivaled in terms of its ancillary data sets, which include extremely deep Chandra, Hubble Space Telescope (HST), and Spitzer observations, deep UBVRIJHK ground-based imaging and ~3500 spectroscopic redshifts from 8 to 10 m telescopes). The resulting 1.4-GHz map has a synthesized beam size of ~1.7" and an rms noise level of ~3.9 microJansky per beam (µJy/beam) near its center and ~8 µJy/beam at 15 arcminutes from phase center. The authors have cataloged 1230 discrete radio emitters, within a 40' x 40' region, above a 5-sigma detection threshold of ~20 uJy at the field center. New techniques, pioneered by Owen & Morrison (2008, AJ, 136, 1889), have enabled the authors to achieve a dynamic range of 6800:1 in a field that has significantly strong confusing sources. The authors compare the 1.4-GHz (20-cm) source counts with those from other published radio surveys. Their differential counts are nearly Euclidean below 100 uJy with a median source diameter of ~1.2". This adds to the evidence presented by Owen & Morrison that the natural confusion limit may lie near 1 uJy. If the Euclidean slope of the counts continues down to the natural confusion limit as an extrapolation of their log N-log S, this indicates that the cutoff must be fairly sharp below 1 uJy, else the cosmic microwave background temperature would increase above 2.7K at 1.4GHz. A useful combined total of 165 hours of NRAOS's Very Large Array (VLA) A-configuration 1.4-GHz observations were obtained between 2005 February and 2006 February, all done at night so as to avoid solar interference, for a region centered at RA and Dec of 12:36:49.4, +62:12:58 (J2000). (See Table 1 of the reference paper for the VLA observing log) This table was created by the HEASARC in September 2013 based on CDS Catalog J/ApJS/188/178 file table2.dat This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlagoodsn.html
bib_reference = 2010ApJS..188..178M
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlagoodsn&
tap_tablename = vlagoodsn
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client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743945
ID = nasa.heasarc/vlahdf20cm
publisher_did = ivo://nasa.heasarc/vlahdf20cm
obs_collection = VLAHDF20CM
obs_title = VLA Hubble Deep Field 20-cm Source Catalog
obs_description = The authors have conducted a deep radio survey with the Very Large Array (VLA) at 1.4 GHz of a region containing the Hubble Deep Field (HDF). This survey overlaps previous observations at 8.5 GHz allowing them to investigate the radio spectral properties of microJansky sources to flux densities greater than 40 microJy (uJy) at 1.4 GHz and greater than 8 uJy at 8.5 GHz. A total of 371 sources have been catalogued at 1.4 GHz as part of a complete sample within 20 arcminutes of the HDF. The differential source count for this region is only marginally sub-Euclidean and is given by n(S) = (8.3 +/- 0.4) S^(-2.4 +/- 0.1) sr<sup>-1</sup> Jy<sup>-1</sup>. Above about 100 uJy the radio source count is systematically lower in the HDF as compared to other fields. The authors conclude that there is clustering in this radio sample on size scales of 1 to 40 arcminutes. The 1.4 GHz-selected sample shows that the radio spectral indices are preferentially steep (mean spectral index of 0.85) and that the sources are moderately extended with average angular size Theta = 1.8". Optical identification with disk-type systems at z ~ 0.1 - 1 suggests that synchrotron emission, produced by supernovae remnants, is powering the radio emission in the majority of sources. In 1996 November, the authors observed a field centered on the Hubble Deep Field (RA, Dec (J2000.0) = (12<sup>h</sup> 36<sup>m</sup> 49.4<sup>s</sup>, 62<sup>o</sup> 12' 58.00") for a total of 50 hours at 20 cm in the A configuration of the VLA. They reached an rms noise level near the center of the field of 7.5 uJy. They adopted 40 uJy as the formal completeness limit over the entire 1 degree field in their untapered naturally weighted 2 arcseconds image. The authors identified 314 sources within 20 arcminutes of the field center (20% power contour). They found 57 additional sources within this same region (presumably resolved at 2" resolution) in lower resolution (3.5 and 6") tapered images above completeness levels of 50 uJy at 3.5" resolution and 75 uJy at 6" resolution, making a grand total of 371 radio sources detected at 1.4 GHz within 20 arcminutes of the phase center of the field. This table was created by the HEASARC in June 2012 based on CDS Catalog J/ApJ/533/611 file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlahdf20cm.html
bib_reference = 2000ApJ...533..611R
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlahdf20cm&
tap_tablename = vlahdf20cm
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TIMESTAMP = 1714845743953
ID = nasa.heasarc/vlalh1400m
publisher_did = ivo://nasa.heasarc/vlalh1400m
obs_collection = VLALH1400M
obs_title = VLA Lockman Hole 1400-MHz Radio Source Catalog
obs_description = In the run-up to routine observations with the upcoming generation of radio facilities, the nature of the sub-mJy radio population has been hotly debated. In this paper, the authors describe multi-frequency data designed to probe the emission mechanism that dominates in these faint radio sources. Their analysis is based on observations of the Lockman Hole (LH) using the Giant Metrewave Radio Telescope (GMRT) near Pune, India - the deepest 610-MHz imaging yet reported - together with 1.4-GHz imaging from the Very Large Array (VLA), which are well matched in resolution and sensitivity to the GMRT data: sigma<sub>610MHz</sub> ~ 15 microJy/beam (uJy/beam), sigma}<sub>1.4GHz</sub> ~ 6 uJy/beam, and full width at half-maximum (FWHM) ~ 5 arcseconds. The GMRT and VLA data are cross-matched to obtain the radio spectral indices for the faint radio emitters. During six 12-hr sessions in 2006 February and July, the authors obtained data at 610 MHz for three pointings (FWHM ~ 43 arcminutes) in the LH (see Table 1 of the reference paper for full details), separated by 11 arcminutes (the LOCKMAN-E, LOCK-3 and LHEX-4 fields), typically with 28 of the 30 antennas that comprise the GMRT. The total integration time in each field, after overheads, was 16 hr. The final image had a noise level in the central 100 arcmin<sup>2</sup> of 14.7 uJy/beam, the deepest map reported at 610 MHz as of the date of publication, despite the modest integration time. New and archival data were obtained at the same three positions using the National Radio Astronomy Observatory's VLA, largely in its B configuration. This table contains 1450 sources found in the LH field at 1400 MHz by the VLA. For 17 of the sources which have multiple components, the 29 individual components are listed as well. Thus, the final table contains 1479 (1450 + 29) entries. Source extraction was based on criteria of peak brightness > 5 times the local rms and integrated flux density > 3 times the local rms. This table was created by the HEASARC in February 2012 based on CDS Catalog J/MNRAS/397/281 file table4.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlalh1400m.html
bib_reference = 2009MNRAS.397..281I
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlalh1400m&
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client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743965
ID = nasa.heasarc/vlalhn3ghz
publisher_did = ivo://nasa.heasarc/vlalhn3ghz
obs_collection = VLALHN3GHZ
obs_title = VLA Lockman Hole 3-GHz Radio Source Catalog
obs_description = This table is from the second of two papers describing the observations and source catalogs derived from sensitive 3-GHz images of the Lockman Hole North using the Karl G. Jansky Very Large Array (VLA). In their paper, the authors describe the reduction and cataloguing process, which yielded an image with 8-arcsecond resolution and instrumental noise of sigma<sub>n</sub> = 1.01 µJy/beam (µJy/beam) rms (before primary beam corrections) and a catalog of 558 sources detected above 5 * sigma<sub>n</sub>. The authors also include details of how they estimate source spectral indices across the 2-GHz VLA bandwidth, finding a median index of -0.76 +/- 0.04. Stacking of source spectra reveals a flattening of spectral index with decreasing flux density. In the reference paper, the authors present a source count derived from the catalog. They show a traditional count estimate compared with a completely independent estimate made via a P(D) confusion analysis, and find very good agreement. Cross-matches of the catalog with X-ray, optical, infrared, radio, and redshift catalogs are also presented. The X-ray, optical and infrared data, as well as AGN selection criteria allow them to classify 10% as radio-loud AGN, 28% as radio-quiet AGN, and 58% as star-forming galaxies, with only 4% unclassified. Observations were made with the VLA in the C configuration at S band, with a frequency range of 2 to 4GHz, with a total of roughly 50 hours of on-source time in 2012. The HEASARC has converted the radio and IR flux density units from those given in the original table (µJy and µJy/beam) to its standard units for radio flux densities (mJy and mJy/beam). This table was created by the HEASARC in April 2017 based on CDS Catalog J/MNRAS/462/2934 files cat3ghz.dat and catcrx.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlalhn3ghz.html
bib_reference = 2016MNRAS.462.2934V
obs_regime = radio
obs_regime = optical
obs_regime = infrared
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlalhn3ghz&
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tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743973
ID = nasa.heasarc/vlam311p4g
publisher_did = ivo://nasa.heasarc/vlam311p4g
obs_collection = VLAM311P4G
obs_title = VLA M 31 1.4-GHz Source Catalog
obs_description = This table contains the Data Release 2 of the Point Source Catalog created from a series of previously constructed radio-continuum images of M 31 at a wavelength lambda of 20 cm (frequency nu = 1.4 GHz) from archived VLA observations. In total, the authors identify a collection of 916 unique discrete radio sources across the field of M 31. Comparing these detected sources with those listed by Gelfand et al. (2004, ApJS, 155, 89, HEASARC table VLAM31325M) at lambda = 92 cm (325 MHz), the spectral index of 98 sources has been derived. The majority (73%) of these sources exhibit a spectral index of alpha < -0.6, indicating that their emission is predominantly non-thermal in nature, which is typical for background objects and Supernova Remnants (SNRs). This table contains the integrated flux densities for 1,131 detections of 916 unique sources detected at 1.4 GHz in 28 VLA observations. Of these 916 unique sources, 109 were detected in at least two separate images. For such sources, the authors list a group identifier, a group count, and an average flux and error. Sources were cross referenced with the Gelfand et al. (2004) catalog of sources detected at 92 cm. For matched sources, the flux density at this wavelength and the derived spectral index between 20 and 92 cm are listed. This table was created by the HEASARC in May 2015 based on CDS Catalog J/Other/Ser/189.15 file m31radio.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlam311p4g.html
bib_reference = 2014SerAJ.189...15G
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlam311p4g&
tap_tablename = vlam311p4g
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743985
ID = nasa.heasarc/vlam31325m
publisher_did = ivo://nasa.heasarc/vlam31325m
obs_collection = VLAM31325M
obs_title = VLA M 31 325-MHz Source Catalog
obs_description = This table contains some of the results from a 325-MHz radio survey of M 31, conducted with the A configuration of the Very Large Array. The survey covered an area of 7.6 square degrees, and a total of 405 radio sources between <~ 6" and 170" in extent were mapped with a resolution of 6" and a 1-sigma sensitivity of ~ 0.6mJy/beam. For each source, its morphological class, major axis theta<sub>M</sub>, minor axis theta<sub>m</sub>, position angle theta<sub>PA</sub>, peak flux I, integrated flux density S, spectral index alpha, and spectral curvature parameter {phi were calculated. A comparison of the flux and radial distribution - both in the plane of the sky and in the plane of M 31 - of these sources with those of the XMM-Newton Large-Scale Structure Survey and the Westerbork Northern Sky Survey revealed that a vast majority of sources detected are background radio galaxies. As a result of this analysis, the authors expect that only a few sources are intrinsic to M 31. This study is based on a 5 hr (4 hr on-source) observation of M 31 conducted on 2000 December 15 with the VLA in A configuration. The procedures used to generate the source list and the source properties (essentially making use of the MIRIAD task SFIND) are discussed in Sections 2.2.2 and 2.3 of the reference paper, respectively. This table was created by the HEASARC in September 2014 based on CDS Catalog J/ApJS/155/89 file table3.dat, the GLG (Gelfand, Lazio, Gaensler) source list. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlam31325m.html
bib_reference = 2004ApJS..155...89G
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlam31325m&
tap_tablename = vlam31325m
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845743993
ID = nasa.heasarc/vlanep
publisher_did = ivo://nasa.heasarc/vlanep
obs_collection = VLA
obs_title = VLA 1.5-GHz North Ecliptic Pole Survey
obs_description = The VLANEP database contains the VLA-NEP survey of 29.3 square degrees around the North Ecliptic Pole mapped with the VLA at 20 cm (1.5 GHz) in the `C-configuration`. The database table contains 2435 radio sources with flux densities ranging from 0.3 to 1000 mJy, including over 200 fainter than 1 mJy. Source positions have been corrected for instrumental effects, and most positions are accurate to less than 2 arcseconds. The sensitivity varies from field to field, with the 1 sigma level being approximately 0.06 mJy at the center of the inner fields and 0.12 mJy at the center of the outer fields. Sensitivity drops with distance from the center of each field due to the primary beam response of the VLA antennas and interferometer effects. Source flux densities have been corrected for these effects. The spatial resolution varies from field to field, with the typical HPBW being 20 arcseconds. Source positions have been corrected for instrumental effects, and most positions are accurate to less than 2 arcseconds. Approximately 6% of the sources were found to be extended with angular sizes greater than 30 arcseconds. This catalog was recreated at the HEASARC in February 2001 (replacing a previous version: some parameters were renamed, and the source names were changed to the format recommended for VLA-NEP sources in the Dictionary of Nomenclature of Celestial Objects maintained at the CDS) based on CDS/ADC Catalog J/ApJS/93/145/table2. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlanep.html
bib_reference = 1994ApJS...93..145K
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlanep&
tap_tablename = vlanep
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744005
ID = nasa.heasarc/vlaonccat
publisher_did = ivo://nasa.heasarc/vlaonccat
obs_collection = VLAONCCAT
obs_title = VLA Orion Nebula Cluster Compact Source Catalog
obs_description = This table contains a deep centimeter-wavelength catalog of the Orion Nebula Cluster (ONC), based on a 30-hr single-pointing observation with the Karl G. Jansky Very Large Array (JVLA) in its high-resolution A configuration using two 1-GHz bands centered on 4.7 and 7.3 GHz. A total of 556 compact sources were detected in a map with a nominal rms noise of 3 µJy/beam, limited by complex source structure and the primary beam response. Compared to previous catalogs, these detections increase the sample of known compact radio sources in the ONC by more than a factor of seven. The new data show complex emission on a wide range of spatial scales. Following a preliminary correction for the wideband primary-beam response, the authors determine radio spectral indices for 170 sources whose index uncertainties are less than +/-0.5. They compare the radio to the X-ray and near-infrared point-source populations, noting similarities and differences. The observations were carried out with the JVLA of the National Radio Astronomy Observatory on 2012 September 30 and October 2-5 under the auspices of the project code SD630. Data were taken using the VLA's C-band (4-8 GHz) receivers in full polarization mode, with two 1-GHz basebands centered at 4.736 and 7.336 GHz to provide a good baseline for source spectral index determination. Apart from the first epoch, the field was simultaneously observed with the Chandra X-Ray Observatory. Mostly of interest for variability information, these data will be presented as part of a follow-up paper. This table was created by the HEASARC in September 2016 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/822/93">CDS Catalog J/ApJ/822/93</a> file table1.dat (the compact source catalog). Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlaonccat.html
bib_reference = 2016ApJ...822...93F
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlaonccat&
tap_tablename = vlaonccat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744017
ID = nasa.heasarc/vlasdf20cm
publisher_did = ivo://nasa.heasarc/vlasdf20cm
obs_collection = VLASDF20CM
obs_title = VLA SWIRE Deep Field 20-cm Source Catalog
obs_description = This table contains some of the results from deep radio observations taken with the Very Large Array at a center frequency of 1400 MHz covering a region of the Spitzer Wide-area InfraRed Extragalactic (SWIRE) Survey of the Spitzer Legacy survey, centered at RA and Dec of 10:46:00, +59:01:00 (J2000). The reduction and cataloging of radio sources are described in the reference paper. This table comprises the catalog of the sources detected above 5 sigma. The survey presented is the deepest so far in terms of the radio source density on the sky. Perhaps surprisingly, the sources down to the bottom of the catalog appear to have median angular sizes which are still greater than 1 arcsecond, like their cousins 10-100 times stronger. The shape of the differential log N-log S counts also seems to require a correction for the finite sizes of the sources in order to be self-consistent. If the log N-log S normalization remains constant at the lowest flux densities, there are about six sources per square arcminute at 15 microJy (uJy) at 20 cm. Given the finite-source size this implies that we may reach the natural confusion limit near 1 uJy. The observations were made with the VLA in A, B, C, and D configurations for a total of almost 140 hr on-source between 2001 December and 2004 January. Since the total time is dominated by the A congiguration, the final image for analysis has a resolution of ~1.6 arcseconds. This table was created by the HEASARC in September 2010 based on CDS catalog J/AJ/136/1889/ file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlasdf20cm.html
bib_reference = 2008AJ....136.1889O
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlasdf20cm&
tap_tablename = vlasdf20cm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744029
ID = nasa.heasarc/vlasdf90cm
publisher_did = ivo://nasa.heasarc/vlasdf90cm
obs_collection = VLASDF90CM
obs_title = VLA SWIRE Deep Field 90-cm Source Catalog
obs_description = This table contains some of the results from the deepest radio continuum surveys to date at a radio wavelength of >~ 1m. The observations were taken with the VLA at 324.5 MHz covering a region of the SWIRE Spitzer Legacy survey, centered at RA and Dec of 10:46:00, +59:01:00 (J2000). The data reduction and analysis are described in the reference paper and a catalog of the sources detected above 5 sigma is presented herein. The authors also discuss the observed angular size distribution for the sample in their paper, and, using their deeper 20-cm survey of the same field (Owen and Morrison 2008, AJ, 136, 1889), they calculate spectral indices for sources detected in both surveys. They report log N-log S counts at 90 cm which show a flattening below 5 mJy. Given the median redshift of the population, z ~ 1, the spectral flattening and the flattening of the log N-log S counts occur at radio luminosities normally associated with AGN rather than with galaxies dominated by star formation. Observations were made of a single pointing center position (given above), with the VLA in A and C configurations for a total of almost 85 hours on-source between 2006 February and 2007 January. However, due to the ongoing EVLA upgrade, only 22 working antennae were typically avaliable in A and 18 in C. Thus, the total integration time was equivalent to ~ 63 hours in A and even less in C, with correspondingly less u-v coverage. This table was created by the HEASARC in September 2010 based on CDS catalog J/AJ/137/4846/ file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlasdf90cm.html
bib_reference = 2009AJ....137.4846O
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlasdf90cm&
tap_tablename = vlasdf90cm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744037
ID = nasa.heasarc/vlass821p4
publisher_did = ivo://nasa.heasarc/vlass821p4
obs_collection = VLASS821P4
obs_title = VLA SDSS Stripe 82 Survey 1.4-GHz Source Catalog
obs_description = This table contains results from a high-resolution radio survey of the Sloan Digital Sky Survey (SDSS) Southern Equatorial Stripe, also known as Stripe 82. This 1.4-GHz survey was conducted with the Very Large Array (VLA) primarily in the A configuration, with supplemental B configuration data to increase sensitivity to extended structure. The survey has an angular resolution of 1.8 arcseconds and achieves a median rms noise of 52 microJy/beam (uJy/beam) over 92 deg<sup>2</sup>. This is the deepest 1.4-GHz survey to achieve this large of an area, filling a gap in the phase space between small, deep and large, shallow surveys. It also serves as a pilot project for a larger high-resolution survey with the Expanded Very Large Array (EVLA). The authors discuss the technical design of the survey and details of the observations, and outline their method for data reduction, in the reference paper. They present a catalog of 17,969 isolated radio components, for an overall source density of ~195 sources deg<sup>-2</sup>. The astrometric accuracy of the data is excellent, with an internal check utilizing multiply observed sources yielding an rms scatter of 0.19 arcseconds in both Right Ascension and Declination. A comparison to the SDSS DR7 Quasar Catalog further confirms that the astrometry is well-tied to the optical reference frame, with mean offsets of 0.02" +/- 0.01" in Right Ascension, and 0.01" +/- 0.02" in Declination. A check of their photometry reveals a small, negative CLEAN-like bias on the level of 35 uJy. The authors report on the catalog completeness, finding that 97% of FIRST-detected quasars are recovered in the new Stripe 82 radio catalog, while faint, extended sources are more likely to be resolved out by the resolution bias. In their paper, they conclude with a discussion of the optical counterparts to the catalog sources, including 76 newly detected radio quasars. The full catalog as well as a search page and cutout server are available online at <a href="http://third.ucllnl.org/cgi-bin/stripe82cutout">http://third.ucllnl.org/cgi-bin/stripe82cutout</a>. The SDSS Stripe 82 observations were made with the National Radio Astronomy Observatory's (NRAO's) VLA. The data were collected over two VLA cycles, 2007-2008 and 2008-2009. The majority of the observations were taken in the A configuration, but the authors also obtained B-configuration coverage of the area in order to improve the sampling of the Fourier (U-V) plane and to increase sensitivity to the extended structure. Area 1 (delineated in black in Figure 1(a) of the paper) was covered in the A and B configurations in 2007-2008, and Area 2 (delineated in purple in Figure 1(a) of the paper) in the A and B configurations in 2008-2009. Area 1 is made up of 275 pointings, and Area 2 has 374, coming to 649 fields, and 92 deg<sup>2</sup> covered in total. This table was created by the HEASARC in August 2013 based on a complete machine-readable version of Table 1 from the reference paper which was kindly provided by the first author. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlass821p4.html
bib_reference = 2011AJ....142....3H
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlass821p4&
tap_tablename = vlass821p4
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744049
ID = nasa.heasarc/vlasxdf1p4
publisher_did = ivo://nasa.heasarc/vlasxdf1p4
obs_collection = VLASXDF1P4
obs_title = VLA Subaru/XMM-Newton Deep Field 1.4-GHz Source Catalog
obs_description = This table contains results from the deep radio imaging at 1.4 GHz of the 1.3-deg<sup>2</sup> Subaru/XMM-Newton Deep Field (SXDF), made with the Very Large Array (VLA) in B and C configurations. This resulted in a radio map of the entire field, and a catalog of 505 sources covering 0.8 deg<sup>2</sup> to a peak flux density limit of 100 microJansky (uJy), which corresponds to signal-to-noise (S/N) ratios of between 5 and 8. Robust optical identifications are provided for 90 per cent of the sources, and suggested identifications are presented for all but 14 (of which seven are optically blank, and seven are close to bright contaminating objects). The authors show that the optical properties of the radio sources do not change with flux density, suggesting that active galactic nuclei (AGN) continue to contribute significantly at faint flux densities. they test this assertion by cross-correlating their radio catalog with the X-ray source catalog and conclude that radio-quiet AGN become a significant population at flux densities below 300 uJy, and may dominate the population responsible for the flattening of the radio source counts if a significant fraction of them are Compton-thick. The SXDF was observed with NRAO's VLA in B-array using the 14 overlapping pointings arranged an an hexagonal pattern that are listed in Table 1 of the reference paper. Three test observations of pointings 1, 4 and 6 were taken on 2001 May 17, and the rest of the data were obtained in 13 runs, each lasting 4.5 hours, between 2002 August 10 and September 9. All 14 pointings were re-observed in C-array on 2003 January 15 to provide additional information on larger angular scales. This table contains the catalog of 505 detected radio sources and their proposed optical counterparts (the latter taken mostly from the ultra-deep BRi'z' Suprime-Cam images of the SXDF). As mentioned above, 14 of these 505 radio sources have no suggested identifications. Additionally, 7 of the radio sources (source numbers 16, 114, 129, 263, 360, 361 and 488) have 2 listed optical identifications: in such cases, there are 2 entries for each source listed detailing the alternative optical counterparts, and with identical sets of radio parameters. Thus, there are 512 = 505 + 7 entries in this table. This table was created by the HEASARC in August 2013 based on CDS Catalog J/MNRAS/372/741 file table3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlasxdf1p4.html
bib_reference = 2006MNRAS.372..741S
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlasxdf1p4&
tap_tablename = vlasxdf1p4
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744057
ID = nasa.heasarc/vlasxdfoid
publisher_did = ivo://nasa.heasarc/vlasxdfoid
obs_collection = VLASXDFOID
obs_title = VLA Subaru/XMM-Newton Deep Field 1.4-GHz Sources Optical/Near-IR Counterparts
obs_description = In Simpson et al. (2006, MNRAS, 372, 741, hereafter Paper I, available at the HEASARC as the <a href="/W3Browse/radio-catalog/vlasxdf1p4.html">VLASXDF1P4</a> table, the authors presented a catalog of 505 sources with 1.4-GHz peak radio flux densities greater than 100 uJy over a 0.81 deg<sup>2</sup> region of the Subaru/XMM-Newton Deep Field (SXDF) and some of the properties of their optical counterparts. In this study (Simpson et al. 2012, MNRAS, 421, 3060, Paper III in the series) the authors present spectroscopic and 11-band photometric redshifts for galaxies in the 100-uJy Subaru/XMM-Newton Deep Field radio source sample. The authors find good agreement between their redshift distribution and that predicted by the Square Kilometre Array (SKA) Simulated Skies project. They find no correlation between K-band magnitude and radio flux, but show that sources with 1.4-GHz flux densities below ~ 1 mJy are fainter in the near-infrared than brighter radio sources at the same redshift, and they discuss in their paper the implications of this result for spectroscopically incomplete samples where the K-z relation has been used to estimate redshifts. The authors use the infrared-radio correlation to separate their sample into radio-loud and radio-quiet objects and show that only radio-loud hosts have spectral energy distributions consistent with predominantly old stellar populations, although the fraction of objects displaying such properties is a decreasing function of radio luminosity. Many of the spectra presented in this study were obtained as part of the European Southern Observatory (ESO) program P074.A-0333, undertaken using the Visible Multi-Object Spectrograph (VIMOS) instrument on UT3/Melipal. Several observational campaigns have obtained spectra of objects within the SXDF, and Paper II in this series (Vardoulaki et al. 2008, MNRAS, 387, 505) presented spectra for 28 of the brightest 37 radio sources, obtained from a variety of sources. The near-infrared data used here come from the third data release (DR3) of the UKIRT (United Kingdom Infrared telescope) Infrared Deep Sky Survey, while the optical data in the UDS come from the SXDF, which comprises five separate Suprime-Cam pointings. This table was created by the HEASARC in August 2013 based on CDS Catalog J/MNRAS/421/3060 file table1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlasxdfoid.html
bib_reference = 2012MNRAS.421.3060S
obs_regime = infrared
obs_regime = optical
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlasxdfoid&
tap_tablename = vlasxdfoid
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744069
ID = nasa.heasarc/vlaxl325mh
publisher_did = ivo://nasa.heasarc/vlaxl325mh
obs_collection = VLAXL325MH
obs_title = VLA XMM Large Scale Structure Field 325-MHz Source Catalog
obs_description = The XMM Large Scale Structure survey (XMM-LSS) is an X-ray survey aimed at studying the large scale structure of the Universe. The XMM-LSS field (centered at RA (J2000) = 02<sup>h</sup> 24<sup>m</sup> 00.27<sup>s</sup>, Dec (J2000) = -04<sup>o</sup> 09' 47.6") is currently being followed up using observations across a wide range of wavelengths, and in their paper the authors present the observational results of a low frequency radio survey of the XMM-LSS field using the Very Large Array at 74 and 325 MHz. This survey will map out the locations of the extragalactic radio sources relative to the large scale structure as traced by the X-ray emission. This is of particular interest because radio galaxies and radio-loud AGN show strong and complex interactions with their small and larger scale environment, and different classes of radio galaxies are suggested to lie at different places with respect to the large scale structure. For the phase calibration of the radio data, the authors used standard self-calibration at 325 MHz and field-base calibration at 74 MHz. Polyhedron-based imaging as well as mosaicking methods were used at both frequencies. At 74 MHz, the resolution was 30 arcseconds, the median 5-sigma sensitivity was ~ 162 mJy/beam and 666 sources were detected over an area of 132 square degrees. At 325 MHz, the resolution was 6.7 arcseconds, the median 5-sigma sensitivity was 4 mJy/beam, and 847 sources were detected over an area of 15.3 square degrees. At 325 MHz, a region of diffuse radio emission which is a cluster halo or relic candidate was detected. The observations were conducted using the VLA in July 2003 in the A-configuration (most extended) and in June 2002 in the B-configuration. This table contains the VLA 325-MHz source list, comprising 605 single sources and 615 components of 237 multiple sources, for a total of 1220 entries. (Notice that, in Section 4.1 of the reference paper, somewhat different numbers are given, i.e., the authors quote 621 single sources and 226 multiple sources). For the multiple sources, each component (A, B, etc.) is listed separately, in order of decreasing brightness. This table was created by the HEASARC in March 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/456/791">CDS Catalog J/A+A/456/791</a> file tablea1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlaxl325mh.html
bib_reference = 2006A&A...456..791T
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlaxl325mh&
tap_tablename = vlaxl325mh
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744077
ID = nasa.heasarc/vlaxl74mhz
publisher_did = ivo://nasa.heasarc/vlaxl74mhz
obs_collection = VLAXL74MHZ
obs_title = VLA XMM Large Scale Structure Field 74-MHz Source Catalog
obs_description = The XMM Large Scale Structure survey (XMM-LSS) is an X-ray survey aimed at studying the large scale structure of the Universe. The XMM-LSS field (centered at RA (J2000) = 02<sup>h</sup> 24<sup>m</sup> 00.27<sup>s</sup>, Dec (J2000) = -04<sup>o</sup> 09' 47.6") is currently being followed up using observations across a wide range of wavelengths, and in their paper the authors present the observational results of a low frequency radio survey of the XMM-LSS field using the Very Large Array at 74 and 325 MHz. This survey will map out the locations of the extragalactic radio sources relative to the large scale structure as traced by the X-ray emission. This is of particular interest because radio galaxies and radio-loud AGN show strong and complex interactions with their small and larger scale environment, and different classes of radio galaxies are suggested to lie at different places with respect to the large scale structure. For the phase calibration of the radio data, the authors used standard self-calibration at 325 MHz and field-base calibration at 74 MHz. Polyhedron-based imaging as well as mosaicking methods were used at both frequencies. At 74 MHz, the resolution was 30 arcseconds, the median 5-sigma sensitivity was ~ 162 mJy/beam and 666 sources were detected over an area of 132 square degrees. At 325 MHz, the resolution was 6.7 arcseconds, the median 5-sigma sensitivity was 4 mJy/beam, and 847 sources were detected over an area of 15.3 square degrees. At 325 MHz, a region of diffuse radio emission which is a cluster halo or relic candidate was detected. The observations were conducted using the VLA in July 2003 in the A-configuration (most extended) and in June 2002 in the B-configuration. This table contains the VLA 74-MHz source list, comprising 617 single sources and 108 components of 51 multiple sources, for a total of 725 entries. (Notice that, in Section 4.3 of the reference paper, somewhat different numbers are given, i.e., the authors quote 615 single sources). For the multiple sources, each component (A, B, etc.) is listed separately, in order of decreasing brightness. This table was created by the HEASARC in March 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/456/791">CDS Catalog J/A+A/456/791</a> file tablea2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlaxl74mhz.html
bib_reference = 2006A&A...456..791T
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlaxl74mhz&
tap_tablename = vlaxl74mhz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744089
ID = nasa.heasarc/vlssr
publisher_did = ivo://nasa.heasarc/vlssr
obs_collection = VLSSR
obs_title = VLA Low-Frequency Sky Survey Redux Source Catalog
obs_description = The Very Large Array (VLA) Low-Frequency Sky Survey (VLSS: see Cohen et al. 2007, AJ, 134, 1245) covers 95% of the 3 pi sr of sky area above -30 degrees Declination at most RAs (complete above -10 degrees Declination, while in some areas data are available down to Declinations of -36 degrees) at a frequency of 74 MHz, a resolution of 80", and an average rms map sensitivity of sigma ~ 0.130 Jy/beam. The survey was intended to serve as a low-frequency counterpart to the National Radio Astronomy Observatory (NRAO)-VLA Sky Survey (NVSS) at 1400 MHz, allowing spectral information to be compiled for statistical samples of sources. It also provides a low-frequency sky model. In their 2012 and 2014 reference papers, the authors present the details of improvements to data processing and analysis which were used for a re-reduction of the VLSS data, which they dub the VLSS redux or VLSSr. They used the VLSS catalogue as a sky model to correct the ionospheric distortions in the data and create a new set of sky maps and corresponding catalog at 73.8 MHz. The VLSS Redux (VLSSr) has a resolution of 75", and an average map rms noise level of sigma ~ 0.1 Jy beam<sup>-1</sup>. The clean bias is 0.66 x sigma and the theoretical largest angular size is 36 arcminutes. Six previously unimaged fields are included in the VLSSr, which has an unbroken sky coverage over 9.3 steradian above an irregular southern boundary. The final catalog includes 92,965 sources (in the abstract of Lane et al. (2014) it states 92.964 sources). The VLSSr improves upon the original VLSS in a number of areas including imaging of large sources, image sensitivity, and clean bias; however the most critical improvement is the replacement of an inaccurate primary beam correction which caused source flux errors which vary as a function of radius to the nearest pointing center in the VLSS. This table was initially created by the HEASARC in December 2012, based on the FITS file CATALOG.FIT obtained from the NRAO website at <a href="http://www.cv.nrao.edu/vlss/CATALOG/">http://www.cv.nrao.edu/vlss/CATALOG/</a>. It was updated in July 2014 with the the table data from the latest file on the NRAO website (which was marked as last modified on 26 August 2013). Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlssr.html
bib_reference = 2012RaSc...47.....L
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlssr&
tap_tablename = vlssr
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744097
ID = nasa.heasarc/vlulxcat
publisher_did = ivo://nasa.heasarc/vlulxcat
obs_collection = VLULXCAT
obs_title = Extremely Luminous X-Ray Source Candidates Catalog
obs_description = Using Chandra archive data, the authors conducted a thorough survey of luminous X-ray sources. They directly analyzed about 9400 Chandra ACIS observations and cross-correlated the detected X-ray sources with 77,000 galaxies within a distance of 250 Mpc. The final catalog includes 119 unique luminous X-ray source candidates with L<sub>X</sub> > 3 x 10<sup>40</sup> erg/s from 93 galaxies or 41 HLX candidates with L<sub>X</sub> > 1 x 10<sup>41</sup> erg/s from 35 galaxies. The authors derive a moderate contamination rate due to foreground or background sources. In the reference paper, they also cross-correlate the catalog with FIRST, perform variability and periodicity tests, and analyze one HLX candidate in particular. This catalog could be a starting point to perform follow-up observations. In order to know whether an X-ray source falls within a particular galaxy, for each galaxy, the authors collected its center's RA, Dec, distance, and D<sub>25</sub> isophotal info, which includes major axis length, minor axis length, and the position angle of the major axis from the PGC2003 Catalog (Paturel et al. 2003, A&A, 412, 45), which includes the full RC3 catalog and has all of the necessary parameters except for distance. The authors restricted the minimum major axis length to be 10 arcseconds, and collected their distances from NED as much as possible. Their final sample includes 77,000 galaxies within 250 Mpc. The authors used all of the Chandra ACIS data in TE mode that were released before 2014, which includes 9400 ObsIDs. A roughly linear relation between the flux and count rate derived by PIMMS 4.6b was established assuming a power-law spectral shape and galactic foreground extinction (Kalberla et al. 2005, A&A, 440, 775). Any source with a PIMMS luminosity larger than 5 x 10<sup>39</sup> erg s<sup>-1</sup> would be recalculated by the CIAO script model flux assuming a power-law index of 1.7 in the 0.3 - 8.0 keV energy band. After the recalculation, 1,809 X-ray sources with L<sub>x</sub> > 3 x 10<sup>40</sup> erg s<sup>-1</sup> falling within 640 D<sub>25</sub> contours covered by 905 ObsIDs were picked out. A large fraction of the 1,809 sources are galactic nuclei and some of them are repeated. Only off-nuclear sources are considered in this paper. In addition, the centers of the galaxies given by PGC2003 are not necessarily precise and the specific environments of the 1,809 sources are different. Therefore, the authors visually checked the Chandra and DSS images simultaneously, since two-band inspection can help to exclude the nuclear sources, bright knots, and extended sources. X-ray sources with clear DSS features would be dropped because, for a source with a visual magnitude <20 and a distance >30 Mpc, its absolute magnitude would be brighter than -12.4, which is beyond the limit of the brightest star clusters. This table was created by the HEASARC in February 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/222/12">CDS Catalog J/ApJS/222/12</a> file table1.dat, the list of very luminous X-ray source candidates found within the D<sub>25</sub> ellipses of Chandra ACIS-observed PGC2003 galaxies lying within 250 Mpc. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vlulxcat.html
bib_reference = 2016ApJS..222...12G
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vlulxcat&
tap_tablename = vlulxcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744109
ID = nasa.heasarc/vvds20cm
publisher_did = ivo://nasa.heasarc/vvds20cm
obs_collection = VVDS20CM
obs_title = VLA-VIRMOS Deep Field 20-cm Source Catalog
obs_description = The authors of this table conducted a deep survey (rms noise ~ 17 microJansky or uJy) with the Very Large Array (VLA) at 1.4 GHz, with a resolution of 6 arcseconds, of a 1 deg<sup>2</sup> region included in the VIRMOS VLT Deep Survey that is centered at RA and Dec (J2000.0) of 02 26 00, -04 30 00, hereafter the VLA-VIRMOS Deep Field, or VLA-VDF. In the same field, they already had multiband photometry down to I<sub>AB</sub> = 25, and spectroscopic observations were to be obtained during the VIRMOS VLT survey. The homogeneous sensitivity over the whole field allowed them to derive a complete sample of 1054 radio sources (5-sigma limit) down to a limit of 0.08 mJy. In their paper, the authors give a detailed description of the data reduction and of the analysis of the radio observations, with particular care to the effects of clean bias and bandwidth smearing, and of the methods used to obtain the catalog of radio sources. To estimate the effect of the resolution bias on their observations, they have modeled the effective angular-size distribution of the sources in their sample and they have used this distribution to simulate a sample of radio sources. Finally, they present the radio count distribution down to 0.08 mJy derived from the catalog. Their counts are in good agreement with the best fit derived from earlier surveys, and are about 50% higher than the counts in the Hubble Deep Field (HDF). The radio count distribution clearly shows, with extremely good statistics, the change in the slope for the sub-mJy radio sources. 19 of the 1054 radio sources were fitted with multiple components. In such cases, the authors list in the catalog an entry for each of the components, identified with a trailing letter (A, B, C or D) in the source name, and an entry for the whole source, identified with a trailing T in the source name. In these cases the total flux was calculated using the task TVSTAT, which allows the integration of the map values over irregular areas, and the sizes are the largest angular sizes. Thus, this catalog contains 1103 entries on 1054 sources, including 49 entries on individual components of composite sources. This table was created by the HEASARC in February 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/403/857">CDS Catalog J/A+A/403/857</a> file catalog.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/vvds20cm.html
bib_reference = 2003A&A...403..857B
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=vvds20cm&
tap_tablename = vvds20cm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744117
ID = nasa.heasarc/w2ragncat
publisher_did = ivo://nasa.heasarc/w2ragncat
obs_collection = W2RAGNCAT
obs_title = WISE/2MASS/RASS (W2R) AGN Sample Catalog
obs_description = The authors of this catalog have developed the S<sub>IX</sub> statistic to identify bright, highly likely active galactic nucleus (AGN) candidates solely on the basis of Wide-field Infrared Survey Explorer (WISE), Two-Micron All-Sky Survey (2MASS), and ROSAT All-Sky Survey (RASS) data. This statistic was optimized with data from the preliminary WISE survey and the Sloan Digital Sky Survey, and tested with Lick 3 m Kast spectroscopy. The authors find that sources with S<sub>IX</sub> < 0 have a >~ 95% likelihood of being an AGN (defined in this paper as a Seyfert 1, quasar, or blazar). This statistic was then applied to the full WISE/2MASS/RASS dataset, including the final WISE data release, to yield the "W2R" sample of 4316 sources with S<sub>IX</sub> < 0. Only 2209 of these sources are currently in the Veron-Cetty and Veron (VCV) Catalog of spectroscopically confirmed AGNs, indicating that the W2R sample contains nearly 2000 new, relatively bright (J <~ 16) AGNs. The authors utilize the W2R sample to quantify biases and incompleteness in the VCV Catalog. They find that it is highly complete for bright (J < 14), northern AGNs, but the completeness drops below 50% for fainter, southern samples and for sources near the Galactic plane. This approach also led to the spectroscopic identification of 10 new AGNs in the Kepler field, more than doubling the number of AGNs being monitored by Kepler. The W2R sample contains better than 1 bright AGN every 10 deg<sup>2</sup>, permitting construction of AGN samples in any sufficiently large region of sky. This table contains the 4316 sources comprising the W2R sample. This table was created by the HEASARC in June 2012 based on an electronic version of Table 3 from the reference paper which was obtained from the ApJ website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/w2ragncat.html
bib_reference = 2012ApJ...751...52E
obs_regime = infrared
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=w2ragncat&
tap_tablename = w2ragncat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744129
ID = nasa.heasarc/w40sfrcxo
publisher_did = ivo://nasa.heasarc/w40sfrcxo
obs_collection = W40SFRCXO
obs_title = W 40 Star-Forming Region Chandra X-Ray Point Source Catalog
obs_description = The young stellar cluster illuminating the W40 H II region, one of the nearest massive star-forming regions (SFRs), has been observed with the ACIS detector on board the Chandra X-ray Observatory. Due to its high obscuration, this is a poorly studied stellar cluster with only a handful of bright stars visible in the optical band, including three OB stars identified as primary excitation sources. The authors detect 225 X-ray sources, of which 85% are confidently identified as young stellar members of the region. Two potential distances of the cluster, 260 pc and 600 pc, are used in the paper. Supposing the X-ray luminosity function of SFRs to be universal, it supports a 600 pc distance as a lower limit for W40 and a total population of at least 600 stars down to 0.1 M<sub>sun</sub> under the assumption of a coeval population with a uniform obscuration. In fact, there is strong spatial variation in K<sub>s</sub>-band-excess disk fraction and non-uniform obscuration due to a dust lane that is identified in absorption in optical, infrared, and X-ray. The dust lane is likely part of a ring of material which includes the molecular core within W40. In contrast to the likely ongoing star formation in the dust lane, the molecular core is inactive. The star cluster has a spherical morphology, an isothermal sphere density profile, and mass segregation down to 1.5 M<sub>sun</sub>. However, other cluster properties, including a <= 1 Myr age estimate and ongoing star formation, indicate that the cluster is not dynamically relaxed. X-ray diffuse emission and a powerful flare from a young stellar object are also reported in the reference paper. This table was created by the HEASARC in March 2011 based on electronic versions of Tables, 1, 2 and 4 of the reference paper which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/w40sfrcxo.html
bib_reference = 2010ApJ...725.2485K
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=w40sfrcxo&
tap_tablename = w40sfrcxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744137
ID = nasa.heasarc/wackerling
publisher_did = ivo://nasa.heasarc/wackerling
obs_collection = Wackerling
obs_title = Wackerling Catalog of Early-Type Emission-Line Stars
obs_description = The Wackerling Catalog contains entries for 5326 early-type emission-line stars. Of these stars, 1424 have no spectral classification but are assumed to be of early type. Some 71 percent of the stars in this catalog can also be found in the Mount Wilson and the Mount Wilson-Michigan survey catalogs. The Wackerling Catalog contains numerous cross identifications to other designations (common name, HD, DM, LS, MWC, TON, HIL, WRA, HEN, etc.), rough spectroscopic types, magnitudes (visual and blue), and positions. The version of the Wackerling Catalog on which the HEASARC database is based was obtained from the ADC and differs in some respects from the original published version, notice. This online catalog was originally ingested by the HEASARC in July 1999, based on a machine-readable table obtained from the ADC/CDS data centers. It was updated in May 2020 to reflect updates to the spect_type_code values made by the CDS for improved database compatibility. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wackerling.html
bib_reference = 1970MmRAS..73..153W
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wackerling&
tap_tablename = wackerling
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744149
ID = nasa.heasarc/warps
publisher_did = ivo://nasa.heasarc/warps
obs_collection = ROSAT/WARPS
obs_title = Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)
obs_description = The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06<z<0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10<sup>-14</sup> erg/cm<sup>2</sup>/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. This online catalog was created by the HEASARC in May 2003 based on machine-readable versions of tables 2, 3, 4 and 5 of Perlman et al. (2002) that were obtained from the CDS. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/warps.html
bib_reference = 2002ApJS..140..265P
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=warps&
tap_tablename = warps
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744161
ID = nasa.heasarc/warps2
publisher_did = ivo://nasa.heasarc/warps2
obs_collection = WARPS2
obs_title = Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog
obs_description = This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg<sup>2</sup>. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z >= 0.3 (29 not previously reported in the literature) and 11 clusters with z >= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10<sup>-14</sup> ergs/cm<sup>2</sup>/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table. This table was created by the HEASARC in September 2010 based on the combination of the electronic versions of Tables 2, 3, and 4 from the first reference paper which were obtained from the CDS (their catalog J/ApJS/176/374). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/warps2.html
bib_reference = 2008ApJS..176..374H
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=warps2&
tap_tablename = warps2
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744177
ID = nasa.heasarc/wbhgp20cm
publisher_did = ivo://nasa.heasarc/wbhgp20cm
obs_collection = WBH20cmGP
obs_title = New Catalog of Compact 20cm Sources in the Galactic Plane
obs_description = This table contains the New Catalog of Compact Radio (20-cm) Sources in the Galactic Plane of White et al. (2005). Archival data were combined with more recent observations of the Galactic plane using the Very Large Array to create two new catalogs of compact centimetric radio sources. The 20-cm source catalog contained here covers a longitude range from -20 to +120 degrees in Galactic longitude l; the latitude coverage varies from b = +/- 0.8 to +/- 2.7 degrees. The total survey area is about 331 square degrees; coverage is 90% complete at a flux density threshold of about 14 mJy, and over 5000 sources are recorded. The 6-cm catalog (also available in the HEASARC Browse system as the table WBHGP6CM) covers 43 square degrees in the region -10 degrees < l <42 degrees, |b| < 0.4 degrees to a 90% completeness threshold of 2.9 mJy; over 2700 sources are found. Both surveys have an angular resolution of about 6". These catalogs provide a 30% (at 20 cm) to 50% (at 6 cm) increase in the number of high-reliability compact sources in the Galactic plane, as well as greatly improved astrometry, uniformity, and reliability; they should prove useful for comparison with new mid- and far-infrared surveys of the Milky Way. The images from which this catalog was constructed are available at the MAGPIS web site, <a href="http://third.ucllnl.org/gps">http://third.ucllnl.org/gps</a> This table was created by the HEASARC in July 2006 based on the combination of CDS tables J/AJ/130/586 table3.dat and table4.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wbhgp20cm.html
bib_reference = 2005AJ....130..586W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wbhgp20cm&
tap_tablename = wbhgp20cm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744189
ID = nasa.heasarc/wbhgp6cm
publisher_did = ivo://nasa.heasarc/wbhgp6cm
obs_collection = WBH6cmGP
obs_title = New Catalog of Compact 6cm Sources in the Galactic Plane
obs_description = This table contains the New Catalog of Compact Radio (6-cm) Sources in the Galactic Plane of White et al. (2005). Archival data were combined with more recent observations of the Galactic plane using the Very Large Array to create two new catalogs of compact centimetric radio sources. The 20-cm source catalog (available in the HEASARC Browse system as the table WBHGP20CM) covers a longitude range from -20 to +120 degrees in Galactic longitude l; the latitude coverage varies from b = +/- 0.8 to +/- 2.7 degrees. The total survey area is about 331 square degrees; coverage is 90% complete at a flux density threshold of about 14 mJy, and over 5000 sources are recorded. The 6-cm catalog described here covers 43 square degrees in the region -10 degrees < l <42 degrees, |b| < 0.4 degrees to a 90% completeness threshold of 2.9 mJy; over 2700 sources are found. Both surveys have an angular resolution of about 6". These catalogs provide a 30% (at 20 cm) to 50% (at 6 cm) increase in the number of high-reliability compact sources in the Galactic plane, as well as greatly improved astrometry, uniformity, and reliability; they should prove useful for comparison with new mid- and far-infrared surveys of the Milky Way. The images from which this catalog was constructed are available at the MAGPIS web site, <a href="http://third.ucllnl.org/gps">http://third.ucllnl.org/gps</a> This table was created by the HEASARC in July 2006 based on the combination of CDS tables J/AJ/130/586 table5.dat and table6.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wbhgp6cm.html
bib_reference = 2005AJ....130..586W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wbhgp6cm&
tap_tablename = wbhgp6cm
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744197
ID = nasa.heasarc/wbl
publisher_did = ivo://nasa.heasarc/wbl
obs_collection = WBL
obs_title = WBL Poor Galaxy Clusters Catalog (White et al. 1999)
obs_description = The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog. The WBL table was created by the HEASARC in July 2002 based on CDS Catalog J/AJ/118/2014 (the file table2.dat). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wbl.html
bib_reference = 1999AJ....118.2014W
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wbl&
tap_tablename = wbl
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744213
ID = nasa.heasarc/wblgalaxy
publisher_did = ivo://nasa.heasarc/wblgalaxy
obs_collection = WBL
obs_title = WBL Individual Galaxies Data Catalog (White et al. 1999)
obs_description = The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog). The WBLGALAXY table was created by the HEASARC in July 2002 based on CDS Catalog J/AJ/118/2014 (the file table3.dat). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wblgalaxy.html
bib_reference = 1999AJ....118.2014W
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wblgalaxy&
tap_tablename = wblgalaxy
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744221
ID = nasa.heasarc/wd1cxo
publisher_did = ivo://nasa.heasarc/wd1cxo
obs_collection = WD1CXO
obs_title = Westerlund 1 Chandra X-Ray Point Source Catalog
obs_description = The nature of the X-ray point source population within the young massive cluster Westerlund 1 (Wd 1) is investigated. Chandra X-ray Observatory (CXO) observations were used to determine the X-ray properties of emitters within Wd 1, while a comprehensive multi-wavelength dataset was employed to constrain their nature. Wd 1 (l=339.5, b=-0.4) was observed with the CXO Advanced CCD Spectrometer Spectroscopic array on 2005 May 22 for 18 ks (sequence 6283) and 2005 June 20 for 42 ks (sequence 5411). 241 sources were found above a sensitivity threshold that corresponded to a 10<sup>-6</sup> chance per PSF element of detecting a spurious source. X-ray emission from a multitude of different stellar sources within Wd 1, including both evolved high mass and low-mass pre-MS stars, is found. This table was created by the HEASARC in May 2008 based on CDS table J/A+A/477/147 files table1.dat and table3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wd1cxo.html
bib_reference = 2008A&A...477..147C
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wd1cxo&
tap_tablename = wd1cxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744237
ID = nasa.heasarc/wds
publisher_did = ivo://nasa.heasarc/wds
obs_collection = WDS
obs_title = Washington Double Star Catalog
obs_description = The Washington Double Star Catalog (WDS), maintained by the United States Naval Observatory (USNO), is the world's principal database of astrometric double and multiple star information. The WDS Catalog contains positions, discoverer designations, epochs, position angles, separations, magnitudes, spectral types, proper motions and when available, Durchmusterung numbers and notes for the components of close to 100,000 systems based on ~600,000 means. The current version at the HEASARC is updated weekly and is derived from the version available online at <a href="https://crf.usno.navy.mil/wds/">https://crf.usno.navy.mil/wds/</a> (and mirrored at <a href="http://www.astro.gsu.edu/wds/">http://www.astro.gsu.edu/wds/</a>), the latter being potentially updated nightly. The Washington Visual Double Star Catalog (WDS) is the successor to the Index Catalogue of Visual Double Stars, 1961.0 (IDS; Jeffers & van den Bos, 1963). Three earlier double star catalogs in the 20th century, those by Burnham (BDS; 1906), Innes (SDS; 1927), and Aitken (ADS; 1932), each covered only a portion of the sky. Both the IDS and the WDS cover the entire sky, and the WDS is intended to contain all known visual double stars for which at least one differential measure has been published. The WDS is continually updated as published data become available. Prior to this, two major updates have been published (Worley & Douglass 1984, 1997). The Washington Double Star Catalog (WDS) has seen numerous changes since the last major release of the catalog. The application of many techniques and considerable industry over the past few years has yielded unprecedented gains in both the number of systems and the number of measures. This version of the WDS catalog was first created at the HEASARC in March 2002 based on the USNO online version (available at either <a href="https://crf.usno.navy.mil/wds/">https://crf.usno.navy.mil/wds/</a> or <a href="http://www.astro.gsu.edu/wds/">http://www.astro.gsu.edu/wds/</a>), and is updated by the HEASARC on at least a weekly basis. The table schema was last revised in February 2005. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wds.html
bib_reference = 2001AJ....122.3466M
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wds&
tap_tablename = wds
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744249
ID = nasa.heasarc/wenss
publisher_did = ivo://nasa.heasarc/wenss
obs_collection = WENSS
obs_title = Westerbork Northern Sky Survey
obs_description = The Westerbork Northern Sky Survey (WENSS) is a low-frequency radio survey that covers the whole sky north of declination +30 degrees at a wavelength of 92 cm to a limiting flux density of approximately 18 milliJanskies (mJy) at the 5 sigma level. WENSS is a collaboration between the Netherlands Foundation for Research in Astronomy (NFRA/ASTRON) and the Leiden Observatory. The major personnel involved in WENSS include Ger de Bruyn, George Miley, Roeland Rengelink, Yuan Tang, Malcolm Bremer, Huub Rottgering, Ernst Raimond, Martin Bremer, and David Fullagar. The version of the WENSS Catalog as implemented at the HEASARC is a union of two separate catalogs obtained from the WENSS Website: the WENSS Polar Catalog (18186 sources above +72 degrees declination) and the WENSS Main Catalog (211234 sources in the declination region from +28 to +76 degrees). This database table was created by the HEASARC in February 2001 based on the tables wenssn10.cat (WENSS Main Catalog) and wenssp10.cat (WENSS Polar Catalog) obtained from the WENSS web site at <a href="http://www.strw.leidenuniv.nl/">http://www.strw.leidenuniv.nl/</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wenss.html
bib_reference = 1997A&AS..124..259R
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wenss&
tap_tablename = wenss
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744257
ID = nasa.heasarc/wfcpoint
publisher_did = ivo://nasa.heasarc/wfcpoint
obs_collection = ROSAT/WFC
obs_title = ROSAT Archival WFC EUV Data
obs_description = The WFCPOINT database table contains the list of ROSAT-Wide Field Camera calibration (CAL), performance verification (PV), and AO phase observations. For each observation listed in WFCPOINT, the target name, celestial co-ordinates, sequence number, PI name, and proposal title are given. The date of the observation, date that the data were distributed, and the date that the data will be released to the public are also given. The public release date is nominally 1 year and 14 days after the distribution date; however, because of some processing problems with a few datasets, the actual release date will be delayed from the given date. One duplicate entry was removed from the HEASARC implementation of this catalog in June 2019. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wfcpoint.html
obs_regime = euv
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wfcpoint&
tap_tablename = wfcpoint
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744269
ID = nasa.heasarc/wgacat
publisher_did = ivo://nasa.heasarc/wgacat
obs_collection = WGACAT
obs_title = ROSAT Catalog PSPC WGA Sources
obs_description = WGACAT is a point source catalog generated from all ROSAT PSPC pointed observations. This catalog has been generated by N.E. White (HEASARC/GSFC), P. Giommi (SDC/ASI) and L. Angelini (HEASARC/GSFC) and is a private research effort, not related to the official catalogs generated by the ROSAT project. The WGACAT was made first publicly available in November 1994 through the HEASARC on-line service (White, Giommi and Angelini 1994), with a first minor revision in March 1995 (WGACAT95 hereafter). It was generated using all the public ROSAT PSPC pointed data available than, corresponding to 75 % of the entire set, and featured ~ 68000 detections of which 62000 were unique sources. The current version, released in May 2000 (see also the update section), is the final and complete version of WGACAT and includes the remaining sequences not processed in the WGACAT95. WGACAT (May 2000) contains about 88,000 detections, with more than 84,000 individual sources, obtained from 4160 sequences. The catalog was generated using an optimized sliding cell detect algorithm in XIMAGE (first developed for the EXOSAT project). The inner and outer parts of the images were run separately, to maximize the sensitivity to source detection. This method is very sensitive in finding point sources, but can also find spurious sources where there is extended emission. We have visually inspected each detection, removed the obvious spurious cases and assigned a quality flag to each detection. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wgacat.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wgacat&
tap_tablename = wgacat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744277
ID = nasa.heasarc/wibrals
publisher_did = ivo://nasa.heasarc/wibrals
obs_collection = WIBRALS
obs_title = WISE Blazar-like Radio-Loud Source (WIBRaLS) Catalog
obs_description = This table contains a catalog of radio-loud candidate gamma-ray emitting blazars with WISE mid-infrared colors similar to the colors of confirmed gamma-ray blazars. The catalog is assembled from WISE sources detected in all four WISE filters, with colors that are compatible with the three-dimensional locus of the WISE gamma-ray emitting blazars, and which can be spatially cross-matched with radio sources from one of the three radio surveys: NVSS, FIRST, and/or SUMSS. The authors' initial WISE selection uses a slightly modified version of previously successful algorithms. They then select only the radio-loud sources using a measure of the radio-to-IR flux, the q<sub>22</sub> parameter, which is analogous to the q<sub>24</sub> parameter known in the literature but which instead uses the WISE band-four flux at 22 micron (um). Their final catalog contains 7,855 sources classified as BL Lacs, FSRQs, or mixed candidate blazars; 1,295 of these sources can be spatially re-associated as confirmed blazars. In their paper, the authors describe the properties of the final catalog of WISE blazar-like radio-loud sources and consider possible contaminants. Finally, they discuss why this large catalog of candidate gamma-ray emitting blazars represents a new and useful resource to address the problem of finding low-energy counterparts to currently unidentified high-energy sources. The WISE magnitudes in the [3.4], [4.6], [12] and [22] um nominal filters are in the Vega system. The values of three WISE magnitudes, namely [3.4], [4.6], and [12], and of the colors derived using those magnitudes, have been corrected for galactic extinction according to the extinction law presented by Draine (2003, ARA&A, 41, 241). In their study, the authors adopt the nomenclature proposed in the Multi-wavelength Blazar Catalog (BZCat) that labels BL Lac objects as 'BZBs' and flat-spectrum radio quasars (FSRQs) as 'BZQs'. This table was created by the HEASARC in December 2014 based on a machine-readable version of Table 4 from the reference paper that was obtained from the ApJS web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wibrals.html
bib_reference = 2014ApJS..215...14D
obs_regime = infrared
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wibrals&
tap_tablename = wibrals
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744289
ID = nasa.heasarc/wisehspcat
publisher_did = ivo://nasa.heasarc/wisehspcat
obs_collection = WISEHSPCAT
obs_title = 2WHSP Catalog of High Synchrotron Peaked Blazars and Candidates
obs_description = High Synchrotron Peaked blazars (HSPs) dominate the gamma-ray sky at energies larger than a few GeV, however only a few hundred blazars of this type have been catalogued so far. In this paper, the authors present the 2WHSP sample, the largest and most complete list of HSP blazars available to date, which is an expansion of the 1WHSP catalog (Arsioli et al. 2015, A&A, 579, A34) of gamma-ray source candidates away from the Galactic Plane. They cross-matched a number of multi-wavelength surveys (in the radio, infrared and X-ray bands) and applied selection criteria based on the radio to IR, and IR to X-ray spectral slopes. To ensure the selection of genuine HSPs, the authors examined the spectral energy distribution (SED) of each candidate and estimated the peak frequency of its synchrotron emission (nu<sub>peak</sub>) using the Agenzia Spaziale Italiana Science Data Center (ASDC) SED tool, including only sources with nu<sub>peak</sub> > 10<sup>15</sup> Hz (equivalent to nu<sub>peak</sub> > 4 eV). The authors have assembled the largest and most complete catalog of HSP blazars to date, which includes 1691 sources. A number of population properties, such as infrared colors, synchrotron peak, redshift distributions, and gamma-ray spectral properties, have been used to characterize the sample and maximize completeness. The authors also derived the radio log N - log S distribution. This catalog has already been used to provide seeds to discover new very high energy objects within Fermi-LAT data and to look for the counterparts of neutrino and ultra-high energy cosmic ray sources, showing its potential for the identification of promising high-energy gamma-ray sources and multi-messenger targets. This table comprises the 2WHSP catalog, a multi-frequency catalog of HSP. It contains 1691 sources, 288 of which are newly identified HSPs, 540 are previously known HSPs, 814 are HSP candidates, 45 are HSP blazars taken from the 2FHL catalog, and 4 from TeVCat (<a href="http://tevcat.uchicago.edu">http://tevcat.uchicago.edu</a>). This table was created by the HEASARC in February 2017 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/598/A17">CDS Catalog J/A+A/598/A17</a> file 2whsp.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wisehspcat.html
bib_reference = 2017A&A...598A..17C
obs_regime = gamma-ray
obs_regime = infrared
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wisehspcat&
tap_tablename = wisehspcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744297
ID = nasa.heasarc/wish
publisher_did = ivo://nasa.heasarc/wish
obs_collection = WISH
obs_title = Westerbork in the Southern Hemisphere (WISH) Source Catalog
obs_description = The Westerbork in the Southern Hemishpere (WISH) is a low-frequency (352 MHz) radio survey that covers most of the sky (the Galactic Plane region |b| < 10 degrees is excluded) between -26 and -9 degrees (1.60 sr) at a wavelength of 92 cm to a limiting flux density of approximately 18 mJy (5 sigma). WISH is the southern extension of the Westerbork Northern Sky Survey (WENSS). Due to the very low elevation of the observations, the survey has a much lower resolution in declination than in right ascension (54" x 54" cosec[delta]). A correlation with the 1.4GHz NVSS (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/65">CDS Cat. VIII/65</a>) shows that the positional accuracy is less constrained in declination than in right ascension, but there is no significant systematic error. This table contains 90,357 352-MHz flux density measurements, some of them being multiple observations of the same sources, some of them measurements of individual components of multi-component sources. While the abstract of the reference paper states that there are 73,570 sources in this catalog, the HEASARC counts 77,414 unique sources in this version of the table. The correlation with the NVSS was also used to construct a sample of faint Ultra Steep Spectrum sources (Table 2 in the reference paper, available at <a href="http://cdsarc.u-strasbg.fr/ftp/cats/VIII/69A/uss.dat.gz">http://cdsarc.u-strasbg.fr/ftp/cats/VIII/69A/uss.dat.gz</a>). This sample is aimed at increasing the number of known high redshift radio galaxies to allow detailed follow-up studies of these massive galaxies and their environments in the early Universe. WISH is a collaboration between the Netherlands Foundation for Research in Astronomy (NFRA/ASTRON) and the Leiden Observatory. Carlos De Breuck, Yuan Tang, Ger de Bruyn, Huub Rottgering, Wil van Breugel, and Roeland Rengelink. For more information, see the WENSS home page at <a href="http://www.astron.nl/wow/testcode.php?survey=1">http://www.astron.nl/wow/testcode.php?survey=1</a>. This table was created by the HEASARC in November 2010 base on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VIII/69A">CDS catalog VIII/69A</a> file wish11.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wish.html
bib_reference = 2002A&A...394...59D
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wish&
tap_tablename = wish
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744309
ID = nasa.heasarc/wmapcmbfps
publisher_did = ivo://nasa.heasarc/wmapcmbfps
obs_collection = WMAPCMBFPS
obs_title = WMAP Nine-Year CMB-Free QVW Point Source Catalog
obs_description = The Wilkinson Microwave Anisotropy Probe (WMAP) is designed to produce all-sky maps of the cosmic microwave background (CMB) anisotropy. The WMAP 9-Year CMB-Free Point Source Catalog contained herein has information on 502 point sources in three frequency bands (41, 61 and 94 GHz, also known as the Q, V, and W bands, respectively) based on data from the entire 9 years of the WMAP sky survey from 10 Aug 2001 0:00 UT to 10 Aug 2010 0:00 UT, inclusive. The CMB-free method of point source identification was originally applied to one-year and three-year V- and W-band maps by Chen & Wright (2008, ApJ, 681, 747) and to five-year V- and W-band maps by Wright et al. (2009, ApJS, 180, 283). The method used here is that applied to five-year Q-, V-, and W-band maps by Chen & Wright (2009, ApJ, 694, 222) and to seven-year Q-, V-, and W-band maps by Gold et al. (2011, ApJS, 192, 15). The V- and W-band maps are smoothed to Q-band resolution. An internal linear combination (ILC) map (see Section 5.3.3 of the reference paper) is then formed from the three maps using weights such that CMB fluctuations are removed, flat-spectrum point sources are retained with fluxes normalized to Q-band, and the variance of the ILC map is minimized. The ILC map is filtered to reduce noise and suppress large angular scale structure. Peaks in the filtered map that are > 5 sigma and outside of the nine-year point source catalog mask are identified as point sources, and source positions are obtained by fitting the beam profile plus a baseline to the filtered map for each source. For the nine- year analysis, the position of the brightest pixel is adopted instead of the fit position in rare instances where they differ by > 0.1 degrees. Source fluxes are estimated by integrating the Q, V, and W temperature maps within 1.25 degrees of each source position, with a weighting function to enhance the contrast of the point source relative to background fluctuations, and applying a correction for Eddington bias due to noise (sometimes called "deboosting"). The authors identify possible 5-GHz counterparts to the WMAP sources found by cross-correlating with the GB6 (Gregory et al. 1996, ApJS, 103, 427), PMN (Griffith et al. 1994, ApJS, 90, 179; Griffith et al. 1995, ApJS, 97, 347; Wright et al. 1994, ApJS, 94, 111; Wright et al. 1996, ApJS, 103, 145), Kuehr et al. (1981, A&AS, 45, 367), and Healey et al. (2009, AJ, 138, 1032) catalogs. A 5-GHz source is identified as a counterpart if it lies within 11 arcminutes of the WMAP source position (the mean WMAP source position uncertainty is 4 arcminutes). When two or more 5 GHz sources are within 11 arcminutes, the brightest is assumed to be the counterpart and a multiple identification flag is entered in the catalog. A separate 9-year Point Source Catalog (available in Browse as the <a href="/W3Browse/wmap/wmapptsrc.html">WMAPPTSRC</a> table) has information on 501 point sources in five frequency bands from 23 to 94 GHz that were found using an alternative method. The two catalogs have 387 sources in common. As noted by Gold et al. (2011, ApJS, 192, 15), differences in the source populations detected by the two search methods are largely caused by Eddington bias in the five-band source detections due to CMB fluctuations and noise. At low flux levels, the five-band method tends to detect point sources located on positive CMB fluctuations and to overestimate their fluxes, and it tends to miss sources located in negative CMB fluctuations. Other point source detection methods have been applied to WMAP data and have identified sources not found by our methods (e.g., Scodeller et al. (2012, ApJ, 753, 27); Lanz (2012, ADASS 7); Ramos et al. (2011, A&A, 528, A75), and references therein). For more details of how the point source catalogs were constructed, see Section 5.2.2 of the reference paper. This table was last updated by the HEASARC in January 2013 based on an electronic version of Table 19 from the reference paper which was obtained from the LAMBDA web site, the file <a href="http://lambda.gsfc.nasa.gov/data/map/dr5/dfp/ptsrc/wmap_ptsrc_catalog_cmb_free_9yr_v5.txt">http://lambda.gsfc.nasa.gov/data/map/dr5/dfp/ptsrc/wmap_ptsrc_catalog_cmb_free_9yr_v5.txt</a>. The source_flag values of 'M' in this file were changed to the 'a' values that were used in the printed version of this table. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wmapcmbfps.html
bib_reference = 2013ApJS..208...20B
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wmapcmbfps&
tap_tablename = wmapcmbfps
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
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TIMESTAMP = 1714845744317
ID = nasa.heasarc/wmapitnpts
publisher_did = ivo://nasa.heasarc/wmapitnpts
obs_collection = WMAPITNPTS
obs_title = WMAP 7-Year Internal Templates and Needlets New Source Catalog
obs_description = The authors have developed a new needlet-based method to detect point sources in cosmic microwave background (CMB) maps and have applied it to the Wilkinson Microwave Anisotropy Probe (WMAP) 7-year data. They use both the individual frequency channels as well as internal templates, the latter being the difference between pairs of frequency channels and hence having the advantage that the CMB component is eliminated. Using the area of the sky outside the Kq85 galactic mask, they detect a total of 2102 point sources at the 5-sigma level in either the frequency maps or the internal templates. Of these, 1116 are detected either at 5 sigma directly in the frequency channels or at 5 sigma in the internal templates and >= 3 sigma at the corresponding position in the frequency channels. Of the 1116 sources, 603 are detections that have not been reported so far in WMAP data. The authors have made a catalog of these sources available with position and flux estimated in the WMAP channels where they are seen. In total, they identified 1029 of the 1116 sources with counterparts at 5 GHz and 69 at other frequencies. This table was created by the HEASARC in July 2012 based on an electronic version of Table 6 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wmapitnpts.html
bib_reference = 2012ApJ...753...27S
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wmapitnpts&
tap_tablename = wmapitnpts
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744329
ID = nasa.heasarc/wmapptsrc
publisher_did = ivo://nasa.heasarc/wmapptsrc
obs_collection = WMAPPTSRC
obs_title = WMAP Nine-Year Five-Band Point Source Catalog
obs_description = The Wilkinson Microwave Anisotropy Probe (WMAP) is designed to produce all-sky maps of the cosmic microwave background (CMB) anisotropy. The WMAP 9-Year Point Source Catalog contained herein has information on point sources in five frequency bands from 23 to 94 GHz, based on data from the entire 9 years of the WMAP sky survey from 10 Aug 2001 0:00 UT to 10 Aug 2010 0:00 UT, inclusive. The 5-band search technique used in the first-year, 3-year, 5-year and 7-year analyses now finds 501 point sources, compared to 471 point sources found in the 7-year analysis and 390 sources found in the 5-year analysis. The 5-band search method is largely unchanged from the 7-year analysis (Gold et al. 2011, ApJS, 192, 15). This method searches for point sources in each of the five WMAP wavelength bands. The nine-year signal-to-noise ratio map in each band is filtered in harmonic space by b<sub>l</sub>/[(b<sub>l</sub>)<sup>2</sup> C<sub>l</sub>(cmb) + C<sub>l</sub>(noise)], where b<sub>l</sub> is the transfer function of the WMAP beam response, C<sub>l</sub>(cmb) is the CMB angular power spectrum, and C<sub>l</sub>(noise) is the noise power. The filtering suppresses CMB and Galactic foreground fluctuations relative to point sources. For each peak in the filtered maps that is > 5 sigma in any band, the unfiltered temperature map in each band is fit with the sum of a planar base level and a beam template formed by convolving an azimuthally symmetrized beam profile with a skymap pixel. (This method was previously used by Weiland et al. (2011, ApJS, 192, 19) for selected celestial calibration sources and is more accurate than the Gaussian fitting that was used for the seven-year and earlier point source analyses). The peak temperature from each beam template fit is converted to a source flux density using the conversion factor Gamma given in Table 3 of the reference paper. The flux density uncertainty is calculated from the 1-sigma uncertainty in the peak temperature, and does not include any additional uncertainty due to Eddington bias. Flux density values are entered into the catalog for bands where they exceed 2 sigma and where the source width from an initial Gaussian fit is within a factor of two of the beam width. A point source catalog mask is used to exclude sources in the Galactic plane and Magellanic cloud regions. This mask has changed from the seven-year analysis in accordance with changes in the KQ85 temperature analysis mask. A map pixel is outside of the nine-year point source catalog mask if it is either outside of the diffuse component of the nine-year KQ85 temperature analysis mask or outside of the seven-year point source catalog mask. The present mask admits 83% of the sky, compared to 82% and 78% for the previous 7-year and 5-year versions, respectively. The authors identify possible 5-GHz counterparts to the WMAP sources found by cross-correlating with the GB6 (Gregory et al. 1996, ApJS, 103, 427), PMN (Griffith et al. 1994, ApJS, 90, 179; Griffith et al. 1995, ApJS, 97, 347; Wright et al. 1994, ApJS, 94, 111; Wright et al. 1996, ApJS, 103, 145), Kuehr et al. (1981, A&AS, 45, 367), and Healey et al. (2009, AJ, 138, 1032) catalogs. A 5-GHz source is identified as a counterpart if it lies within 11 arcminutes of the WMAP source position (the mean WMAP source position uncertainty is 4 arcminutes). When two or more 5 GHz sources are within 11 arcminutes, the brightest is assumed to be the counterpart and a multiple identification flag is entered in the catalog. A separate 9-year CMB-free Point Source Catalog (available in Browse as the <a href="/W3Browse/wmap/wmapcmbfps.html">WMAPCMBFPS</a> table) has information on point sources in three frequency bands from 41 to 94 GHz: the CMB-free method identified 502 point sources in a linear combination map formed from 41, 61 and 94 GHz band maps using weights such that CMB fluctuations are removed and flat-spectrum point sources are retained. The two catalogs have 387 sources in common. As noted by Gold et al. (2011, ApJS, 192, 15), differences in the source populations detected by the two search methods are largely caused by Eddington bias in the five-band source detections due to CMB fluctuations and noise. At low flux levels, the five-band method tends to detect point sources located on positive CMB fluctuations and to overestimate their fluxes, and it tends to miss sources located in negative CMB fluctuations. Other point source detection methods have been applied to WMAP data and have identified sources not found by our methods (e.g., Scodeller et al. (2012, ApJ, 753, 27); Lanz (2012, ADASS 7); Ramos et al. (2011, A&A, 528, A75), and references therein). For more details of how the point source catalogs were constructed, see Section 5.2.2 of the reference paper. This table was last updated by the HEASARC in January 2012 based on an electronic version of Table 18 from the 2012 (ApJS, submitted) paper which was obtained from the LAMBDA web site, the file <a href="http://lambda.gsfc.nasa.gov/data/map/dr5/dfp/ptsrc/wmap_ptsrc_catalog_9yr_v5.txt">http://lambda.gsfc.nasa.gov/data/map/dr5/dfp/ptsrc/wmap_ptsrc_catalog_9yr_v5.txt</a>. The source_flag values were modified from those given in this file to reflect the values that were given in the printed version of the table. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wmapptsrc.html
bib_reference = 2013ApJS..208...20B
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wmapptsrc&
tap_tablename = wmapptsrc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744337
ID = nasa.heasarc/woodebcat
publisher_did = ivo://nasa.heasarc/woodebcat
obs_collection = Wood/Bin
obs_title = Wood Interacting Binaries Catalog
obs_description = This catalog, also called the Finding List (FL) of Interacting Binaries (5th edition), was abstracted from the Card Catalog maintained at the University of Florida which contains information on all published, and to the extent available, unpublished work on eclipsing binaries. The Card Catalog originated with Raymond Smith Dugan in the 1930's, who published from it the first edition of "A Finding List for Observers of Eclipsing Variables" (Dugan 1934, Princeton Univ. Obs. Contrib. No. 15). Successive editions of FL were subsequently published by Pierce (1947, Princeton Univ. Obs. Contrib. No. 22), by Wood (1953, Univ. Pennsylvania Astron. Series, Vol. VIII), by Koch et al. (1963, Univ. Pennsylvania Astron. Series, Vol. IX), and by Wood et al. (1980, Univ. Pennsylvania Astron. Series, Vol. XII). The FL was conceived as an aid to observers of eclipsing variables in selecting an observing program efficiently from the collection of all known data in an easy-to-use format. Although this format has changed over the years to meet existing requirements, the basic information content remains the same. The current edition differs from previous ones in the extension of the magnitude limit at minimum light from 13 to 15. In earlier editions, a binary system was not included unless the editors were reasonably certain that the system was indeed an eclipsing or (rarely) an ellipsoidal variable. The fifth edition includes all systems that the editors were fairly certain are either eclipsing or radiometrically variable binaries. The catalog fields are Finding List number; star name; position (given in the original catalog in equinox 1900); blue magnitude at maximum light; bandpass of maximum light; depth of primary minimum in same bandpass; bandpass primary minimum; depth of secondary minimum and its bandpass; spectral class of star eclipsed at primary light and optional uncertainty character; spectral class of star eclipsed at secondary light; most recent reliable epoch of primary minimum; most recent orbital period; duration of primary minimum; duration of totality of primary minimum; BD, CoD, CPD, and HD number; alternate designations of system; and codes indicating the nature of the system. This database was created by the HEASARC in December 1997 based on a computer readable version of the catalog that was obtained from the CDS (their catalog VI/44): a few additions were made by the HEASARC that are listed in the HEASARC_Changes section of the present document. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/woodebcat.html
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=woodebcat&
tap_tablename = woodebcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744349
ID = nasa.heasarc/woolley
publisher_did = ivo://nasa.heasarc/woolley
obs_collection = WOOLLEY
obs_title = Woolley Catalog of Stars within 25 Parsecs
obs_description = This catalog was constructed at the Royal Greenwich Observatory in order to enlarge the Gliese (1957, Mitt. Astron. Rechen-Inst., Ser. A, No. 8) compilation. It contains data on stars nearer than 25 pc that were not included in that version of Gliese's catalog, plus some additional information that had been published after 1957 on stars which were present in the 1957 version of the Gliese catalog. The electronic version contains essentially all information given in Table Ia of the published Woolley catalog, plus positional data, and most cross references to other catalogs given in Table IIa. The notes flags in Table Ia are not included because the notes are not machine-readable. Omitted from Table IIa are the finding-chart indicators (Lowell G numbers or notes references) and miscellaneous cross identifications to other names and catalog identifiers. Tables Ib and IIb, containing 21 systems originally included in Gliese's (1957) catalog but for which revised parallaxes have placed them farther than 25 pc are not included in the electronic version. Data in the electronic version include the Gliese number (newly added stars by Woolley have numbers beginning with 9001, but new parallaxes have removed 9419 and added 9849 and 9850 from the < 25 parsecs sample), component identifications for multiple systems, parallaxes, annual proper motions, radial velocities, (U,V,W) space velocities, box orbit parameters (omega, e, i), spectral types, UBV data, absolute visual magnitudes, positions, GCTP (General Catalogue of Trigonometric Stellar Parallaxes) and its Supplement (Jenkins 1952, 1963) names, HD, DM, GCRV (General Catalogue of Stellar Radial Velocities, Publ. Carnegie Inst., Washington, No. 601, Wilson 1953) and other catalog identifiers, BS (= HR) (Hoffleit 1964) numbers, and remarks codes for spectroscopic binaries (SB), doubles, variables, etc. Note that there is an entry in this catalog for the Sun, for which many fields, such as RA and Dec, have not been populated. This table was recreated by the HEASARC in December 2002 based on the 21-Jul-1997 version of the CDS Catalog V/32A. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/woolley.html
bib_reference = 1970ROAn....5....1W
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=woolley&
tap_tablename = woolley
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744357
ID = nasa.heasarc/wrcat
publisher_did = ivo://nasa.heasarc/wrcat
obs_collection = WR
obs_title = The VIIth Catalog of Galactic Wolf-Rayet Stars
obs_description = The VIIth Catalogue of Galactic Population I Wolf-Rayet (WR) Stars provides improved coordinates, spectral types, and bv photometry of known WR stars and adds 71 new stars compared to the VIth Catalog. This census of galactic WR stars has reached 227 stars (226 entries in this catalog), comprising 127 WN stars, 87 WC stars, 10 WN/WC stars, and 3 WO stars. This includes 15 WNL and 11 WCL stars within 30 pc of the Galactic Center. The catalog includes information on periodicity, binarity, terminal wind velocities, correlations with open clusters, OB associations, H I bubbles, H II regions, and ring nebulae, observed and dereddened narrow-band bv photometry, and distances, both heliocentric and galactocentric, and lists the references from which this information was obtained. This catalog was created by the HEASARC in April 2001, based on electronic versions of Tables 13, 14, 15, and 28 from the published paper containing the catalog which were directly supplied to the HEASARC by the author. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wrcat.html
bib_reference = 2001NewAR..45..135V
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wrcat&
tap_tablename = wrcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744369
ID = nasa.heasarc/wsrt20anep
publisher_did = ivo://nasa.heasarc/wsrt20anep
obs_collection = WSRT20ANEP
obs_title = AKARI NEP WSRT 20-cm Source Catalog
obs_description = The Westerbork Radio Synthesis Telescope (WSRT) has been used in 2004 to make a deep radio survey of an ~1.7 degree<sup>2</sup> field coinciding with the AKARI north ecliptic pole (NEP) deep field. The WSRT survey consisted of 10 pointings, mosaiced with enough overlap to maintain a similar sensitivity across the central region that reached as low as 21 microJanskies/beam (µJy/beam) at 1.4 GHz. The observations, data reduction and source count analysis are presented in the reference paper, along with a description of the overall scientific objectives. A catalog containing 462 sources detected with a resolution of 17.0 arcsecs by 15.5 arcsecs is presented. The differential source counts calculated from the WSRT data have been compared with those from the shallow VLA-NEP survey of Kollgaard et al. (1994, ApJS, 93, 145), and show a pronounced excess for sources fainter than ~1 mJy, consistent with the presence of a population of star-forming galaxies at sub-mJy flux levels. The AKARI NEP deep field is the focus of a major observing campaign conducted across the entire spectral region. The combination of these data sets, along with the deep nature of the radio observations will allow unique studies of a large range of topics including the redshift evolution of the luminosity function of radio sources, the clustering environment of radio galaxies, the nature of obscured radio-loud active galactic nuclei, and the radio/far-infrared correlation for distant galaxies. This catalog provides the basic data set for a future series of paper dealing with source identifications, morphologies, and the associated properties of the identified radio sources. This table was created by the HEASARC in March 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/517/A54">CDS catalog J/A+A/517/A54</a> file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wsrt20anep.html
bib_reference = 2010A&A...517A..54W
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wsrt20anep&
tap_tablename = wsrt20anep
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744377
ID = nasa.heasarc/wsrtgp
publisher_did = ivo://nasa.heasarc/wsrtgp
obs_collection = WSRTGP
obs_title = WSRT Galactic Plane Compact 327-MHz Source Catalog
obs_description = The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| < 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parametrized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity > 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis < 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct non-thermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at <a href="http://www.ras.ucalgary.ca/wsrt_survey.html">http://www.ras.ucalgary.ca/wsrt_survey.html</a> for the WSRTGP images available in JPEG, PostScript, and FITS formats. This table was created by the HEASARC in February 2012 based on CDS Catalog J/ApJS/107/239 file wsrt.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/wsrtgp.html
bib_reference = 1996ApJS..107..239T
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=wsrtgp&
tap_tablename = wsrtgp
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744389
ID = nasa.heasarc/xbootes
publisher_did = ivo://nasa.heasarc/xbootes
obs_collection = XBootes
obs_title = XBOOTES: NDWFS Bootes Field X-Ray Point Source Catalog
obs_description = The XBootes table contains the X-Ray point source catalog from a Chandra survey of the 9 square degrees Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). This XBootes survey consists of 126 separate contiguous ACIS-I observations each of approximately 5000 s in duration. These unique Chandra observations allowed the authors to search for large-scale structure and to calculate X-ray source statistics over a wide, contiguous field of view with arcsecond angular resolution and uniform coverage. Optical spectroscopic follow-up observations and the rich NDWFS data set will allow the authors to identify and classify these X-ray-selected sources. Using wavelet decomposition, they have detected 4642 point sources with n >= 2 counts. In order to keep their detections ~ 99% reliable, they have limited their list to sources with n >= 4 counts. For a 5000 s observation and assuming a canonical unabsorbed active galactic nucleus (AGN) type X-ray spectrum, a 4 count on-axis source corresponds to a flux of 4.7 x 10^-15 ergs cm^-2 s^-1 in the soft (0.5-2 keV) band, 1.5 x 10^-14 ergs cm^-2 s^-1 in the hard (2-7 keV) band, and 7.8 x 10^-15 ergs cm^-2 s^-1 in the full (0.5-7 keV) band. The full 0.5-7 keV band n >= 4 count list contained in this HEASARC table has 3293 point sources. In addition to the point sources, 43 extended sources (not included in this HEASARC table) have been detected, consistent with the depth of these observations and the number counts of clusters. Presented here in the X-ray point source catalog for the XBootes survey are the source positions, X-ray fluxes, hardness ratios, and their uncertainties, for the 3293 sources with >= 4 counts in the full band. This table was created by the HEASARC in February 2006 based on the machine-readable version of Table 3 in the above paper which was obtained from the electronic ApJ website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xbootes.html
bib_reference = 2005ApJS..161....9K
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xbootes&
tap_tablename = xbootes
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744397
ID = nasa.heasarc/xbootesoid
publisher_did = ivo://nasa.heasarc/xbootesoid
obs_collection = XBOOTESOID
obs_title = XBOOTES:NDWFSBootesFieldOptical&NearIRCounterparts
obs_description = The XBootes Survey is a 5 ks Chandra survey of the Bootes Field of the NOAO Deep Wide-Field Survey (NDWFS). This survey is unique in that it is the largest (9.3 square degrees) contiguous region imaged in X-ray with complementary deep optical and near-infrared (near-IR) observations. The authors present a catalog of the optical counterparts to the 3213 X-ray point sources detected in the XBootes survey. Using a Bayesian identification scheme, they successfully identified optical counterparts for 98% of the X-ray point sources. The optical colors suggest that the optically detected galaxies are a combination of z < 1 massive early-type galaxies and bluer star-forming galaxies whose optical AGN emission is faint or obscured, whereas the majority of the optically detected point sources are likely quasars over a large redshift range. This large-area, X-ray-bright, optically deep survey enables the authors to select a large subsample of sources (773) with high X-ray to optical flux ratios (f<sub>X</sub>/f<sub>o</sub> > 10). These objects are likely high-redshift and/or dust-obscured AGNs. These sources have generally harder X-ray spectra than sources with 0.1 < f<sub>X</sub>/f<sub>o</sub> < 10. Of the 73 X-ray sources with no optical counterpart in the NDWFS catalog, 47 are truly optically blank down to R ~ 25.5 (the average 50% completeness limit of the NDWFS R-band catalogs). These sources are also likely to be high-redshift and/or dust-obscured AGNs. The 9.3 square degrees region of sky chosen to match the area covered with the NDWFS was observed by ACIS-I on the Chandra X-Ray Observatory over a 2 week time interval in 2003 March and April. The data were taken in 126 separate pointings, each observed for ~ 5 ks. The CIAO 3.0.2 wavelet detection algorithm (wavdetect; Freeman et al. 2002) was used to detect X-ray sources in the total (0.5 - 7.0 keV) band data. A probability threshold of 5 x 10-5 was chosen as the best compromise between maximizing the completeness while minimizing the number of spurious detections. The X-ray catalog comprises 3293 unique X-ray sources with >= 4 counts in the total-band images (Paper II). The authors expect only ~ 35 of these sources to be spurious in the full survey (Paper II). For the matching with cataloged optical counterparts, the authors only considered the 3213 X-ray sources that overlap with the NDWFS area. The authors include all multiply matched sources with >1% probability of being the correct optical counterpart. This table contains the X-ray and optical characteristics of the matched optical/X-ray catalog for the Chandra sources in the XBootes and NDWFS survey, and is Version 1.0, dated 21st June 2005. This table was created in November 2006 by the HEASARC based on the file xbootes_cat_xray_opt_IR_21jun_v1.0.txt obtained from the NOAO ftp area <a href="https://www.noao.edu/noao/noaodeep/XBootesPublic/">https://www.noao.edu/noao/noaodeep/XBootesPublic/</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xbootesoid.html
bib_reference = 2006ApJ...641..140B
obs_regime = infrared
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xbootesoid&
tap_tablename = xbootesoid
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744409
ID = nasa.heasarc/xcopraw
publisher_did = ivo://nasa.heasarc/xcopraw
obs_collection = Copern.X
obs_title = Copernicus X-Ray Observations
obs_description = Copernicus was the third satellite in the OAO program. It was launched the 21 august of 1972 and operated till 1981. The main instrument was an ultraviolet telescope with a spectrometer to measure interstellar absorption lines in the spectra of stellar objects. However it carried also an X-ray experiment provided by University College of London/MSSL consisted in 4 co-aligned experiments sensitive in the 1-10 keV energy range. This database accesses the raw FITS file containing data obtained from the UCL X-ray Experiment (UCLXE) package on board Copernicus. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xcopraw.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xcopraw&
tap_tablename = xcopraw
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744417
ID = nasa.heasarc/xcs
publisher_did = ivo://nasa.heasarc/xcs
obs_collection = XCS
obs_title = XMM-Newton Cluster Survey Catalog, DR1 Version
obs_description = The XMM Cluster Survey (XCS) is a serendipitous search for galaxy clusters using all publicly available data in the XMM-Newton Science Archive. Its main aims are to measure cosmological parameters and trace the evolution of X-ray scaling relations. In their paper, the authors present the first data release from the XMM Cluster Survey (XCS-DR1). This consists of 503 optically confirmed, serendipitously detected, X-ray clusters. Of these clusters, 256 are new to the literature and 357 are new X-ray discoveries. They present 463 clusters with a redshift estimate (0.06 < z < 1.46), including 261 clusters with spectroscopic redshifts. The remainder have photometric redshifts. In addition, the authors have measured X-ray temperatures (kT<sub>X</sub>) for 401 clusters (0.4 < kT<sub>X</sub> < 14.7 keV). This table was created by the HEASARC in May 2013 based on CDS Catalog J/MNRAS/423/1024 file xcsdr1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xcs.html
bib_reference = 2012MNRAS.423.1024M
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xcs&
tap_tablename = xcs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744429
ID = nasa.heasarc/xdeep2
publisher_did = ivo://nasa.heasarc/xdeep2
obs_collection = XDEEP2
obs_title = DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog
obs_description = This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg<sup>2</sup> DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg<sup>2</sup> fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (<~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10<sup>-16</sup> erg cm<sup>-1</sup> s<sup>-1</sup>. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10<sup>-14</sup> erg cm<sup>-1</sup> s<sup>-1</sup>), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R<sub>AB</sub> < 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a <~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog. This table was created by the HEASARC in October 2012 based on electronic versions of Tables 5 and 7 from the reference paper which were obtained from the ApJS web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xdeep2.html
bib_reference = 2012ApJS..202....6G
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xdeep2&
tap_tablename = xdeep2
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744437
ID = nasa.heasarc/xmdsvvds4s
publisher_did = ivo://nasa.heasarc/xmdsvvds4s
obs_collection = XMM/VIRMOS
obs_title = XMM-Newton Medium Deep Survey/VIRMOS VLT Deep Survey 4-Sigma Catalog
obs_description = The XMM-Newton Medium Deep Survey/VIRMOS VLT Deep Survey (XMDS/VVDS) 4-Sigma Catalog contains 286 X-ray sources with their optical identification taken from the XMDS survey (using the XMM-Newton EPIC instrument). It is the first catalog of X-ray sources resulting from the central area of the XMM-LSS (Large-Scale Structure Survey). This first version is limited to sources detected at 4{sigma} at least in one energy band, AND falling in the 1 square degree area covered by the optical photometric VVDS survey, which allowed the authors to provide optical and radio identifications. This table was created by the HEASARC in August 2005 based on CDS table J/A+A/439/413/xmds1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmdsvvds4s.html
bib_reference = 2005A&A...439..413C
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmdsvvds4s&
tap_tablename = xmdsvvds4s
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744449
ID = nasa.heasarc/xmmao
publisher_did = ivo://nasa.heasarc/xmmao
obs_collection = XMMAO
obs_title = XMM-Newton Accepted Targets
obs_description = This database table contains the current target list of the X-ray Multi-Mirror Newton (XMM-Newton) mission including those in (i) the routine calibration plan, (ii) the Guaranteed Time Observation (GTO) program, (iii) the triggered target candidates or ToOs accepted for the First through the Twentieth-Third Announcements of Opportunity (AO-1 through AO-23) programs, (iv) the AO-1 through AO-23 Guest Observer (GO) program targets with priority A or B, (v) the AO-1 through AO-19 GO program targets with priority C which have been observed, (vi) the AO-20 through AO-23 GO program targets with priority C, and (vii) the targets granted by agreement of the ESA Director of Science and the National Space Agency of Japan, following the loss of the original Astro-E spacecraft. For complete and authoritative information on the XMM-Newton mission, policies, and data archive, refer to the web pages of the European Space Agency's (ESA's) XMM-Newton Science Operations Center at <a href="http://xmm.esac.esa.int/">http://xmm.esac.esa.int/</a> and of NASA's XMM-Newton Guest Observer Facility at <a href="http://heasarc.gsfc.nasa.gov/docs/xmm/xmmgof.html">http://heasarc.gsfc.nasa.gov/docs/xmm/xmmgof.html</a> Notice that all priority C targets from AOs 1 through 19 which were never observed by XMM-Newton (and hence have expired) have been removed from this table. To check which targets have either already been observed by XMM-Newton or are on the short-term schedule to be observed in the next few weeks, users should examine the <a href="/db-perl/W3Browse/w3table.pl?tablehead=name%3Dxmmmaster&Action=More+Options">XMMMASTER</a> table which is also contained in Browse. To find out which targets are currently scheduled to be observed in the next three months, the user should check the XMM-Newton Advanced Plan at <a href="http://xmm.esac.esa.int/external/xmm_sched/advance_plan.shtml">http://xmm.esac.esa.int/external/xmm_sched/advance_plan.shtml</a> While abstracts are available for most proposals, there are a number of targets for which the HEASARC lacks the corresponding abstracts: e.g., the abstracts for AO-2 Guest Observer targets which have non-US PIs are not available. This database table was last updated by the HEASARC in December 2023, when AO-23's accepted targets were added. <p> AO-22's accepted targets were added in November 2022. <p> AO-21's accepted targets were added and AO-19's unobserved priority C targets were removed in December 2021. <p> AO-20's accepted targets were added and AO-18's unobserved priority C targets were removed in December 2020. <p> AO-19's accepted targets were added and AO-17's unobserved priority C targets were removed in April 2020. <p> In June 2019, many duplicate entries were removed. <p> AO-18's accepted targets were added and AO-16's unobserved priority C targets were removed in November 2018. <p> AO-17's accepted targets were added and AO-15's unobserved priority C targets were removed in November 2017. <p> AO-16's accepted targets were added and AO-14's unobserved priority C targets were removed in December 2016. <p> AO-15's accepted targets were added and AO-13's unobserved priority C targets were removed in December 2015. <p> In August 2015, proposal titles were added. <p> AO-14's accepted targets were added and AO-12's unobserved priority C targets were removed in December 2014. <p> AO-13's accepted targets were added and AO-11's unobserved priority C targets were removed in December 2013. <p> AO-12's accepted targets were added and AO-10's unobserved priority C targets were removed in December 2012. <p> AO-11's accepted targets were added and AO-9's unobserved priority C targets were removed in December 2011. <p> AO-10's accepted targets were added and AO-8's unobserved priority C targets were removed in December 2010. <p> AO-9's accepted targets were added and AO-7's unobserved priority C targets were removed in January 2010. <p> AO-8's accepted targets were added and AO-6's unobserved priority C targets were removed in December 2008. <p> AO-7's accepted targets were added and AO-5's unobserved priority C targets were removed in January 2008. <p> AO-6's accepted targets were added in January 2007, and, in November 2006, an effort was made to remove most of the unobserved priority C targets from previous AOs. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmao.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmao&
tap_tablename = xmmao
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744457
ID = nasa.heasarc/xmmatlas
publisher_did = ivo://nasa.heasarc/xmmatlas
obs_collection = XMMATLAS
obs_title = XMM-Newton Survey Catalog in the Herschel-ATLAS Field
obs_description = Wide area X-ray and far-infrared surveys are a fundamental tool to investigate the link between AGN growth and star formation, especially in the low-redshift universe (z < 1). The Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) has covered 550 deg<sup>2</sup> in five far-infrared and sub-mm bands, 16 deg<sup>2</sup> of which have been presented in the Science Demonstration Phase (SDP) catalogue. The reference paper cited below introduces the XMM-Newton observations in the H-ATLAS SDP area, covering 7.1 deg<sup>2</sup> with flux limits of 2 x 10<sup>-15</sup>, 6 x 10<sup>-15</sup>, and 9 x 10<sup>-15</sup> erg/s/cm<sup>2</sup> in the 0.5-2, 0.5-8 and 2-8keV bands, respectively. The paper presents the source detection techniques and the "main" catalog, which includes 1700, 1582 and 814 sources detected by EMLDetect in the 0.5-8, 0.5-2 and 2-8keV bands, respectively; the number of unique sources is 1816. The authors extract spectra and derive fluxes from power-law fits for 398 sources with more than 40 counts in the 0.5-8 keV band. They compare the best-fit fluxes with those in the catalog, which were obtained assuming a common photon index Gamma of 1.7; the authors find no bulk difference between the fluxes, and a moderate dispersion s of 0.33 dex. Using wherever possible the fluxes from the spectral fits, the authors derive the 2-10 keV Log N-Log S distribution, which is consistent with a Euclidean distribution. Finally, they release the computer code for the tools which they developed for this project. Sources were detected with a two-stage process. With the first pass at low significance, the authors got a list of candidate detections; and on the second pass they raised the significance threshold and derived accurate source parameters. Between the two passes, and because the second pass needs an input catalog, they identified the sources detected in more than one band. In the first pass, the SAS wavelet detection program ewavelet was run separately on each of the 0.5-2, 2-8 and 0.5-8 keV images of the entire mosaic, with a significance threshold of 4 sigma and the default wavelet scales (minimum 2 pixels, maximum 8 pixels, with a pixel size of 4). All parameters in this catalog which were derived from ewavelet have been given a prefix of 'wav' in this HEASARC representation so as to distinguish them from the parameters derived using EMLDetect. In the second pass, the authors used the SAS EMLDetect program to validate the detections, refine the coordinates and obtain maximum-likelihood estimates of the source counts, count rates and fluxes. The EMLDetect minimum likelihood was set at L = 4.6, as in Ranalli et al. (2013, A&A, 555, A42), which corresponds to a false-detection probability of 1.01 x 10<sup>-2</sup>. Together with the 4-sigma threshold for ewavelet, for the final catalog this yields a joint significance between 4 sigma and 5 sigma, but which cannot be further constrained without simulations. This table contains the X-ray sources which were detected in the 7.1 deg<sup>2</sup> XMM-Newton observations of the H-ATLAS field. The 1816 sources which were detected by both programs were presented in the main table in the reference paper (and are included in this HEASARC table where they are indicated by a value of the source_sample parameter of 'main'), while the 234 sources which were only detected by ewavelet were presented in the supplementary table in the reference paper (and are included in this HEASARC table where they are indicated by a value of the source_sample parameter of 'supp'). The same parameters were present in both the main and supplementary tables in the reference paper, but those parameters which came from EMLDetect are empty for the sources in the supplementary table. The parameters obtained using ewavelet (those parameters with the 'wav' prefix in their names) containing the source properties (counts, count rates, fluxes, exposure times, background, wavelet detection scale and source extent), while reported in this table for all sources, are actually only interesting for supplementary sources, according to the authors. This table was created by the HEASARC in May 2015 based on the union of <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/577/A121">CDS Catalog J/A+A/577/A121</a> files main.dat (which contain 1816 sources detected by both detection algorithms) and suppl.dat (which contains 234 'supplementary' sources detected only by the wavelet detection algorithm ewavelet). It thus contains a total of 2050 sources. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmatlas.html
bib_reference = 2015A&A...577A.121R
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmatlas&
tap_tablename = xmmatlas
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744469
ID = nasa.heasarc/xmmbss
publisher_did = ivo://nasa.heasarc/xmmbss
obs_collection = XMMBSS
obs_title = XMM-Newton Bright Serendipitous Survey
obs_description = We present here the XMM-Newton Bright Serendipitous Survey, composed of two flux-limited samples: the XMM-Newton Bright Source Sample (BSS, hereafter) and the XMM-Newton "Hard" Bright Source Sample (HBSS, hereafter). The selection criteria for these two sample, 0.5 - 4.5 keV count rate >= 0.01 ct/s (BSS) and 4.5 - 7.5 keV count rate >= 0.002 ct/s (HBSS), correspond to a flux limit of f<sub>X</sub> ~ 7 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s in the 0.5 - 4.5 keV and 4.5 - 7.5 keV energy bands, respectively, for sources with power-law spectra with energy spectral indices between 0.7 and 0.8. This table contains the basic data on a complete sample of 400 X-ray sources (389 of them belong to the BSS, 67 to the HBSS, with 56 X-ray sources in common) derived from the analysis of 237 suitable XMM-Newton fields (211 for the HBSS). At the flux limit of the survey, it covers a survey area of 28.10 (25.17 for the HBSS) square degrees. The extragalactic number-flux relationships (in the 0.5 - 4.5 keV and in the 4.5 - 7.5 keV energy bands) are in good agreement with previous and new results making the authors confident in the correctness of the data selection and their analysis. This table was created by the HEASARC in October 2006 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/428/383">CDS Catalog J/A+A/428/383</a> (the merger of files table3.dat and table4.dat). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmbss.html
bib_reference = 2004A&A...428..383D
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmbss&
tap_tablename = xmmbss
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744481
ID = nasa.heasarc/xmmbssagn
publisher_did = ivo://nasa.heasarc/xmmbssagn
obs_collection = XMMBSSAGN
obs_title = XMM-Newton Bright Serendipitous Survey: AGN X-Ray Spectral Properties
obs_description = X-ray surveys are a key instrument in the study of active galactic nuclei (AGN). Thanks to their penetrating ability, X-rays are able to map the innermost regions close to the central super massive black hole (SMBH) as well as to detect and characterize its emission up to high redshift. This table contains results from a detailed X-ray spectral analysis of the AGN belonging to the XMM-Newton Bright Serendipitous Survey (XBS, the HEASARC Browse XMMBSS table, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/IX/41">CDS Cat. IX/41</a>). The XBS is composed of two flux-limited samples selected in the complementary 0.5 to 4.5 and 4.5 to 7.5 keV energy bands and comprising more than 300 AGN up to redshift ~2.4. The authors have performed an X-ray analysis following two different approaches: by analyzing individually each AGN X-ray spectrum and by constructing average spectra for different AGN types. From the individual analysis, the authors find that there seems to be an anticorrelation between the spectral index and the sources' hard X-ray luminosity, such that the average photon index for the higher luminosity sources (>10<sup>44</sup> erg s<sup>-1</sup>) is significantly (>2 sigma) flatter than the average for the lower luminosity sources. They also find that the intrinsic column density distribution agrees with AGN unified schemes, although a number of exceptions are found (3% of the whole sample), which are much more common among optically classified type 2 AGN. The authors also find that the so-called "soft-excess", apart from the intrinsic absorption, constitutes the principal deviation from a power-law shape in AGN X-ray spectra and it clearly displays different characteristics, and likely a different origin, for unabsorbed and absorbed AGN. Regarding the shape of the average spectra, they find that it is best reproduced by a combination of an unabsorbed (absorbed) power law, a narrow Fe K-alpha emission line and a small (large) amount of reflection for unabsorbed (absorbed) sources. This table was created by the HEASARC in November 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/530/A42">CDS Catalog J/A+A/530/A42</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmbssagn.html
bib_reference = 2011A&A...530A..42C
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmbssagn&
tap_tablename = xmmbssagn
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744489
ID = nasa.heasarc/xmmcdfs210
publisher_did = ivo://nasa.heasarc/xmmcdfs210
obs_collection = XMMCDFS210
obs_title = XMM-Newton Deep Survey in the CDF-S 2-10 keV Source Catalog
obs_description = Nuclear obscuration plays a key role in the initial phases of AGN growth, yet not many highly obscured AGN are currently known beyond the local Universe, and their search is an active topic of research. The XMM-Newton survey in the Chandra Deep Field South (XMM-CDFS) aims at detecting and studying the spectral properties of a significant number of obscured and Compton-thick (N<sub>H</sub> >= 10<sup>24</sup> cm<sup>-2</sup>) AGN. The large effective area of XMM-Newton in the 2-10 and 5-10 keV bands, coupled with a 3.45-Ms nominal exposure time (2.82 and 2.45 Ms after lightcurve cleaning for MOS and PN respectively), allows the authors to build clean samples in both bands, and makes the XMM-CDFS the deepest XMM-Newton survey currently published in the 5-10 keV band. The large multi-wavelength and spectroscopic coverage of the CDFS area allows for an immediate and abundant scientific return. In this paper, the authors present the data reduction of the XMM-CDFS observations, the method for source detection in the 2-10 and 5-10 keV bands, and the resulting catalogs. A number of 339 and 137 sources are listed in the above bands with flux limits of 6.6 x 10<sup>-16</sup> and 9.5 x 10<sup>-16</sup> erg/s/cm<sup>2</sup>, respectively. The flux limits at 50% of the maximum sky coverage are 1.8 x 10<sup>-15</sup> and 4.0 x 10<sup>-15</sup> erg/s/cm<sup>2</sup>, respectively. The catalogs have been cross-correlated with the Chandra ones: 315 and 130 identifications have been found with a likelihood-ratio method, respectively. 15 new sources, previously undetected by Chandra, have been found; 5 of them lie in the 4-Ms area. Redshifts, either spectroscopic or photometric, are available for ~92% of the sources. The number counts in both bands are presented and compared to other works. The survey coverage has been calculated with the help of two extensive sets of simulations, one set per band. The simulations have been produced with a newly-developed simulator, written with the aim of the most careful reproduction of the background spatial properties. For this reason, the authors present a detailed decomposition of the XMM-Newton background into its components: cosmic, particle, and residual soft protons. The three components have different spatial distributions. The importance of these three components depends on the band and on the camera; the particle background is the most important one (80-90% of the background counts), followed by the soft protons (4-20%). X-ray sources were detected in the 3-Ms XMM-Newton observations of the Chandra Deep Field South. Source detection was done in two steps, first using the PWXDetect software, and then using emldetect. 339 Sources detected by both programs are presented in the main tables, while 74 sources only detected by PWXDetect are presented in the supplementary tables. The 2-10 and 5-10 keV bands were analyzed separately. This HEASARC table contains the main sample of 339 sources detected in the 2-10 keV band in the XMM-CDFS survey. (The table of 5-10 keV XMM-CDFS sources is also available at the HEASARC as the XMMCDFS510 table). This table does not include the 74 supplementary sources which were detected only with PWXDetect. These supplementary sources were on average detected at low significance; many of them were on the borders of the FOV; and a few were in crowded fields where EMLDetect had trouble separating the different PSF components. Nevertheless, 4 of these sources were bright enough that a spectrum could be extracted. This table was created by the HEASARC in September 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/555/A42">CDS Catalog J/A+A/555/A42</a> files main210.dat and notes210.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcdfs210.html
bib_reference = 2013A&A...555A..42R
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcdfs210&
tap_tablename = xmmcdfs210
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744501
ID = nasa.heasarc/xmmcdfs510
publisher_did = ivo://nasa.heasarc/xmmcdfs510
obs_collection = XMMCDFS510
obs_title = XMM-Newton Deep Survey in the CDF-S 5-10 keV Source Catalog
obs_description = Nuclear obscuration plays a key role in the initial phases of AGN growth, yet not many highly obscured AGN are currently known beyond the local Universe, and their search is an active topic of research. The XMM-Newton survey in the Chandra Deep Field South (XMM-CDFS) aims at detecting and studying the spectral properties of a significant number of obscured and Compton-thick (N<sub>H</sub> >= 10<sup>24</sup> cm<sup>-2</sup>) AGN. The large effective area of XMM-Newton in the 2-10 and 5-10 keV bands, coupled with a 3.45-Ms nominal exposure time (2.82 and 2.45 Ms after lightcurve cleaning for MOS and PN, respectively), allows the authors to build clean samples in both bands, and makes the XMM-CDFS the deepest XMM-Newton survey currently published in the 5-10 keV band. The large multi-wavelength and spectroscopic coverage of the CDFS area allows for an immediate and abundant scientific return. In this paper, the authors present the data reduction of the XMM-CDFS observations, the method for source detection in the 2-10 and 5-10 keV bands, and the resulting catalogs. A number of 339 and 137 sources are listed in the above bands with flux limits of 6.6 x 10<sup>-16</sup> and 9.5 x 10<sup>-16</sup> erg/s/cm<sup>2</sup>, respectively. The flux limits at 50% of the maximum sky coverage are 1.8 x 10<sup>-15</sup> and 4.0 x 10<sup>-15</sup> erg/s/cm<sup>2</sup>, respectively. The catalogs have been cross-correlated with the Chandra ones: 315 and 130 identifications have been found with a likelihood-ratio method, respectively. 15 new sources, previously undetected by Chandra, have been found; 5 of them lie in the 4-Ms area. Redshifts, either spectroscopic or photometric, are available for ~92% of the sources. The number counts in both bands are presented and compared to other works. The survey coverage has been calculated with the help of two extensive sets of simulations, one set per band. The simulations have been produced with a newly-developed simulator, written with the aim of the most careful reproduction of the background spatial properties. For this reason, the authors present a detailed decomposition of the XMM-Newton background into its components: cosmic, particle, and residual soft protons. The three components have different spatial distributions. The importance of these three components depends on the band and on the camera; the particle background is the most important one (80-90% of the background counts), followed by the soft protons (4-20%). X-ray sources were detected in the 3-Ms XMM-Newton observations of the Chandra Deep Field South. Source detection was done in two steps, first using the PWXDetect software, and then using emldetect. 137 Sources detected in the 5-10 keV band by both programs are presented in the main table, while 61 5-10 keV sources only detected by PWXDetect are presented in the supplementary table. The 2-10 and 5-10 keV bands were analyzed separately. This HEASARC table contains the main sample of 137 sources detected in the 5-10 keV band in the XMM-CDFS survey. (The table of 2-10 keV XMM-CDFS sources is also available at the HEASARC as the XMMCDFS210 table.) This table does not include the 61 supplementary sources which were detected only with PWXDetect. These supplementary sources were on average detected at low significance; many of them were on the borders of the FOV; and a few were in crowded fields where EMLDetect had trouble separating the different PSF components. Nevertheless, 4 of these sources were bright enough that a spectrum could be extracted. This table was created by the HEASARC in September 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/555/A42">CDS Catalog J/A+A/555/A42</a> files main510.dat and notes510.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcdfs510.html
bib_reference = 2013A&A...555A..42R
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcdfs510&
tap_tablename = xmmcdfs510
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744509
ID = nasa.heasarc/xmmcfrscat
publisher_did = ivo://nasa.heasarc/xmmcfrscat
obs_collection = XMM/CFRS
obs_title = XMM-Newton/Canada-France Redshift Survey Fields X-Ray Sources
obs_description = This table contains the X-ray source catalogs for the XMM-Newton surveys of the 3 and 14 hours Right Ascension (hereafter 3-h and 14-h, respectively) fields from the Canada-France Redshift Survey. (These fields are also known as the Groth Strip). The X-ray sources cover the 0.5-10 keV flux range from ~2 x 10^-15 - 10^-13 erg/cm^2^/s. The authors have used a subset of the XMM-Newton sources, which have Chandra positions, to determine the best method of obtaining optical identifications of sources with only XMM-Newton positions. They have found optical identifications for 79% of the XMM-Newton sources for which there were deep optical images. The sources without optical identifications are likely to be optically fainter and have higher redshifts than the sources with identifications. The authors have estimated 'photometric redshifts' for the identified sources, calibrating their method using ~200 galaxies in the fields with spectroscopic redshifts. They find that the redshift distribution has a strong peak at z~0.7. This table was created by the HEASARC in July 2005 based on CDS table J/MNRAS/350/785/tablea12.dat (the merged Tables A1 and A2 from the published paper). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcfrscat.html
bib_reference = 2004MNRAS.350..785W
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcfrscat&
tap_tablename = xmmcfrscat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744521
ID = nasa.heasarc/xmmcfrsoid
publisher_did = ivo://nasa.heasarc/xmmcfrsoid
obs_collection = XMM/CFRSID
obs_title = XMM-Newton/Canada-France Redshift Survey Fields Optical Identifications
obs_description = This table contains the proposed identifications for all the good optical ID candidates (true probability value P' that the object is not associated of < 0.15) corresponding to the X-ray sources from the XMM-Newton surveys of the 3 and 14 hours Right Ascension (hereafter 3-h and 14-h, respectively) fields from the Canada-France Redshift Survey. (These fields are also known as the Groth Strip). The X-ray sources cover the 0.5 - 10 keV flux range from ~2 x 10^-15 - 10^-13 erg/cm^2^/s. The authors have used a subset of the XMM-Newton sources, which have Chandra positions, to determine the best method of obtaining optical identifications of sources with only XMM-Newton positions. They found optical identifications for 79% of the XMM-Newton sources for which there were deep optical images. The sources without optical identifications are likely to be optically fainter and have higher redshifts than the sources with identifications. The authors have estimated 'photometric redshifts' for the identified sources, calibrating their method using ~200 galaxies in the fields with spectroscopic redshifts. They find that the redshift distribution has a strong peak at z ~ 0.7. This table was created by the HEASARC in July 2005 based on the combination of CDS table J/MNRAS/350/785/tablea34.dat (the merged Tables A3 and A4 from the published paper) and CDS table J/MNRAS/350/785/tablea56.dat (the merged Tables A5 and A6 from the published paper). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcfrsoid.html
bib_reference = 2004MNRAS.350..785W
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcfrsoid&
tap_tablename = xmmcfrsoid
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744529
ID = nasa.heasarc/xmmcosmagn
publisher_did = ivo://nasa.heasarc/xmmcosmagn
obs_collection = XMMCOSMAGN
obs_title = XMM-COSMOS Catalog of X-Ray Selected Type 1 AGN
obs_description = This table contains the results from a study of the X-ray to optical properties of a sample of 545 X-ray selected Type 1 AGN, from the XMM-Newton Cosmic Evolution (XMM-COSMOS) survey, over a wide range of redshifts (0.04 < z < 4.25) and X-ray luminosities (40.6 <= log(L<sub>2-10keV</sub>) <= 45.3). About 60% of them are spectroscopically identified Type 1 AGN, while the others have a reliable photometric redshift and are classified as Type 1 AGN on the basis of their multi-band Spectral Energy Distributions (SEDs). In the reference, the authors discuss the relationship between UV and X-ray luminosity, as parametrized by the X-ray to optical-UX alpha<sub>ox</sub> spectral slope, and its dependence on redshift and luminosity. Herein optical and X-ray properties for 545 Type 1 AGN in XMM-COSMOS are presented. For each source, X-ray ID, spectroscopic redshift, photometric redshift, upper error on the photometric redshift, lower error on the photometric redshift, logarithm of the monochromatic luminosity at 2500 Angstroms, logarithm of the monochromatic luminosity at 2 keV, alpha<sub>ox</sub>, logarithm of the 2-10 keV luminosity, logarithm of the bolometric luminosity in solar units, bolometric correction, photometric classification, logarithm of the Eddington ratio, logarithm of the black hole mass in solar masses, and a flag for the 2-10 keV detection (flag = 1 [343 entries] means a detection in the 2-10 keV band, while flag = 0 is for 2-10 keV upper limits) are given. This table was created by the HEASARC in May 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/512/A34">CDS catalog J/A+A/512/A34</a> file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcosmagn.html
bib_reference = 2010A&A...512A..34L
obs_regime = optical
obs_regime = uv
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcosmagn&
tap_tablename = xmmcosmagn
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744541
ID = nasa.heasarc/xmmcosmoid
publisher_did = ivo://nasa.heasarc/xmmcosmoid
obs_collection = XMMCOSMOID
obs_title = XMM-COSMOS Catalog of Optical/IR Counterparts
obs_description = This table contains the final optical identifications of the medium-depth (~60 ks), contiguous (2 degree<sup>2</sup>) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~1800 X-ray sources down to limiting fluxes of ~5 x 10<sup>-16</sup>, ~3 x 10<sup>-15</sup>, and ~7 x 10<sup>-15</sup> erg cm<sup>-2</sup> s<sup>-1</sup> in the 0.5-2 keV, 2-10 keV, and 5-10 keV bands, respectively (~1 x 10<sup>-15</sup>, ~6 x 10<sup>-15</sup>, and ~1 x 10<sup>-14</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, in the three bands, respectively, over 50% of the area). The work is complemented by an extensive collection of multi-wavelength data from 24 microns to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for >~50% of the sample, and high-quality photometric redshifts for the rest. The XMM-Newton and multi-wavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24 um detections. Thanks to the redshift completeness (almost 100%) the authors were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of log L<sub>X</sub> > 44.5 active galactic nuclei (AGNs) is at z ~ 2. Spectroscopically identified obscured and unobscured AGNs, as well as normal and star-forming galaxies, present well-defined optical and infrared properties. The authors devised a robust method to identify a sample of ~150 high-redshift (z > 1), obscured AGN candidates for which optical spectroscopy is not available. They were able to determine that the fraction of the obscured AGN population at the highest (L<sub>X</sub> > 10<sup>44</sup> erg s<sup>-1</sup>) X-ray luminosity is ~15%-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. The authors studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO (source number 2028), caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations. This table was created by the HEASARC in July 2010 based on the electronic version of Table 2 from the paper which was obtained from the Astrophysical Journal web site. <p> The HEASARC has made some changes to this material in order to make it more compliant with CDS/IAU Nomenclature and HEASARC table standards: <p> (i) The original naming convention suggested by the authors used a prefix of 'XMMC_' and the J2000.0 RA and Dec position in decimal degrees to 10<sup>-5</sup> degrees precision, e.g., XMMC_150.10515+1.98082'; the HEASARC has replaced these names by alternative new ones (in the alt_name parameter) of the form 'XMMU JHHMMSS.s+DDMMSS' where the prefix is the usual one for XMM-Newton sources and the remainder of the field is the J2000.0 equatorial coordinates truncated to 0.1 seconds of time in RA and to 1 arcsecond in Declination; <p> (ii) We have used for the alt_name parameter the naming convention recommended by the Dictionary of Nomenclature of Celestial Objects for XMM-COSMOS sources, viz. the "XMMC' prefix and the source (XID) number, e.g., "XMMC 2028'. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcosmoid.html
bib_reference = 2010ApJ...716..348B
obs_regime = infrared
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcosmoid&
tap_tablename = xmmcosmoid
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744637
ID = nasa.heasarc/xmmcosmos
publisher_did = ivo://nasa.heasarc/xmmcosmos
obs_collection = XMMCOSMOS
obs_title = XMM-Newton COSMOS X-Ray Point Source Catalog
obs_description = This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg<sup>2</sup> of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg<sup>2</sup>. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml > 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s, ~9.3 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s and ~1.3 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s over 90% of the area (1.92 deg<sup>2</sup>) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively. This table was created by the HEASARC in April 2009 based on the electronic version of Table 3 from the paper which was obtained from the CDS (their catalog J/A+A/497/635 file catalog.dat). It was last updated in May 2010 to correct the source number for XMMU J100100.7+015947 to be XMMC 129, as indicated by SIMBAD. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcosmos.html
bib_reference = 2009A&A...497..635C
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcosmos&
tap_tablename = xmmcosmos
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744645
ID = nasa.heasarc/xmmcphotz
publisher_did = ivo://nasa.heasarc/xmmcphotz
obs_collection = XMMCPHOTZ
obs_title = XMM-Newton COSMOS (XMM-COSMOS) Survey Photometric Redshift Catalog
obs_description = In their paper, the authors release accurate photometric redshifts for 1692 counterparts to Chandra sources in the central square degree of the Cosmic Evolution Survey (COSMOS) field. The availability of a large training set of spectroscopic redshifts that extends to faint magnitudes enabled photometric redshifts comparable to the highest quality results presently available for normal galaxies. The authors demonstrate that morphologically extended, faint X-ray sources without optical variability are more accurately described by a library of normal galaxies (corrected for emission lines) than by active galactic nucleus (AGN) dominated templates, even if these sources have AGNlike X-ray luminosities. Preselecting the library on the bases of the source properties allowed them to reach an accuracy sigma[Delta-z/(1+Z<sub>spec</sub>)] ~ 0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS sample. These Chandra sources are not contained in this table but are available in the HEASARC table CCOSMPHOTZ). In addition, in this study the authors released revised photometric redshifts for the 1735 optical counterparts of the XMM-detected sources over the entire 2 deg<sup>2</sup> of COSMOS, and these are the sources listed in the present table. For 248 sources, their updated photometric redshift differs from the previous release by Delta-z > 0.2. These changes are predominantly due to the inclusion of newly available deep H-band^ photometry (H<sub>AB</sub> = 24 mag). The authors illustrate once again the importance of a spectroscopic training sample and how an assumption about the nature of a source together, with the number and the depth of the available bands, influences the accuracy of the photometric redshifts determined for AGN. These considerations should be kept in mind when defining the observational strategies of upcoming large surveys targeting AGNs, such as eROSITA at X-ray energies and the Australian Square Kilometre Array Pathfinder Evolutionary Map of the Universe in the radio band. This table contains the photometric redshifts and related quantities for 1735 XMM-Newton sources over the entire 2 square degrees of the COSMOS field. Notice that in the original as-published paper no positional information was provided. The HEASARC has assumed that the source numbers used in the present catalog are in the same source numbering scheme as used by Cappelluti et al. (2009, A&A, 497, 635, the XMM-Newton Wide-Field Survey in the COSMOS Field Point-like X-ray Source Catalog, available at the HEASARC as the XMMCOSMOS table) and thus obtained the positions and (position-based) names corresponding to these X-ray sources from the latter. This table was created by the HEASARC in November 2011 based on an electronic version of Table 5 from the reference paper which was obtained from the ApJ website. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcphotz.html
bib_reference = 2011ApJ...742...61S
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcphotz&
tap_tablename = xmmcphotz
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744657
ID = nasa.heasarc/xmmcty2agn
publisher_did = ivo://nasa.heasarc/xmmcty2agn
obs_collection = XMMCTY2AGN
obs_title = XMM-COSMOS X-Ray Selected Type-2 AGN
obs_description = This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10<sup>10</sup> solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M<sub>U</sub>, absolute magnitude M<sub>V</sub>, absolute magnitude M<sub>J</sub> (Johnson-Kron-Cousin system), and the morphological class. This table was created by the HEASARC in October 2011 based on CDS table J/A+A/534/A110 file table1.dat. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmcty2agn.html
bib_reference = 2011A&A...534A.110L
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmcty2agn&
tap_tablename = xmmcty2agn
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744665
ID = nasa.heasarc/xmmgps
publisher_did = ivo://nasa.heasarc/xmmgps
obs_collection = XMM/GPS
obs_title = XMM-Newton Galactic Plane Survey - XGPS
obs_description = This table contains the first results from the XMM-Newton Galactic Plane Survey (XGPS). In the first phase of the program, 22 pointings were used to cover a region of approximately 3 square degrees between 19 and 22 degrees in Galactic Longitude and +/-0.6 degrees in Galactic Latitude. In total, over 400 point X-ray sources have been resolved at >=5-sigma significance, down to a flux limit of ~2 x 10^-14 erg/s/cm^2 (2-10 keV). The sources exhibit a very wide range of spectral hardness, with interstellar absorption identified as a major influence. The source populations detected in the soft (0.4 - 2 keV) band and hard (2 - 6 keV) band show surprisingly little overlap. The majority of the soft sources appear to be associated with relatively nearby stars with active stelaar coronae, judging from their high coincidence with bright stellar counterparts. The combination of the XGPS measurements in the hard X-ray band with the results from earlier surveys carried out by ASCA and Chandra reveals the form of the low-latitude X-ray source counts over 4 decades of flux. It appears that extragalactic sources dominate below ~10^-13 erg/s/cm^2 (2-10 keV), with a predominantly Galactic source population present above this flux threshold. The nature of the faint Galactic population observed by XMM-Newton remains uncertain, although cataclysmic variables and RS CVn systems may contribute substantially. This table was created by the HEASARC in February 2005 based on CDS Catalog J/MNRAS/351/31/tablea1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmgps.html
bib_reference = 2004MNRAS.351...31H
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmgps&
tap_tablename = xmmgps
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744677
ID = nasa.heasarc/xmmlss
publisher_did = ivo://nasa.heasarc/xmmlss
obs_collection = XMMLSS
obs_title = XMM-Newton Large-Scale Structure X-Ray Source Catalog
obs_description = The XMM-Newton Large-Scale Structure (XMM-LSS) X-Ray Source Catalog contains the source list for the first 5.5 surveyed square degrees of the XMM-LSS, with a total of 3385 point-like or extended sources above a detection likelihood of 15 in either 0.5 - 2 keV or 2 - 10 keV bands. The agreement with deep log N- log S is excellent. The main parameters considered are position, count rate, source extent with associated likelihood values. A set of additional quantities such as astrometric corrections and fluxes are further calculated while errors on the position and count rate are deduced from simulations. This table contains the main parameters, while further parameters and data products (X-ray images and optical thumbnails) are available at the Milan XMM-LSS database site: <a href="http://cosmos.iasf-milano.inaf.it/~lssadmin/Website/LSS/Query">http://cosmos.iasf-milano.inaf.it/~lssadmin/Website/LSS/Query</a> This table was created by the HEASARC in February 2008 based on the CDS Catalog J/MNRAS/382/279 file xlss.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmlss.html
bib_reference = 2007MNRAS.382..279P
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmlss&
tap_tablename = xmmlss
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744685
ID = nasa.heasarc/xmmlss10ks
publisher_did = ivo://nasa.heasarc/xmmlss10ks
obs_collection = XMMLSS10KS
obs_title = XMM-Newton Large-Scale Structure Uniform 10-ksec Exposure X-Ray Source Catalog
obs_description = This table contains some of the X-ray results from the final release of the multiwavelength XMM-Large Scale Structure (LSS) data set, covering the full survey area of 11.1 deg<sup>2</sup>. The 124 XMM-Newton observations used in the complete XMM-LSS are described in Section 2 and Table 1 of the primary reference paper (Chiappetti et al. 2013, hereafter Paper II). The X-ray data were processed with the latest XMM-LSS XAMIN pipeline version. The catalogs in Paper II supersede the catalog from the first paper in this series (Paper I: Pierre et al. 2007, MNRAS, 382, 279, available at the HEASARC as the XMMLSS table) pertaining to the initial 5 deg<sup>2</sup>. The authors provide X-ray source lists in the customary soft and hard energy bands (0.5-2 keV and 2-10 keV, respectively) for a total of 5572 objects in the catalog limited to 10 ks exposures presented in this table, and a total of 6721 objects in the deep full-exposure 2XLSSd catalog (available at the HEASARC as the XMMLSSDEEP table), above a detection likelihood of 15 in at least one band. At the XMMLSS web site which they maintain (<a href="http://cosmosdb.iasf-milano.inaf.it/XMM-LSS/">http://cosmosdb.iasf-milano.inaf.it/XMM-LSS/</a>), the authors also provide a multiwavelength catalog, cross-correlating their list of X-ray sources with infrared, near-infrared, optical and ultraviolet catalogs. Customary data products, such as X-ray FITS images and thumbnail images from the Canada-France-Hawaii Telescope Legacy Survey and the Spitzer Wide-Area Infrared Extragalactic Survey, are made available there, together with their data base in Milan, which can be queried interactively. In this table, the authors provide the source list for the full area (11.1 square degrees) of the XMM-LSS, with a total of 5572 point-like or extended sources above a detection likelihood of 15 in either the 0.5-2 or 2-10 keV bands. This table, the "standard" 2XLSS catalog containing the results of the analysis of the survey area using uniform 10-ksec exposures for all pointings longer than 10 ksec, lists the main X-ray parameters, while further multiwavelength parameters and data products (X-ray images and optical/IR thumbnails) are available at the Milan XMM-LSS database site referenced above. It supersedes the first XMM-LSS version (Pierre et al. 2007, available at the HEASARC as the XMMLSS table). Analogously to Paper I, only sources with an off-axis angle < 13 arcmin were processed by the authors' X-ray data processing pipeline software, XAMIN. The catalog includes all the extended sources classified in the customary C1 and C2 classes (see Section 3.6 of Paper II) plus all point-like sources with a point source detection likelihood (DET_LH) greater than 15 (so-called non-spurious sources). This table was created by the HEASARC in February 2013 based on the CDS catalog J/MNRAS/429/1652 file 2xlss.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmlss10ks.html
bib_reference = 2013MNRAS.429.1652C
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmlss10ks&
tap_tablename = xmmlss10ks
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744697
ID = nasa.heasarc/xmmlssclas
publisher_did = ivo://nasa.heasarc/xmmlssclas
obs_collection = XMMLSSCLAS
obs_title = XMM-Newton Large-Scale Structure Optical Counterparts and Redshifts
obs_description = The XMM-Large Scale Structure (XMM-LSS) survey, covering an area of 11.1 square degrees, contains more than 6,000 X-ray point-like sources detected with the XMM-Newton Observatory to a flux of 3 x 10<sup>-15</sup> erg/s/cm<sup>2</sup> in the 0.5-2.0 keV band. The vast majority of these sources have optical (CFHTLS: Canada France Hawaii Telescope Legacy Survey), infrared (SWIRE: Spitzer Wide-area InfraRed Extragalactic legacy survey) InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS), near-infrared (UKIDSS: UKIRT Infrared Deep Sky Survey) and/or ultraviolet (GALEX: Galaxy Evolution Explorer) counterparts. The authors wished to investigate the environmental properties of the different types of the XMM-LSS X-ray sources by defining their environment using the i'-band CFHTLS W1 catalog of optical galaxies to a magnitude limit of 23.5 magnitudes. They have classified 4,435 X-ray selected sources on the basis of their spectra, spectral energy distributions (SEDs), and X-ray luminosities, and estimated their photometric redshifts, which have a 4-11 band photometry with an accuracy of sigma[Delta<sub>z</sub>/(1+z<sub>sp</sub>)] = 0.076, with 22.6% outliers for i' < 26 mag. The authors estimated the local overdensities of 777 X-ray sources that have spectro-z or photo-z calculated by using more than seven bands (accuracy of sigma[(Delta<sub>z</sub>/(1+z<sub>sp</sub>)] = 0.061, with 13.8% outliers) within the volume-limited region defined by 0.1 <= z <= 0.85 and -23.5 < M_i'_ < -20. Although X-ray sources may be found in variety of environments, a high fraction (~55-60%), as verified by comparing with the random expectations, reside in overdense regions. The galaxy overdensities within which X-ray sources reside show a positive recent redshift evolution (at least for the range studied; z <~ 0.85). The authors also find that X-ray selected galaxies, when compared to AGN, inhabit significantly higher galaxy overdensities, although their spatial extent appear to be smaller than that of AGN. Hard AGN (harness ratios HR >= -0.2) are located in more overdense regions than soft AGN (HR < -0.2), which is clearly seen in both redshift ranges, although it appears to be stronger in the higher redshift range (0.55 < z < 0.85). Furthermore, the galaxy overdensities (with delta > 1.5, where delta is defined in equation (3) of the reference paper) within which soft AGN are embedded appear to evolve more rapidly compared to the corresponding overdensities around hard AGN. This table contains the spectroscopic and/or photometric redshifts for 4,206 X-ray selected sources in the XMM-LSS field which have optical counterparts and have been classified by the authors. This table was created by the HEASARC in September 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/557/A81">CDS Catalog J/A+A/557/A81</a> file table2.dat This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmlssclas.html
bib_reference = 2013A&A...557A..81M
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmlssclas&
tap_tablename = xmmlssclas
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744705
ID = nasa.heasarc/xmmlssdeep
publisher_did = ivo://nasa.heasarc/xmmlssdeep
obs_collection = XMMLSSDEEP
obs_title = XMM-Newton Large-Scale Structure Deep Full-Exposure X-Ray Source Catalog
obs_description = This table contains some of the X-ray results from the final release of the multiwavelength XMM-Large Scale Structure (LSS) data set, covering the full survey area of 11.1 deg<sup>2</sup>. The 124 XMM-Newton observations used in the complete XMM-LSS are described in Section 2 and Table 1 of the primary reference paper (Chiappetti et al. 2013, hereafter Paper II). The X-ray data were processed with the latest XMM-LSS XAMIN pipeline version. The catalogs in Paper II supersede the catalog from the first paper in this series (Paper I: Pierre et al. 2007, MNRAS, 382, 279, available at the HEASARC as the XMMLSS table) pertaining to the initial 5 deg<sup>2</sup>. The authors provide X-ray source lists in the customary soft and hard energy bands (0.5-2 keV and 2-10 keV, respectively) for a total of 6721 objects in the deep full-exposure 2XLSSd catalog presented in this table, and 5572 objects in the catalog limited to 10 ks exposures (available at the HEASARC as the XMMLSS10KS table), above a detection likelihood of 15 in at least one band. At the XMMLSS web site which they maintain (<a href="http://cosmosdb.iasf-milano.inaf.it/XMM-LSS/">http://cosmosdb.iasf-milano.inaf.it/XMM-LSS/</a>), the authors also provide a multiwavelength catalog, cross-correlating their list of X-ray sources with infrared, near-infrared, optical and ultraviolet catalogs. Customary data products, such as X-ray FITS images and thumbnail images from the Canada-France-Hawaii Telescope Legacy Survey and the Spitzer Wide-Area Infrared Extragalactic Survey, are made available there, together with their data base in Milan, which can be queried interactively. In this table, the authors provide the source list for the full area (11.1 square degrees) of the XMM-LSS, with a total of 6721 point-like or extended sources above a detection likelihood of 15 in either the 0.5-2 or 2-10 keV bands. This table, the 2XLSSd "deep catalog" version containing the result of the analysis of the full-length exposures, lists the main X-ray parameters, while further multiwavelength parameters and data products (X-ray images and optical/IR thumbnails) are available at the Milan XMM-LSS database site referenced above. It supersedes the first XMM-LSS version (Pierre et al. 2007, available at the HEASARC as the XMMLSS table). Analogously to Paper I, only sources with an off-axis angle < 13 arcmin were processed by the authors' X-ray data processing pipeline software, XAMIN. The catalog includes all the extended sources classified in the customary C1 and C2 classes (see Section 3.6 of Paper II) plus all point-like sources with a point source detection likelihood (DET_LH) greater than 15 (so-called non-spurious sources). This table was created by the HEASARC in February 2013 based on the CDS catalog J/MNRAS/429/1652 file 2xlssd.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmlssdeep.html
bib_reference = 2013MNRAS.429.1652C
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmlssdeep&
tap_tablename = xmmlssdeep
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744717
ID = nasa.heasarc/xmmlssoid
publisher_did = ivo://nasa.heasarc/xmmlssoid
obs_collection = XMMLSSOID
obs_title = XMM-Newton Large-Scale Structure Optical Identifications Catalog
obs_description = This table contains optical spectroscopic identifications of X-ray sources in ~3 square degrees of the XMM-Large Scale Structure survey (XMM-LSS), also covered by the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS), which were obtained with the AAOmega instrument at the 3.9-m Anglo-Australian Telescope during the nights of 2006 September 25-27 and 2007 September 11-13. In a flux-limited sample of 829 point-like sources in the optical band with g' <= 22 magnitudes and the 0.5-2 keV flux (f_0.5-2keV) > 10<sup>-15</sup> erg/cm<sup>2</sup>/s, the authors observed 693 objects and obtained reliable spectroscopic identification for 487 sources, approximately 59% of the overall sample. The authors therefore have increased the number of identifications in this field by a factor close to 5. Galactic stellar sources represent about 15% of the total (74/487). About 54% (265/487) are broad-line active galactic nuclei (AGN) spanning redshifts between 0.15 and 3.87 with a median value of 1.68. The optical-to-X-ray spectral index (alpha_ox) of the broad-line AGN is 1.47 +/- 0.03, typical of optically selected type I quasars, and is found to correlate with the rest-frame X-ray and optical monochromatic luminosities at 2 keV and 2500 Angstroms, respectively. Consistent with previous studies, the authors find that alpha_ox is not correlated with z. In addition, 32 and 116 X-ray sources are, respectively, absorption- and emission-line galaxies at z < 0.76. From a line ratio diagnostic diagram, it is found that in about 50% of these emission-line galaxies, the emission lines are powered significantly by the AGN. 30 of the XMM sources are detected at one or more radio frequencies (see Table 5 in the published paper). In addition, 24 sources (listed in table 4 of the published paper) have ambiguous identification: in eight cases, two XMM sources have a single optical source within 6 arcsec of each of them, whereas two and 14 XMM sources have, respectively, three and two possible optical sources within 6 arcsec of each of them. Spectra of multiple possible counterparts were obtained in such ambiguous cases. This HEASARC table contains the 487 sources which were reliably spectroscopically identified. This table was created by the HEASARC in July 2010 based on the CDS Catalog J/MNRAS/401/294 file table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmlssoid.html
bib_reference = 2010MNRAS.401..294S
obs_regime = x-ray
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmlssoid&
tap_tablename = xmmlssoid
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744725
ID = nasa.heasarc/xmmmaster
publisher_did = ivo://nasa.heasarc/xmmmaster
obs_collection = XMM
obs_title = XMM-NewtonMasterLog&PublicArchive
obs_description = This is the XMM-Newton Master Catalog and Public Archive table which has been created from information supplied to the HEASARC by the XMM-Newton Project. It is periodically updated as necessary. This database table contains the list of observations which have already been made by the XMM-Newton observatory, as well as those which are scheduled to be made in the near future (usually a a few weeks to a month ahead of the present). It does not contain observations which are scheduled to be performed further in the future, nor does it contain accepted observations which have not yet been scheduled. The list of all accepted XMM-Newton observations, including a number of ones which are unlikely to ever be carried out, such as accepted priority C targets, is available in the XMMAO Browse table. This table includes entries for both pointed data and for data obtained during spacecraft slews. The slew observations all have obsid values beginning with the digit 9 and, because they were not made at a fixed position, lack any positional information such as RA and Declination. Some XMM-Newton observations for which the archived data has become publicly available as indicated by the public_date parameter value, i.e., the proprietary period has expired, are not currently available at the HEASARC: such cases will have values of 'N' for the data_in_heasarc parameter. These datasets in most cases are available at the ESA XMM-Newton Science Archive (XSA) at <a href="http://nxsa.esac.esa.int/nxsa-web/">http://nxsa.esac.esa.int/nxsa-web/</a>. For much more detailed information on the XMM-Newton instruments and their operation, please refer to the XMM-Newton Users Handbook at <a href="http://heasarc.gsfc.nasa.gov/docs/xmm/uhb/">http://heasarc.gsfc.nasa.gov/docs/xmm/uhb/</a>. This database table was created by the HEASARC based on information supplied by the XMM-Newton Project at the following URLs: <pre> <a href="http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaobslog.txt">http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaobslog.txt</a> <a href="http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaslewlog.txt">http://nxsa.esac.esa.int/ftp_public/heasarc_obslog/xsaslewlog.txt</a> <a href="https://xmm-tools.cosmos.esa.int/external/xmm_mission_plan/odf_pps/catstrip.shtml">https://xmm-tools.cosmos.esa.int/external/xmm_mission_plan/odf_pps/catstrip.shtml</a> </pre> It is periodically updated within a few days of whenever these XMM-Newton Project's URLs are modified. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmmaster.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmmaster&
tap_tablename = xmmmaster
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
sia_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=xmmmaster&
sia2_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/sia?table=xmmmaster&
sia2_glutag = SIA2
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744745
ID = nasa.heasarc/xmmobstars
publisher_did = ivo://nasa.heasarc/xmmobstars
obs_collection = XMMOBSTARS
obs_title = XMM-Newton OB Stars Catalog
obs_description = Following the advent of increasingly sensitive X-ray observatories, deep observations of early-type stars became possible. However, the results for only a few objects or clusters have until now been reported and there has been no large survey comparable to that based upon the ROSAT All-Sky Survey (RASS). A limited survey of X-ray sources, consisting of all public XMM observations (2XMMi) and slew survey data (XMMSL1), is now available. The X-ray counterparts to hot, massive stars have been searched for in these catalogs. About 300 OB stars were detected with XMM. Half of them were bright enough for a spectral analysis to be possible, and we make available the detailed spectral properties that were derived. The X-ray spectra of O stars are represented well by low (< 1 keV) temperature components and seem to indicate that an absorption column is present in addition to the interstellar contribution. The X-ray fluxes are well correlated with the bolometric fluxes, with a scatter comparable to that of the RASS studies and thus larger than found previously with XMM for some individual clusters. These results contrast with those of B stars that exhibit a large scatter in the L<sub>X</sub> - L<sub>bol</sub> relation, no additional absorption being found, and the fits indicate a plasma at higher temperatures. Variability (either within one exposure or between multiple exposures) was also investigated whenever possible: short-term variations are far more rare than long-term ones (the former affects a few percent of the sample, while the latter concerns between one third and two thirds of the sources). This is a catalog of X-ray emitters amongst early-type stars following a correlation between the Reed (2003, AJ, 125, 2531) Catalog of galactic OB Stars and the 2XMMi Catalog (Watson et al. 2009, A&A, 493, 339). See the reference paper for more details. This table was created by the HEASARC in November 2009 based on CDS table J/A+A/506/1055 file table1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmobstars.html
bib_reference = 2009A&A...506.1055N
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmobstars&
tap_tablename = xmmobstars
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744757
ID = nasa.heasarc/xmmomcat
publisher_did = ivo://nasa.heasarc/xmmomcat
obs_collection = XMMOMCAT
obs_title = XMM-Newton OM Object Catalog
obs_description = The Optical Monitor Catalog of serendipitous sources (OMCat) contains entries for every source detected in the publicly available XMM-Newton Optical Monitor (OM) images taken in the imaging mode. Since the OM records data simultaneously with the X-ray telescopes on XMM-Newton, it typically produces images in one or more near-UV/optical bands for every pointing of the observatory. As of the beginning of 2014, the data in the public archive covered roughly 0.5% of the sky in 3425 fields. The OMCat is not dominated by sources previously undetected at other wavelengths; the bulk of objects have optical counterparts. However, the OMCat can be used to extend optical or X-ray spectral energy distributions for known objects into the ultraviolet, to study at higher angular resolution objects detected with GALEX, or to find high-Galactic-latitude objects of interest for UV spectroscopy. Differences between the current OMCat and the previous version of the OMCat (which was designated as XMMOMOBJ) are improved coordinates, improved quality flags, and a reduced number of spurious sources. The OM reduction was done with the standard ESAS software, with post-processing to apply the coordinate corrections in a more consistent manner. There is a major change in the way the data are represented in the table. In the previous XMMOMOBJ table a separate row was generated for each filter. In the current XMMOMCAT table each observation of each object generates only a single row regardless of how many filters were used. Unused filters have nulls while filters where the object is not detected have nulls for the detection parameters but a non-zero value for exposure. The table includes information for each filter and averaged information for the object as a whole. Only filters in which the object was detected are used in the averages. The parameters in this table comprise two sets: parameters describing the detection overall including id's and mean values, and values specific to the individual bands. There are three possible situations for the band data: (1) If there was no exposure in that band, then all fields for that band will be null. (2) If there was some exposure in the band but the object was not detected in that band, then the exposure field will give the actual exposure, but all of the other fields for that band will be null. (3) If the object was detected, then all of the fields for the band should be filled in. The filters included are V, B, U, UVW1, UVM2, UVW2 and white (i.e., unfiltered). The original table (formerly known as XMMOMOBJ) was created by the HEASARC in March 2008, based on a table supplied by the authors. The XMMOMCAT version was generated and ingested in February 2014 using a program which concatenated the objects detected in processing each observation. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmomcat.html
bib_reference = 2008PASP..120..740K
obs_regime = optical
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmomcat&
tap_tablename = xmmomcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744765
ID = nasa.heasarc/xmmomcdfs
publisher_did = ivo://nasa.heasarc/xmmomcdfs
obs_collection = XMMOMCDFS
obs_title = XMM-Newton Optical Monitor Chandra Deep Field-South UV Catalog
obs_description = The XMM-Newton X-ray observatory has performed repeated observations of the Chandra Deep Field-South (CDFS) in 33 epochs (2001 - 2010) through the XMM-CDFS Deep Survey (Comastri et al. 2011, A&A, 526, L9). During the X-ray observations, the XMM-Newton Optical Monitor (XMM-OM) targeted the central 17 x 17 arcmin<sup>2</sup> region of the X-ray field of view, providing simultaneous optical/UV coverage of the CDFS. The resulting set of data can be taken into account to build an XMM-OM catalog of the CDFS, filling the UV spectral coverage between the optical surveys and GALEX observations. This table contains the UV catalog of the XMM-CDFS Deep Survey. Its main purpose is to provide complementary UV average photometric measurements of known optical/UV sources in the CDFS, taking advantage of the unique characteristics of the survey. The data reduction is intended also to improve the standard source detection on individual observations, by cataloguing faint sources through the stacking of their exposure images. The authors reprocessed the XMM-OM data of the survey and stacked the exposures from consecutive observations using the standard SAS tools to process the data obtained during single observations. Average measurements of detections with SAS good quality flags from individual observations and from stacked images have been joined to compile the catalogue. Sources have been validated through the cross-identification within the ESO Imaging Survey (EIS: Arnouts et al. 2001, A&A, 379, 740) and COMBO-17 (Wolf et al. 2004, A&A, 421, 913; 2008, A&A, 492, 933) surveys. Photometric data of 1129 CDFS sources are provided in the main catalog, and optical/UV/X-ray photometric and spectroscopic information from other surveys are also included. The stacking extends the detection limits by ~1 mag in the three UV bands, contributing 30% of the catalogued UV sources. The comparison with the available measurements in similar spectral bands confirms the validity of the XMM-OM calibration. The combined COMBO-17/X-ray classification of the "intermediate" sources (e.g. optically diluted and/or X-ray absorbed AGN) is also discussed in the reference paper. This table was created by the HEASARC in June 2015 based on the union of <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/217/4/">CDS Catalog J/ApJS/217/4/</a> files omcdfst7.dat (the 1,129 sources in the main catalog) and omcdfst8.dat (the 44 sources in the supplementary catalog). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmomcdfs.html
bib_reference = 2015A&A...574A..49A
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmomcdfs&
tap_tablename = xmmomcdfs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744773
ID = nasa.heasarc/xmmomsuob
publisher_did = ivo://nasa.heasarc/xmmomsuob
obs_collection = XMMOMSUOB
obs_title = XMM-Newton Optical Monitor SUSS Catalog, v6.1: Observation IDs
obs_description = The 2023 release of the XMM OM Serendipitous Ultraviolet Source Survey (XMM-SUSS6.1) Catalog, a catalog of optical/UV sources detected by the Optical Monitor (OM) on-board the European Space Agency's (ESA's) XMM-Newton observatory, spans the period of observations from 2000 to November 2022. The data processing was performed at the European Space Astronomy Centre (ESAC, Madrid, Spain) using the XMM Science Analysis Software system (SAS) versions 18 and 19. In addition to covering a larger observation period, this sixth release reflects a change in philosophy with regard to the origin of the incorporated data. In previous releases, the data were generated via a bespoke processing of the OM Observation Data Files (ODFs) while in this new release, the catalog has been guided by the XMM user community and the authors have sought to harmonize the contents of the catalog with those of the OM data in the XMM-Newton Science Archive (XSA), which derive from the standard XMM-Newton pipeline processing system. While the bespoke processing and pipeline systems are fundamentally very similar, they are not identical and the differences lead to some differences in the output. The number of observations (OBSIDs) included in the catalog is 12,057. This table (XMMOMSUOB) contains the list of these observations and their characteristics, giving for each observation the filters used, the exposure time for each filter, the number of sources detected in each filter and the detection magnitude limit for each filter. The total number of entries in this release is 9,920,390. They correspond to 6,659,554 unique sources, of which 1,225,117 have multiple entries in the source table, corresponding to different observations. This list of sources is available at the HEASARC as the <a href="/W3Browse/xmm-newton/xmmomsuss.html">XMMOMSUSS table</a>. The documentation on the first release of this catalog is available at <a href="http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/Summary.shtml">http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/Summary.shtml</a>. This HEASARC database table contains the sixth release of the XMM-OM SUSS catalog, XMM-SUSS6.1, released by ESA in October 2023, obtained from the XMM-Newton Science Archive (<a href="http://xmm.esac.esa.int/xsa">http://xmm.esac.esa.int/xsa</a>), and ingested into the HEASARC database in October 2023. It is also available at the HEASARC as the gzipped FITS file <a href="https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSS6-1.1.fits.gz">https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSS6-1.1.fits.gz</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmomsuob.html
bib_reference = 2012MNRAS.426..903P
obs_regime = optical
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmomsuob&
tap_tablename = xmmomsuob
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744781
ID = nasa.heasarc/xmmomsuss
publisher_did = ivo://nasa.heasarc/xmmomsuss
obs_collection = XMMOMSUSS
obs_title = XMM-Newton Optical Monitor Serendipitous UV Source Survey Catalog, v6.1
obs_description = The 2023 release of the XMM OM Serendipitous Ultraviolet Source Survey (XMM-SUSS6.1) Catalog, a catalog of optical/UV sources detected by the Optical Monitor (OM) on-board the European Space Agency's (ESA's) XMM-Newton observatory, spans the period of observations from 2000 to November 2022. The data processing was performed at the European Space Astronomy Centre (ESAC, Madrid, Spain) using the XMM Science Analysis Software system (SAS) versions 18 and 19. In addition to covering a larger observation period, this sixth release reflects a change in philosophy with regard to the origin of the incorporated data. In previous releases, the data were generated via a bespoke processing of the OM Observation Data Files (ODFs) while in this new release, the catalog has been guided by the XMM user community and the authors have sought to harmonize the contents of the catalog with those of the OM data in the XMM-Newton Science Archive (XSA), which derive from the standard XMM-Newton pipeline processing system. While the bespoke processing and pipeline systems are fundamentally very similar, they are not identical and the differences lead to some differences in the output. The number of observations (OBSIDs) included in the catalog is 12,057. The total number of entries in this release is 9,920,390. They correspond to 6,659,554 unique sources, of which 1,225,117 have multiple entries in the source table, corresponding to different observations. For each entry, positional and photometric data (count rate, magnitude and flux) and quality flags for each measurement are provided. The description of the previous release of the catalog can be found in Page M.J. et al. (2012, MNRAS, 426, 903). U, B, V, UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the Source Properties: Filter Set section of the MSSL documentation for this catalog: <a href="http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/SourcePropertiesFilters.shtml">http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/SourcePropertiesFilters.shtml</a>. There is a second, related table which gives a summary of the observations from which the XMM-SUSS6.1 sources listed in this table have been detected and measured. That summary table is available at the HEASARC as the <a href="/W3Browse/xmm-newton/xmmomsuob.html">XMMOMSUOB table</a>. This HEASARC database table contains the sixth release of the XMM-OM SUSS catalog, XMM-SUSS6.1, released by ESA in October 2023, obtained from the XMM-Newton Science Archive (<a href="http://xmm.esac.esa.int/xsa">http://xmm.esac.esa.int/xsa</a>), and ingested into the HEASARC database in October 2023. It is also available at the HEASARC as the gzipped FITS file <a href="https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSS6-1.1.fits.gz">https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSS6-1.1.fits.gz</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmomsuss.html
bib_reference = 2012MNRAS.426..903P
obs_regime = optical
obs_regime = uv
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmomsuss&
tap_tablename = xmmomsuss
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744789
ID = nasa.heasarc/xmmsdssgce
publisher_did = ivo://nasa.heasarc/xmmsdssgce
obs_collection = XMMSDSSGCE
obs_title = 2XMMi/SDSS Galaxy Cluster Survey Extension
obs_description = This table contains results from the analysis of a sample of 383 X-ray selected galaxy groups and clusters with spectroscopic redshift measurements (up to z ~ 0.79) from the 2XMMi/SDSS Galaxy Cluster Survey. The X-ray cluster candidates were selected as serendipitously detected sources from the 2XMMi-DR3 catalog that were located in the footprint of the Sloan Digital Sky Survey (SDSS-DR7). The cluster galaxies with available spectroscopic redshifts were selected from the SDSS-DR10. The authors developed an algorithm for identifying the cluster candidates that are associated with spectroscopically targeted luminous red galaxies and for constraining the cluster spectroscopic redshift. A cross-correlation of the constructed cluster sample with published optically selected cluster catalogs yielded 264 systems with available redshifts. The present redshift measurements (presented in reference paper III) are consistent with the published values. The current cluster sample extends the optically confirmed cluster sample from the authors' cluster survey by 67 objects. Moreover, it provides spectroscopic confirmation for 78 clusters among their published cluster sample, which previously had only photometric redshifts. Of the new cluster sample that comprises 67 systems, 55 objects are newly X-ray discovered clusters and 52 systems are sources newly discovered as galaxy clusters in optical and X-ray wavelengths. Based on the measured redshifts and the fluxes given in the 2XMMi-DR3 catalogue, the authors have estimated the X-ray luminosities and masses of the cluster sample. This table contains 145 entries, 67 of which are new (as of Paper III) optically confirmed clusters (marked by values of ref_source = 'Paper III') and 78 of which are clusters from Paper II which have now been spectroscopically confirmed (marked by values of ref_source = 'Paper II'). The tabular information on the 530 clusters that was presented in Paper II of this set of papers is available as the HEASARC <a href="/W3Browse/xmm-newton/xmmsdssgcs.html">XMMSDSSGCS table</a>). The following parameters were obtained from the current optical-band cluster detection algorithm: sdss_dr10_bcg_id, sdss_dr10_bcg_ra, sdss_dr10_bcg_dec, bcg_rmag, redshift, num_spect_members, phot_redshift, num_phot_members, and spatial_offset. This table was created by the HEASARC in July 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/564/A54">CDS catalog J/A+A/564/A54</a> file table1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmsdssgce.html
bib_reference = 2014A&A...564A..54T
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmsdssgce&
tap_tablename = xmmsdssgce
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744797
ID = nasa.heasarc/xmmsdssgcs
publisher_did = ivo://nasa.heasarc/xmmsdssgcs
obs_collection = XMMSDSSGCS
obs_title = 2XMMi/SDSS Galaxy Cluster Survey
obs_description = The authors have compiled a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton Serendipitous Source Catalog (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). In their paper, they present an analysis of the X-ray properties of this new sample with particular emphasis on the X-ray luminosity-temperature (L<sub>X</sub> - T) relation. The X-ray cluster candidates were selected from the 2XMMi-DR3 catalog in the footprint of the SDSS-DR7. The authors developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. For optically confirmed clusters with good quality X-ray data, they derived the X-ray flux, luminosity, and temperature from proper spectral fits, while the X-ray flux for clusters with low-quality X-ray data was obtained from the 2XMMi-DR3 catalogue. The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03 to 0.70 (median z = 0.32). In this paper, they present the catalog of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalog has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting; (these objects are identified by having values for the table_sample parameter of 1 in this HEASARC implementation of the catalog) and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalog, because their X-ray data are insufficient for spectral fitting (these objects are identified by having values for the table_sample parameter of 2 herein). For each cluster, the catalog also provides the X-ray bolometric luminosity and the cluster mass at R<sub>500</sub> based on scaling relations and the position of the likely brightest cluster galaxy (BCG). The updated L<sub>X</sub> - T relation of the current sample with X-ray spectroscopic parameters is presented in the paper. The authors found the slope of the L<sub>X</sub> - T relation to be consistent with published ones. They see no evidence for evolution in the slope and intrinsic scatter of the L<sub>X</sub> - T relation with redshift when excluding the low-luminosity groups. This catalog of X-ray selected galaxy clusters and groups supersedes and subsumes the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprising 175 clusters of galaxies, which was presented in Takey et al. (2011, A&A, 534, A120). This table was created by the HEASARC in October 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/558/A75">CDS catalog J/A+A/558/A75</a> files table1.dat and table2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmsdssgcs.html
bib_reference = 2013A&A...558A..75T
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmsdssgcs&
tap_tablename = xmmsdssgcs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744809
ID = nasa.heasarc/xmmslewcln
publisher_did = ivo://nasa.heasarc/xmmslewcln
obs_collection = XMMSlewClean
obs_title = XMM-Newton Slew Survey Clean Source Catalog, v2.0
obs_description = This table contains the 'clean' sample of sources from the second catalog of X-ray sources found in slew data taken by the European Space Agency's XMM-Newton Observatory, XMMSL2 or XMMSLEW, Version 2.0. It has been constructed by members of the XMM-Newton Science Operations Centre (SOC) and the European Photon Imaging Camera (EPIC) consortium on behalf of ESA. This release uses results of work which was carried out within the framework of the EXTraS project ("Exploring the X-ray variable and Transient Sky"), funded from the EU's Seventh Framework Programme under grant agreement no.607452. This is the first release of XMMSL2 which contains data taken between revolutions 314 and 2758. The previous catalog was called XMMSL1_Delta6 and contained slews up to revolution 2441. XMMSL2 has been generated from 2114 slews, executed between 2001-08-26 and 2014-12-31, revolutions 314 to 2758. Not all slews made in this period have been used; slews with particularly high background throughout the slew or which gave processing problems have been rejected. A full discussion of the differences between XMMSL2 and XMMSL1 is given in Section 12 of the XMMSL2 Users Guide at <a href="https://www.cosmos.esa.int/web/xmm-newton/xmmsl2-ug">https://www.cosmos.esa.int/web/xmm-newton/xmmsl2-ug</a>. This database table was first created by the HEASARC in August 2007 based on the FITS version of XMMSL1D1 (v1.1) of the XMM Slew Catalog. The current version was created in April 2017 based on the FITS version of XMMSL2 (v2.0) of the XMM Slew Catalog obtained from the following URLs: <a href="http://nxsa.esac.esa.int/catalogues/xmmsl2_clean.fits.gz">http://nxsa.esac.esa.int/catalogues/xmmsl2_clean.fits.gz</a> (the clean sample), and <a href="http://nxsa.esac.esa.int/catalogues/xmmsl2_total.fits.gz">http://nxsa.esac.esa.int/catalogues/xmmsl2_total.fits.gz</a> (the total sample). <p> The HEASARC has endeavored to retain the same parameter names as in the ESA version, but has changed some so as to conform to the standard HEASARC parameters naming conventions, e.g., all error parameter names which ended in "_err" in the ESA version end in "_error" in this HEASARC version. For other parameters which have had their names changed, their original ESA names are listed in square brackets in their descriptions below. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmslewcln.html
bib_reference = 2008A&A...480..611S
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmslewcln&
tap_tablename = xmmslewcln
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744817
ID = nasa.heasarc/xmmslewegs
publisher_did = ivo://nasa.heasarc/xmmslewegs
obs_collection = XMMSLEWEGS
obs_title = XMM-Newton Slew Survey Extragalactic Sample
obs_description = The ongoing XMM-Newton Slew Survey (XSS) provides coverage of a significant fraction of the sky in a broad X-ray bandpass. Although shallow by contemporary standards, in the "classical" 2-10 keV band of X-ray astronomy the XSS provides significantly better sensitivity than any currently available all-sky survey. The authors investigate the source content of the XSS, focusing on detections in the hard 2-10 keV band down to a very low threshold (>= 4 counts net of background). At the faint end, the survey reaches a flux sensitivity of roughly 3 x 10<sup>-12</sup> erg/cm<sup>2</sup>/s (2-10 keV). The starting point was a sample of 487 sources detected in the XSS (up to and including release XMMSL1d2) at high galactic latitude in the hard band. Through cross-correlation with published source catalogs from surveys spanning the electromagnetic spectrum from radio through to gamma-rays, they find that 45% of the sources have likely identifications with normal/active galaxies. A further 18% are associated with other classes of X-ray object (nearby coronally active stars, accreting binaries, clusters of galaxies), leaving 37% of the XSS sources with no current identification. The authors go on to define an XSS extragalactic sample comprised of 219 galaxies and active galaxies selected in the XSS hard band. They investigate the properties of this extragalactic sample including its X-ray log N - log S distribution, and it is this sample that is contained in this table. The authors find that, in the low-count limit, the XSS is, as expected, strongly affected by Eddington bias. There is also a very strong bias in the XSS against the detection of extended sources, most notably clusters of galaxies. A significant fraction of the detections at and around the low-count limit may be spurious. Nevertheless, it is possible to use the XSS to extract a reasonably robust sample of extragalactic sources, excluding galaxy clusters. The differential log N - log S relation of these extragalactic sources matches very well to the HEAO-1 A2 all-sky survey measurements at bright fluxes and to the 2XMM source counts at the faint end. The substantial sky coverage afforded by the XSS makes this survey a valuable resource for studying X-ray bright source samples, including those selected specifically in the hard 2 - 10 keV band. This table was created by the HEASARC in December 2012, based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/548/A99">CDS Catalog J/A+A/548/A99</a> file tablea1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmslewegs.html
bib_reference = 2012A&A...548A..99W
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmslewegs&
tap_tablename = xmmslewegs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744825
ID = nasa.heasarc/xmmslewful
publisher_did = ivo://nasa.heasarc/xmmslewful
obs_collection = XMMSlewFull
obs_title = XMM-Newton Slew Survey Full Source Catalog, v2.0
obs_description = This table contains the 'total' sample of sources from the second catalog of X-ray sources found in slew data taken by the European Space Agency's XMM-Newton Observatory, XMMSL2 or XMMSLEW, Version 2.0. It has been constructed by members of the XMM-Newton Science Operations Centre (SOC) and the European Photon Imaging Camera (EPIC) consortium on behalf of ESA. This release uses results of work which was carried out within the framework of the EXTraS project ("Exploring the X-ray variable and Transient Sky"), funded from the EU's Seventh Framework Programme under grant agreement no.607452. This is the first release of XMMSL2 which contains data taken between revolutions 314 and 2758. The previous catalog was called XMMSL1_Delta6 and contained slews up to revolution 2441. XMMSL2 has been generated from 2114 slews, executed between 2001-08-26 and 2014-12-31, revolutions 314 to 2758. Not all slews made in this period have been used; slews with particularly high background throughout the slew or which gave processing problems have been rejected. A full discussion of the differences between XMMSL2 and XMMSL1 is given in Section 12 of the XMMSL2 Users Guide at <a href="https://www.cosmos.esa.int/web/xmm-newton/xmmsl2-ug">https://www.cosmos.esa.int/web/xmm-newton/xmmsl2-ug</a>. This database table was first created by the HEASARC in August 2007 based on the FITS version of XMMSL1D1 (v1.1) of the XMM Slew Catalog. The current version was created in April 2017 based on the FITS version of XMMSL2 (v2.0) of the XMM Slew Catalog obtained from the following URLs: <a href="http://nxsa.esac.esa.int/catalogues/xmmsl2_clean.fits.gz">http://nxsa.esac.esa.int/catalogues/xmmsl2_clean.fits.gz</a> (the clean sample), and <a href="http://nxsa.esac.esa.int/catalogues/xmmsl2_total.fits.gz">http://nxsa.esac.esa.int/catalogues/xmmsl2_total.fits.gz</a> (the total sample). <p> The HEASARC has endeavored to retain the same parameter names as in the ESA version, but has changed some so as to conform to the standard HEASARC parameters naming conventions, e.g., all error parameter names which ended in "_err" in the ESA version end in "_error" in this HEASARC version. For other parameters which have had their names changed, their original ESA names are listed in square brackets in their descriptions below. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmslewful.html
bib_reference = 2008A&A...480..611S
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmslewful&
tap_tablename = xmmslewful
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744833
ID = nasa.heasarc/xmmssc
publisher_did = ivo://nasa.heasarc/xmmssc
obs_collection = XMM/SSC
obs_title = XMM-Newton Serendipitous Source Catalog (4XMM-DR13 Version)
obs_description = The XMMSSC table contains the Fourth XMM-Newton Serendipitous Source Catalog, Thirteenth Data Release, or 4XMM-DR13. 4XMM-DR13 is the fourth-generation catalog of serendipitous X-ray sources from the European Space Agency's (ESA) XMM-Newton observatory, and has been created by the XMM-Newton Survey Science Centre (SSC) on behalf of ESA. It is an incremental version of the the 4XMM catalog and contains 531 more observations and 44,678 more detections than the preceding 4XMM-DR12 catalog, which was made public in July 2022. In addition, the team provides spectra and lightcurves for more than 16,762 more detections than in 4XMM-DR12. The catalog contains source detections drawn from a total of 13,243 XMM-Newton EPIC observations made between 2000 February 1 and 2022 December 31; all datasets included were publicly available by 2022 December 31 but not all public observations are included in this catalog. For net exposure time >= 1ksec, the net area of the catalog fields taking account of the substantial overlaps between observations is ~1,328 deg<sup>2</sup>. 4XMM-DR13 contains 983,948 X-ray detections above the processing likelihood threshold of 6. These X-ray detections relate to 656,997 unique X-ray sources. A significant fraction of sources (129,133, 20%) have more than one detection in the catalog (up to 90 repeat observations in the most extreme case). The catalog distinguishes between extended emission and point-like detections. Parameters of detections of extended sources are only reliable up to the maximum extent measure of 80 arcseconds. There are 91,763 detections of extended emission, of which 20,971 are 'clean' (in the sense that they were not flagged). Due to intrinsic features of the instrumentation as well as some shortcomings of the source detection process, some detections are considered to be spurious or their parameters are considered to be unreliable. It is recommended to use a detection flag and an observation flag as filters to obtain what can be considered a 'clean' sample. There are 854,095 out of 983,948 detections that are considered to be clean (i.e., summary flag < 3). For 353,538 detections, EPIC time series and 353,821 detections, EPIC spectra were automatically extracted during processing, and a chi<sup>2</sup>-variability test was applied to the time series. 8,029 detections in the catalog are considered variable, within the timespan of the specific observation, at a probability of 10<sup>-5</sup> or less based on the null-hypothesis that the source is constant. Of these, 6,039 have a summary flag <3. The median flux (in the total photon-energy band 0.2 - 12 keV) of the catalog detections is ~ 2.2 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s; in the soft energy band (0.2 - 2 keV) the median flux is ~ 5.2 x 10<sup>-15</sup>, and in the hard band (2 - 12 keV) it is ~1.2 x 10<sup>-14</sup>. About 23% have fluxes below 1 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s. The flux values from the three EPIC cameras are, overall, in agreement to ~10% for most energy bands. The median positional accuracy of the catalog point source detections is generally < 1.57 arcseconds (with a standard deviation of 1.43 arcseconds). With 4XMM-DR13, the team also released 4XMM-DR13s, available from HEASARC as <a href="/W3Browse/xmm-newton/xmmstack.html">XMMSTACK</a>, a new version of the stacked catalog built from 9,796 4XMM-DR13 overlapping observations. 4XMM-DR13s contains 1,688 stacks (or groups). Most of the stacks are composed of 2 observations and the largest has 372. The catalog contains 401,596 sources, of which 310,478 have several contributing observations. Stacking observations allows yet fainter sources to be detected in sky regions observed more than once, increasing the number of detections and uncovering long-term variability on repeatedly observed objects. 4XMM-DR13s reaches a depth of ~2.5 x 10<sup>-15</sup> and ~6.8 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s in the soft (0.2-2keV) and hard (2-12 keV) X-ray band, respectively. The energy bands used in the 4XMM-DR13 processing were the same as for the 3XMM catalog. The following are the basic energy bands: <pre> 1 = 0.2 - 0.5 keV 2 = 0.5 - 1.0 keV 3 = 1.0 - 2.0 keV 4 = 2.0 - 4.5 keV 5 = 4.5 - 12.0 keV </pre> while these are the broad energy bands: <pre> 6 = 0.2 - 2.0 keV soft band, no images made 7 = 2.0 - 12.0 keV hard band, no images made 8 = 0.2 - 12.0 keV total band 9 = 0.5 - 4.5 keV XID band </pre> This database table was last updated by the HEASARC in June 2023. It contains the 4XMM-DR13 catalog, released by ESA on 2023-06-12 and obtained from the XMM-Newton Survey Science Center Consortium (<a href="http://xmmssc.irap.omp.eu/Catalogue/4XMM-DR13/4XMM_DR13.html">http://xmmssc.irap.omp.eu/Catalogue/4XMM-DR13/4XMM_DR13.html</a>). It is also available as a gzipped FITS file at <a href="https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/4XMM_DR13cat_v1.0.fits.gz">https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/4XMM_DR13cat_v1.0.fits.gz</a>. <p> The previous versions of the Serendipitous Source Catalog, 3XMM-DR5, 3XMM-DR6, 3XMM-DR7, 3XMM-DR8, 4XMM-DR9, 4XMM-DR10, 4XMM-DR11, and 4XMM-DR12 are also available in the same directory for comparison purposes as the files 3XMM_DR5cat_v1.0.fits.gz, 3XMM_DR6cat_v1.0.fits.gz, 3XMM_DR7cat_v1.0.fits.gz, 3XMM_DR8_cat_v1.0.fits.gz, 4XMM_DR9_cat_v1.0.fits.gz, 4XMM_DR10cat_v1.0.fits.gz, 4XMM_DR11cat_v1.0.fits.gz, and 4XMM_DR12cat_v1.0.fits.gz, respectively. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmssc.html
bib_reference = 2009A&A...493..339W
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmssc&
tap_tablename = xmmssc
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744841
ID = nasa.heasarc/xmmsscgps
publisher_did = ivo://nasa.heasarc/xmmsscgps
obs_collection = XMMSSCGPS
obs_title = XMM-Newton Survey Science Center Survey of the Galactic Plane
obs_description = Many different classes of X-ray sources contribute to the Galactic landscape at high energies. Although the nature of the most luminous X-ray emitters is now fairly well understood, the population of low-to-medium X-ray luminosity (L<sub>X</sub> = 10<sup>27</sup> - 10<sup>34</sup> erg/s) sources remains much less studied, our knowledge being mostly based on the observation of local members. The advent of wide-field and high-sensitivity X-ray telescopes such as XMM-Newton now offers the opportunity to observe this low-to-medium L<sub>X</sub> population at large distances. This study reports the results of a Galactic plane survey conducted by the XMM-Newton Survey Science Centre (SSC). Beyond its astrophysical goals, this survey aims at gathering a representative sample of identified X-ray sources at low latitude that can be used later on to statistically identify the rest of the serendipitous sources discovered in the Milky Way. The survey is based on 26 XMM-Newton observations, obtained at |b| < 20 degrees, distributed over a large range in Galactic longitudes and covering a summed area of 4 deg<sup>2</sup>. The flux limit of this survey is 2 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s in the soft (0.5 - 2 keV) band and 1 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s in the hard (2 - 1 2keV) band. A total of 1319 individual X-ray sources have been detected. Using optical follow-up observations supplemented by cross-correlation with a large range of multi-wavelength archival catalogs, the authors identify 316 X-ray sources. This constitutes the largest group of spectroscopically identified low-latitude X-ray sources at this flux level. The majority of the identified X-ray sources are active coronae with spectral types in the range A to M at maximum distances of ~1 kpc. The number of identified active stars increases towards late spectral types, reaching a maximum at K. Using infrared colors, the authors classify 18% of the stars as giants. The observed distributions of F<sub>X</sub>/F<sub>V</sub>, X-ray and infrared colors indicates that their sample is dominated by a young (100 Myr) to intermediate (600 Myr) age population with a small contribution of close main-sequence or evolved binaries. The authors find other interesting objects such as cataclysmic variables (d ~ 0.6 - 2 kpc), low-luminosity high-mass stars (likely belonging to the class of Gamma-Cas-like systems, d ~ 1.5 - 7 kpc), T Tauri and Herbig-Ae stars. A handful of extragalactic sources located in the highest Galactic latitude fields could be optically identified. For the 20 fields observed with the EPIC pn camera, the authors have constructed log N(>S) - log S curves in the soft and hard bands. In the soft band, the majority of the sources are positively identified with active coronae and the fraction of stars increases by about one order of magnitude from b = 60 degrees to b = 0 degrees at an X-ray flux of 2 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s. The hard band is dominated by extragalactic sources, but there is a small contribution from a hard Galactic population formed by CVs, HMXB candidates or Gamma-Cas-like systems and by some active coronal stars that are also detected in the soft band. At b = 0 degrees, the surface density of hard sources brighter than 1 x 10<sup>-13</sup> erg/cm<sup>2</sup>/s steeply increases by one order of magnitude from l = 20 degrees to the Galactic center region (l = 0.9 degrees). This HEASARC table contains 739 X-ray sources detected in the 26 different fields observed in this study and listed in Tables 8 - 33, inclusive, of the reference paper. These 739 sources have the best XMM quality, i.e. the summary flag sum_flag which contains information about flags set automatically and manually for a given source is zero, meaning that there are no negative flags for the source detection, have either a 2MASS, USNO, GSC, or SDSS counterpart, whatever the probability of identification is, or have some information via SIMBAD or the authors own imaging or spectroscopic observations. For each X-ray source, its X-ray parameters are summarized, listing the pn count rates, and information on optical and infrared counterparts is provided. The properties of the 26 target fields are given in Table 1 of the reference paper, along with the breakdown of source classes in each field. This table was created by the HEASARC in May 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/553/A12">CDS Catalog J/A+A/553/A12</a>, the 26 files table8.dat to table33.dat, inclusive. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmsscgps.html
bib_reference = 2013A&A...553A..12N
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmsscgps&
tap_tablename = xmmsscgps
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744849
ID = nasa.heasarc/xmmssclwbd
publisher_did = ivo://nasa.heasarc/xmmssclwbd
obs_collection = XMMSSCLWBD
obs_title = XMM-Newton 2XMMi-DR3 Selected Source Detections Catalog
obs_description = The authors have carried out a classification of 4,330 X-ray sources in the 2XMMi-DR3 catalog. The sources were selected under the requirement of being a point source with multiple XMM-Newton observations and at least one detection with a signal-to-noise ratio larger than 20. For about one-third of the sources, the authors are able to obtain reliable source types from the literature. They mostly correspond to various types of stars (611), active galactic nuclei (AGNs, 753), and compact object systems (138) containing white dwarfs, neutron stars, and stellar-mass black holes. The authors find that about 99% of stars can be separated from other source types based on their low X-ray-to-IR flux ratios and frequent X-ray flares. AGNs have remarkably similar X-ray spectra, with the power-law photon index centered around 1.91 +/- 0.31, and their 0.2-4.5 keV flux long-term variation factors have a median of 1.48, with 98.5% being less than 10. In contrast, 70% of compact object systems can be very soft or hard, highly variable in X-rays, and/or have very large X-ray-to-IR flux ratios, separating them from AGNs. Using these results, the authors derive a source type classification scheme to classify the other sources and find 644 candidate stars, 1,376 candidate AGNs, and 202 candidate compact object systems, whose false identification probabilities are estimated to be about 1%, 3%, and 18%, respectively. There are still 320 sources associated with nearby galaxies and 151 in the Galactic plane, which the authors expect to be mostly compact object systems or background AGNs. There are also 100 candidate ultraluminous X-ray sources. They are found to be much less variable than other accreting compact objects. This table contains the list of 19,637 detections of the 4,330 unique X-ray sources which comprise the authors' sample. The list of 4,330 unique X-ray sources and their classifications is also available as the HEASARC XMMSSCLWBS table. This table was created by the HEASARC in October 2012 based on an electronic version of Table 3 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmssclwbd.html
bib_reference = 2012ApJ...756...27L
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmssclwbd&
tap_tablename = xmmssclwbd
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744857
ID = nasa.heasarc/xmmssclwbs
publisher_did = ivo://nasa.heasarc/xmmssclwbs
obs_collection = XMMSSCLWBS
obs_title = XMM-Newton 2XMMi-DR3 Selected Source Classifications Catalog
obs_description = The authors have carried out a classification of 4,330 X-ray sources in the 2XMMi-DR3 catalog. The sources were selected under the requirement of being a point source with multiple XMM-Newton observations and at least one detection with a signal-to-noise ratio larger than 20. For about one-third of the sources, the authors are able to obtain reliable source types from the literature. They mostly correspond to various types of stars (611), active galactic nuclei (AGNs, 753), and compact object systems (138) containing white dwarfs, neutron stars, and stellar-mass black holes. The authors find that about 99% of stars can be separated from other source types based on their low X-ray-to-IR flux ratios and frequent X-ray flares. AGNs have remarkably similar X-ray spectra, with the power-law photon index centered around 1.91 +/- 0.31, and their 0.2-4.5 keV flux long-term variation factors have a median of 1.48, with 98.5% being less than 10. In contrast, 70% of compact object systems can be very soft or hard, highly variable in X-rays, and/or have very large X-ray-to-IR flux ratios, separating them from AGNs. Using these results, the authors derive a source type classification scheme to classify the other sources and find 644 candidate stars, 1,376 candidate AGNs, and 202 candidate compact object systems, whose false identification probabilities are estimated to be about 1%, 3%, and 18%, respectively. There are still 320 sources associated with nearby galaxies and 151 in the Galactic plane, which the authors expect to be mostly compact object systems or background AGNs. There are also 100 candidate ultraluminous X-ray sources. They are found to be much less variable than other accreting compact objects. This table was created by the HEASARC in October 2012 based on an electronic version of Table 4 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmssclwbs.html
bib_reference = 2012ApJ...756...27L
obs_regime = optical
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmssclwbs&
tap_tablename = xmmssclwbs
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744869
ID = nasa.heasarc/xmmstack
publisher_did = ivo://nasa.heasarc/xmmstack
obs_collection = XMMSTACK
obs_title = XMM-Newton Serendipitous Source Catalog from Stacked Observations (4XMM-DR13s)
obs_description = The stacked catalog 4XMM-DR13s has been compiled from 1,688 groups, comprising 9,796 overlapping good-quality XMM-Newton observations. They were selected from the public observations taken between 2000 February 1 and 2022 November 29 which overlap by at least one arcminute in radius. It contains 401,596 unique sources, 310,478 of them multiply observed, with positions and source parameters like fluxes in the XMM-Newton standard energy bands, hardness ratios, quality estimate, and information on inter-observation variability. The parameters are directly derived from the simultaneous fit, and, wherever applicable, additionally calculated for each contributing observation. Exposures that do not qualify for source detection, for example because of a high background level, are used for subsequent PSF photometry: source fluxes and flux-related parameters are derived for them at the source position and extent found during source detection. 4XMM-DR13s lists 1,683,264 individual flux measurements of the 401,596 unique sources. Stacked source detection aims at exploring the multiply observed sky regions and exploit their survey potential, in particular to study the long-term behavior of X-ray emitting sources. It thus makes use of the long(er) effective exposure time per sky area and offers the opportunity to investigate flux variability directly through the source detection process. The main catalog properties are summarized in the table below, the data processing and the stacked source detection are described in the processing summary. To ensure detection quality, background levels are assessed, and event-based astrometric corrections are applied before running source detection. After source detections, problematic detections and detection parameters are flagged by an automated algorithm. All detections are screened visually, and obviously spurious sources are flagged manually. This table contains the parameters of the 401,596 unique sources (provided in this table) derived simultaneously from all of the observations (provided in the associated table of observations referred to as <a href="/W3Browse/xmm-newton/xmmstackob.html">XMMSTACKOB</a>) at the fitted position. The authors referred to the EPIC instruments with the following designations: PN, M1 (MOS1), and M2 (MOS2). The energy bands used in the 4XMM processing were the same as for the 3XMM catalog. The following are the basic energy bands: <pre> 1: 0.2-0.5 keV 2: 0.5-1.0 keV 3: 1.0-2.0 keV 4: 2.0-4.5 keV 5: 4.5-12.0 keV </pre> All-EPIC values cover the energy range 0.2-12.0 keV. The full catalog documentation can be found at <a href="https://xmmssc.aip.de/">https://xmmssc.aip.de/</a>. The following table gives an overview of the statistics of this catalog in comparison with the previous stacked catalogs, 4XMM-DR13s through 3XMM-DR7s: <pre> 4XMM-DR13s 4XMM-DR12s 4XMM-DR11s 4XMM-DR10s 4XMM-DR9s 3XMM-DR7s Number of stacks 1,688 1,620 1,475 1,396 1,329 434 Number of observations 9,796 9,355 8,292 7,803 6,604 789 Time span first to last observation Feb 01, 2000 Feb 01, 2000 Feb 03, 2000 Feb 03, 2000 Feb 03, 2000 Feb 20, 2000 -- Nov 29, 2022 -- Dec 04, 2021 -- Dec 17, 2020 -- Dec 14, 2019 -- Nov 13, 2018 -- Apr 02, 2016 Approximate sky coverage (sq. deg.) 650 625 560 540 485 150 Approximate multiply observed sky area(sq. deg) 420 400 350 335 300 100 Total number of sources 401,596 386,043 358,809 335,812 288,191 71,951 Sources with several contributing observations 310,478 298,626 275,440 256,213 218,283 57,665 Multiply observed sources with flag 0 or 1 262,842 252,445 233,542 216,999 191,497 55,450 Multiply observed with a total detection 251,555 241,880 224,178 208,921 181,132 49,935 likelihood of at least six Multiply observed with a total detection 213,812 205,394 189,556 176,680 153,487 42,077 likelihood of at least ten Total measurements 1,683,264 1,592,263 1,421,966 1,322,299 1,033,264 216,393 Maximum exposures per source 170 155 140 140 103 69 Maximum observations per source 77 70 65 65 40 23 Maximum on-time per source 2.8 Ms 2.8 Ms 2.8 Ms 2.8 Ms 1.9 Ms 1.3 Ms </pre> This database table was last updated by the HEASARC in June 2023. It contains the 4XMM-DR13s source catalog, released by ESA on 2023-06-12 and obtained from the XMM-Newton Survey Science Center Consortium at <a href="https://xmmssc.aip.de/cms/catalogues/4xmm-dr13s/">https://xmmssc.aip.de/cms/catalogues/4xmm-dr13s/</a>. It is <a href="https://xmmssc.aip.de/data/xmmstack_v3.1_4xmmdr13s.fits.gz">also available as a gzipped FITS file</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmstack.html
bib_reference = 2020A&A...641A.137T
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmstack&
tap_tablename = xmmstack
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744877
ID = nasa.heasarc/xmmstackob
publisher_did = ivo://nasa.heasarc/xmmstackob
obs_collection = XMMSTACKOB
obs_title = XMM-Newton Serendipitous Source Catalog from Stacked Observations: Obs. Data
obs_description = The stacked catalog 4XMM-DR13s (<a href="/W3Browse/xmm-newton/xmmstack.html">XMMSTACK</a>) has been compiled from 1,688 groups, comprising 9,796 overlapping good-quality XMM-Newton observations. They were selected from the public observations taken between 2000 February 1 and 2022 November 29 which overlap by at least one arcminute in radius. It contains 401,596 unique sources, 310,478 of them multiply observed, with positions and source parameters like fluxes in the XMM-Newton standard energy bands, hardness ratios, quality estimate, and information on inter-observation variability. The parameters are directly derived from the simultaneous fit, and, wherever applicable, additionally calculated for each contributing observation. Exposures that do not qualify for source detection, for example because of a high background level, are used for subsequent PSF photometry: source fluxes and flux-related parameters are derived for them at the source position and extent found during source detection. 4XMM-DR13s lists 1,683,264 individual flux measurements of the 401,596 unique sources. Stacked source detection aims at exploring the multiply observed sky regions and exploit their survey potential, in particular to study the long-term behavior of X-ray emitting sources. It thus makes use of the long(er) effective exposure time per sky area and offers the opportunity to investigate flux variability directly through the source detection process. The main catalog properties are summarized in the table below, the data processing and the stacked source detection are described in the processing summary. To ensure detection quality, background levels are assessed, and event-based astrometric corrections are applied before running source detection. After source detections, problematic detections and detection parameters are flagged by an automated algorithm. All detections are screened visually, and obviously spurious sources are flagged manually. This table contains the source parameters from the individual observations in the stacked catalog, <a href="/W3Browse/xmm-newton/xmmstack.html">4XMM-DR13s</a>. The parameters are derived from the simultaneous source-detection fit to all stacked observations at the common source position for each observation that covers a source, amounting to 1,683,264 measurements. The mean source parameters from stacked source detection are provided in the associated main table <a href="/W3Browse/xmm-newton/xmmstack.html">4XMM-DR13s</a>, referred to as XMMSTACK. The authors referred to the EPIC instruments with the following designations: PN, M1 (MOS1), and M2 (MOS2). The energy bands used in the 4XMM processing were the same as for the 3XMM catalog. The following are the basic energy bands: <pre> 1: 0.2-0.5 keV 2: 0.5-1.0 keV 3: 1.0-2.0 keV 4: 2.0-4.5 keV 5: 4.5-12.0 keV </pre> All-EPIC values cover the energy range 0.2-12.0 keV. The full catalog documentation can be found at <a href="https://xmmssc.aip.de/">https://xmmssc.aip.de/</a>. The following table gives an overview of the statistics of this catalog in comparison with the previous stacked catalogs, 4XMM-DR13s through 3XMM-DR7s: <pre> 4XMM-DR13s 4XMM-DR12s 4XMM-DR11s 4XMM-DR10s 4XMM-DR9s 3XMM-DR7s Number of stacks 1,688 1,620 1,475 1,396 1,329 434 Number of observations 9,796 9,355 8,292 7,803 6,604 789 Time span first to last observation Feb 01, 2000 Feb 01, 2000 Feb 03, 2000 Feb 03, 2000 Feb 03, 2000 Feb 20, 2000 -- Nov 29, 2022 -- Dec 04, 2021 -- Dec 17, 2020 -- Dec 14, 2019 -- Nov 13, 2018 -- Apr 02, 2016 Approximate sky coverage (sq. deg.) 650 625 560 540 485 150 Approximate multiply observed sky area(sq. deg) 420 400 350 335 300 100 Total number of sources 401,596 386,043 358,809 335,812 288,191 71,951 Sources with several contributing observations 310,478 298,626 275,440 256,213 218,283 57,665 Multiply observed sources with flag 0 or 1 262,842 252,445 233,542 216,999 191,497 55,450 Multiply observed with a total detection 251,555 241,880 224,178 208,921 181,132 49,935 likelihood of at least six Multiply observed with a total detection 213,812 205,394 189,556 176,680 153,487 42,077 likelihood of at least ten Total measurements 1,683,264 1,592,263 1,421,966 1,322,299 1,033,264 216,393 Maximum exposures per source 170 155 140 140 103 69 Maximum observations per source 77 70 65 65 40 23 Maximum on-time per source 2.8 Ms 2.8 Ms 2.8 Ms 2.8 Ms 1.9 Ms 1.3 Ms </pre> This database table was last updated by the HEASARC in December 2023 in order to remove 49 duplicate entries. It contains the 4XMM-DR13s source catalog, released by ESA on 2023-06-12 and obtained from the XMM-Newton Survey Science Center Consortium at <a href="https://xmmssc.aip.de/cms/catalogues/4xmm-dr13s/">https://xmmssc.aip.de/cms/catalogues/4xmm-dr13s/</a>. It is <a href="https://xmmssc.aip.de/data/xmmstack_v3.1_4xmmdr13s.fits.gz">also available as a gzipped FITS file</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmstackob.html
bib_reference = 2020A&A...641A.137T
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmstackob&
tap_tablename = xmmstackob
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744889
ID = nasa.heasarc/xmmt2flare
publisher_did = ivo://nasa.heasarc/xmmt2flare
obs_collection = XMMT2FLARE
obs_title = 2XMM Flares Detected from Tycho-2 Stars
obs_description = This table contains the results from a uniform, large-scale survey of X-ray flare emission, based on the XMM-Newton Serendipitous Source Catalog (2XMM) and its associated data products. This survey comprises both XMM-targeted active stars and those observed serendipitously in the half-degree diameter field-of-view of an observation. The 2XMM Catalog and the associated time-series ('light-curve') data products have been used as the basis for the survey of X-ray flares from cool stars in the Hipparcos Tycho-2 catalog. In addition, the authors have generated and analyzed spectrally-resolved (i.e. hardness-ratio) X-ray light-curves. Where available, they have compared XMM OM UV/optical data with the X-ray light-curves. Their sample contains ~130 flares with well-observed profiles; they originate from ~70 stars. The flares range in duration from ~10<sup>3</sup> to ~10<sup>4</sup> s, have peak X-ray fluxes from ~10<sup>-13</sup> to ~10<sup>-11</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, peak X-ray luminosities from ~10<sup>29</sup> to ~10<sup>32</sup> erg s<sup>-1</sup>, and X-ray energy output from ~10<sup>32</sup> to ~10<sup>35</sup> erg. Most of the ~30 serendipitously-observed (target_flag = 'N') stars have little previously reported information. The hardness-ratio plots clearly illustrate the spectral (and hence inferred temperature) variations characteristic of many flares, and provide an easily accessible overview of the data. In the reference paper, the authors present flare frequency distributions from both target and serendipitous observations. The latter provide an unbiased (with respect to stellar activity) study of flare energetics; in addition, they allow the authors to predict the numbers of stellar flares that may be detected in future X-ray wide-field surveys. The serendipitous sample demonstrates the need for care when calculating flaring rates, especially when normalizing the number of flares to a total exposure time, where it is important to consider both the stars seen to flare and those from which variability was not detected (i.e., measured as non-variable), since in the present survey, the latter outnumber the former by more than a factor of ten. This table was created by the HEASARC in September 2015 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/581/A28">CDS Catalog J/A+A/581/A28</a> files tablec1.dat and tablec2.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmt2flare.html
bib_reference = 2013ApJ...770...98V
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmt2flare&
tap_tablename = xmmt2flare
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744897
ID = nasa.heasarc/xmmvaragn
publisher_did = ivo://nasa.heasarc/xmmvaragn
obs_collection = XMMVARAGN
obs_title = Ensemble X-Ray Variability of AGN in 2XMMi-DR3
obs_description = The X-ray variability of active galactic nuclei (AGN) has been most often investigated with studies of individual, nearby sources, and only a few ensemble analyses have been applied to large samples in wide ranges of luminosity and redshift. In their study, the authors aimed to determine the ensemble variability properties of two serendipitously selected AGN samples extracted from the catalogs of XMM-Newton and Swift (the latter is not included in this table, notice), with redshift between ~ 0.2 and ~ 4.5, and X-ray luminosities, in the 0.5 - 4.5 keV band, between ~ 10<sup>43</sup> erg/s and ~ 10<sup>46</sup> erg/s. They used the structure function (SF), which operates in the time domain, and allows for an ensemble analysis even when only a few observations are available for individual sources and the power spectral density (PSD) cannot be derived. The SF is also more appropriate than fractional variability and excess variance, because these parameters are biased by the duration of the monitoring time interval in the rest-frame, and therefore by cosmological time dilation. The authors find statistically consistent results for the two samples, with the SF described by a power law of the time lag tau, approximately as SF ~ tau<sup>0.1</sup>. They do not find evidence of the break in the SF, at variance with the case of lower luminosity AGNs. They confirm a strong anti-correlation of the variability with X-ray luminosity, accompanied by a change of the slope of the SF. They also find evidence in support of a weak, intrinsic, average increase of X-ray variability with redshift. For XMM, the authors used the version of the Serendipitous Source Catalog then available, namely 2XMMi-DR3, the latest incremental update of the second version of the catalogue, with observations made between 2000 February 3 and 2008 October 08; all datasets were publicly available by 2009 October 31, but not all public observations are included in this catalog. The total area of the catalog fields is ~ 814 deg<sup>2</sup>, but taking account of the substantial overlaps between observations, the net sky area covered independently is ~ 504 deg<sup>2</sup>. The 2XMMi-DR3 catalogue contains 353,191 detections (above the processing likelihood threshold of 6), related to 262,902 unique X-ray sources, therefore a significant number of sources (41,979) have more than one record within the catalog. The selected sources were cross-correlated with the DR7 edition of the SDSS Quasar Catalog (Schneider et al. 2010, AJ, 139, 2360) to obtain redshifts and spectral classifications for the sources. The authors used a maximum distance of 1.5 arcseconds, corresponding to the uncertainty in the X-ray positions, resulting in 412 quasars that were observed by XMM-Newton from 2 to 25 epochs each for a total of 1376 observations. The authors refer to these sources as the XMM-Newton sample. This table was created by the HEASARC in April 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/536/A84">CDS Catalog J/A+A/536/A84</a> file table1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmvaragn.html
bib_reference = 2011A&A...536A..84V
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmvaragn&
tap_tablename = xmmvaragn
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744905
ID = nasa.heasarc/xmmxassist
publisher_did = ivo://nasa.heasarc/xmmxassist
obs_collection = XMM/XAssist
obs_title = XMM-Newton XAssist Source List
obs_description = This database table contains the latest XMM-Newton XAssist source list. XAssist is a NASA-funded project for the automation of X-ray astrophysics, with emphasis on galaxies. It is capable of data reprocessing, source detection, and preliminary spatial, temporal, and spectral analysis for all sources with sufficient counts. The bulk of the system is written in Python, which in turn drives underlying software to process the XMM-Newton data. Pipelines running on XMM-Newton observations of galaxies have generated the source list which comprises this HEASARC table. The pipeline also includes fields requested by users for various projects, most notably observations of a sample of quasars and several deep field observations have been processed. Note that the pipline processing is completely automated; therefore, users should visually inspect the results of any queries. This table was first created by the HEASARC in July 2005 based on the XMM source list available at the XAssist website. In December 2012, the HEASARC switched over to using the "pipeline5" XMM source list. It is updated on a weekly basis when and if the XAssist source list file at <a href="https://asd.gsfc.nasa.gov/xassist/pipeline5/xmm/master_srclist.csv">https://asd.gsfc.nasa.gov/xassist/pipeline5/xmm/master_srclist.csv</a> is updated. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmxassist.html
bib_reference = 2003ASPC..295..465P
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xmmxassist&
tap_tablename = xmmxassist
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744917
ID = nasa.heasarc/xms
publisher_did = ivo://nasa.heasarc/xms
obs_collection = XMS
obs_title = XMM-Newton Medium Sensitivity Survey (XMS) Source Catalog
obs_description = X-ray sources at intermediate fluxes (a few x 10<sup>-14</sup> erg/cm<sup>2</sup>/s) with a sky density of ~ 100 deg<sup>2</sup> are responsible for a significant fraction of the cosmic X-ray background at various energies below 10 keV. The aim of this study is to provide an unbiased and quantitative description of the X-ray source population at these fluxes and in various X-ray energy bands. The XMM-Newton Medium sensitivity Survey (XMS) includes a total of 318 X-ray sources found among the serendipitous content of 25 XMM-Newton target fields. The XMS comprises four largely overlapping source samples selected at soft (0.5 - 2 keV), intermediate (0.5 - 4.5 keV), hard (2 - 10 keV) and ultra-hard (4.5 - 7.5 keV) bands, the first three of them being flux-limited. This study reports on the optical identification of the XMS samples, complete to 85 - 95%. At the flux levels sampled by the XMS, the authors find that the X-ray sky is largely dominated by Active Galactic Nuclei. The fraction of stars in soft X-ray selected samples is below 10%, and only a few per cent for hard X-ray selected samples. They find that the fraction of optically obscured objects in the AGN population stays constant at around 15-20% for soft and intermediate band selected X-ray sources, over 2 decades of flux. The fraction of obscured objects amongst the AGN population is larger (~ 35 - 45%) in the hard or ultra-hard selected samples, and constant across a similarly wide flux range. The distribution in X-ray-to-optical flux ratio is a strong function of the selection band, with a larger fraction of sources with high values in hard selected samples. Sources with X-ray-to-optical flux ratios in excess of 10 are dominated by obscured AGN, but with a significant contribution from unobscured AGN. This table was created by the HEASARC in March 2008 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/476/1191">CDS catalog J/A+A/476/1191</a> files table2.dat and table5.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xms.html
bib_reference = 2007A&A...476.1191B
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xms&
tap_tablename = xms
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744925
ID = nasa.heasarc/xray
publisher_did = ivo://nasa.heasarc/xray
obs_collection = X-ray
obs_title = Master X-Ray Catalog
obs_description = The XRAY database table contains selected parameters from almost all HEASARC X-ray catalogs that have source positions located to better than a few arcminutes. The XRAY database table was created by copying all of the entries and common parameters from the tables listed in the Component Tables section. The XRAY database table has many entries but relatively few parameters; it provides users with general information about X-ray sources, obtained from a variety of catalogs. XRAY is especially suitable for cone searches and cross-correlations with other databases. Each entry in XRAY has a parameter called 'database_table' which indicates from which original database the entry was copied; users can browse that original table should they wish to examine all of the parameter fields for a particular entry. For some entries in XRAY, some of the parameter fields may be blank (or have zero values); this indicates that the original database table did not contain that particular parameter or that it had this same value there. The HEASARC in certain instances has included X-ray sources for which the quoted value for the specified band is an upper limit rather than a detection. The HEASARC recommends that the user should always check the original tables to get the complete information about the properties of the sources listed in the XRAY master source list. This master catalog is updated periodically whenever one of the component database tables is modified or a new component database table is added. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xray.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xray&
tap_tablename = xray
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744933
ID = nasa.heasarc/xrayselbll
publisher_did = ivo://nasa.heasarc/xrayselbll
obs_collection = XRAYSELBLL
obs_title = X-Ray Selected BL Lac Objects Catalog
obs_description = This table contains a catalog of 312 X-ray selected BL Lacertae objects (XBLs), optically identified through the end of 2011. It contains the names from different surveys, equatorial coordinates, redshifts, multi-frequency flux values, and luminosities for each source. In the reference, the different characteristics of these XBLs are statistically investigated (redshift, radio/optical/X-ray luminosities, central black hole (BH) mass, synchrotron peak frequency, broadband spectral indices, optical flux variability). Their values were collected through an extensive bibliographic and database search or calculated by the author. The redshifts range from 0.031 to 0.702 with a maximum of the distribution at z = 0.223. The 1.4-GHz luminosities of XBLs log (nu * L<sub>nu</sub>) ~ 39 - 42 (in units of erg s<sup>-1</sup>), while the optical V and X-ray (0.1-2.4 keV) bands show log (nu * L<sub>nu</sub>) ~ 43 - 46 (same units). The XBL hosts are elliptical galaxies with effective radii r<sub>eff</sub> = 3.26 - 25.40 kpc and ellipticities e = 0.04 - 0.52. Their R-band absolute magnitudes M<sub>R</sub> range from -21.11 mag to -24.86 mag with a mean value of -22.83 mag. The V - R indices of the hosts range from 0.61 to 1.52 and reveal a fourth-degree polynomial relationship with z that enabled the author to evaluate the redshifts of five sources whose V - R indices were determined from the observations, but whose redshifts values are either not found or not confirmed. The XBL nuclei show a wider range of 7.31 mag for M<sub>R</sub>, with the highest luminosity corresponding to M<sub>R</sub> = -27.24 mag. The masses of the central BHs are found in the interval log M<sub>BH</sub> = 7.39 - 9.30 (in units of solar masses), with the maximum of the distribution at log M<sub>BH</sub>/M<sub>sun</sub> = 8.30. The synchrotron peak frequencies are spread over the range log nu<sub>peak</sub> = 14.56 - 19.18 Hz, with a peak of the distribution at log nu<sub>peak</sub> = 16.60 Hz. The broad-band radio-to-optical (alpha<sub>ro</sub>), optical-to-X-ray (alpha<sub>ox</sub>), and radio-to-X-ray (alpha<sub>rx</sub>) spectral indices are distributed in the intervals (0.17, 0.59), (0.56, 1.48), and (0.41, 0.75), respectively. In the optical energy range, the overall flux variability increases, on average, towards shorter wavelengths: Delta(m) = 1.22, 1.50, and 1.82 through the R, V, B bands of the Johnson-Cousins system, respectively. XBLs seem be optically less variable at intranight timescales compared to radio-selected BL Lacs (RBLs). This table was created by the HEASARC in June 2013 based on an electronic version of Table 2 from the reference paper which was obtained form the AJ web site. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xrayselbll.html
bib_reference = 2013AJ....145...31K
obs_regime = x-ray
obs_regime = optical
obs_regime = radio
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xrayselbll&
tap_tablename = xrayselbll
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744941
ID = nasa.heasarc/xrbcat
publisher_did = ivo://nasa.heasarc/xrbcat
obs_collection = XRBs
obs_title = X-Ray Binaries Catalog
obs_description = XRBCAT is a catalog of X-ray binaries, based on the van Paradijs (1996) compilation, and updated by Nick White to include all the new (mostly transient) systems discovered since then up until the last update (see below). The information in XRBCAT is basic and does not attempt to be complete. It includes the name of the source, the position, the pulse or orbital period (if one is known), the object class, a flux (a maximum and, if available, a minimum), and an optical V magnitude (if available). To reference XRBCAT, please use the following acknowledgment: "This paper utilized the HEASARC XRBCAT X-ray Binary catalog". Since it is a very time consuming task to keep track of all the new sources and discoveries, there may be incomplete or missing sources. This catalog was last updated on April 22, 1998. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xrbcat.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xrbcat&
tap_tablename = xrbcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744949
ID = nasa.heasarc/xshzagncxo
publisher_did = ivo://nasa.heasarc/xshzagncxo
obs_collection = XSHZAGNCXO
obs_title = X-Ray Selected High-z AGN Catalog
obs_description = This table contains the results from an analysis of the largest high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) sample to date, combining the Chandra Cosmological Evolution Survey and Chandra Multi-wavelength Project surveys and doubling the previous samples. The sample comprises 209 X-ray-detected AGNs, over a wide range of rest-frame 2-10 keV luminosities log L<sub>X</sub> = 43.3 - 46.0 erg/s. X-ray hardness ratios show that ~39 per cent of the sources are highly obscured, N<sub>H</sub> > 10<sup>22</sup> cm<sup>-2</sup>, in agreement with the ~37 per cent of type-2 AGNs found in this sample based on their optical classification. For ~26 per cent of objects, there are mismatched optical and X-ray classifications. Utilizing the 1/V<sub>max</sub> method, the authors confirm that the comoving space density of all luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~ 7. With a significant sample of AGNs (N = 27) at z > 4, it is found that both source number counts in the 0.5-2 keV band and comoving space density are consistent with the expectation of a luminosity-dependent density evolution (LDDE) model at all redshifts, while they exclude the luminosity and density evolution (LADE) model. The measured comoving space density of type-1 and type-2 AGNs shows a constant ratio between the two types at z > 3. These results for both AGN types at these redshifts are consistent with the expectations of LDDE model. The high-redshift AGN sample used in this work has been selected from the C-COSMOS X-ray catalog, combining the spectroscopic and photometric information available from the identification catalogue of X-ray C-COSMOS sources (Civano et al. 2011, ApJ, 741, 91; 2012, ApJS, 201, 30) and the ChaMP (Chandra Multi-wavelength Project) X-ray catalog using only the 323 ChaMP ObsIDs overlapping with Sloan Digital Sky Survey (SDSS; Richards et al. 2006, AJ, 131, 2766) DR5 imaging. This table was created by the HEASARC in March 2016 based on the CDS catalog J/MNRAS/445/1430 file tablea1.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xshzagncxo.html
bib_reference = 2014MNRAS.445.1430K
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xshzagncxo&
tap_tablename = xshzagncxo
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744957
ID = nasa.heasarc/xteao
publisher_did = ivo://nasa.heasarc/xteao
obs_collection = XTEAO
obs_title = XTEProposalInfo&Abstracts
obs_description = The XTEAO database table contains the official observing program for the Rossi X-Ray Timing Explorer (RXTE) satellite. This list contains the targets recommended by the review panels for the various Cycles of Guest Observer (GO) proposals up to and including Cycle 15. Notice that not all entries in this list will actually be observed, since it includes observations of Targets of Opportunity (ToOs) which may never be triggered. Also note that multiple pointings at a particular target are permitted. This database table was updated by the HEASARC periodically, based on information provided by the RXTE Guest Observer Facility (GOF). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xteao.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xteao&
tap_tablename = xteao
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744965
ID = nasa.heasarc/xteasmlong
publisher_did = ivo://nasa.heasarc/xteasmlong
obs_collection = XTE/ASM
obs_title = XTE All-Sky Monitor Long-Term Observed Sources
obs_description = The XTEASMLONG table was created for the purpose of providing a complete listing of RXTE's All-Sky Monitor (ASM) observations of sources. It is based on information culled from the definitive 1-dwell long-term ASM light curve data products. These data products are available for downloading at <a href="https://heasarc.gsfc.nasa.gov/FTP/xte/data/archive/ASMProducts/definitive_1dwell/lightcurves/">https://heasarc.gsfc.nasa.gov/FTP/xte/data/archive/ASMProducts/definitive_1dwell/lightcurves/</a> The XTEASMLONG table is updated usually every week or two whenever new definitive ASM data products are delivered to the RXTE GOF from MIT where the definitive ASM processing is done. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xteasmlong.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xteasmlong&
tap_tablename = xteasmlong
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744977
ID = nasa.heasarc/xteassagn
publisher_did = ivo://nasa.heasarc/xteassagn
obs_collection = XTEASSAGN
obs_title = XTE All-Sky Slew Survey AGN Catalog
obs_description = This table contains the RXTE All-Sky Slew Survey Catalog of AGN and AGN candidates. The catalog authors compiled a sample of 95 AGNs which were serendipitously detected in the 3-20 keV band at Galactic latitude |b| > 10 degrees during the RXTE Slew Survey (XSS, Revnivtsev et al., CDS Cat. <J/A+A/418/927>), and utilized it to study the statistical properties of the local population of AGN, including the X-ray luminosity function and absorption distribution. They find that among low X-ray luminosity (L<sub>X</sub> < 10<sup>43.5</sup> erg/s) AGN, the ratio of absorbed (characterized by intrinsic absorption in the range 10<sup>22</sup> cm<sup>-2</sup> < N<sub>H</sub> < 10<sup>24</sup> cm<sup>-2</sup>) and unabsorbed (N<sub>H</sub> < 10<sup>22</sup> cm<sup>-2</sup>) objects is 2:1, while this ratio drops to less than 1:5 for higher luminosity AGN. The summed X-ray output of AGN with L<sub>X</sub> > 10<sup>41</sup> erg/s estimated here is smaller than the earlier estimated total X-ray volume emissivity in the local Universe, suggesting that a comparable X-ray flux may be produced together by lower luminosity AGN, non-active galaxies and clusters of galaxies. The authors also presented a sample of 35 AGN candidates, composed of unidentified XSS sources. Most of these AGN belong to the local population (z < 0.1). For each confirmed AGN source, the following information is provided: AGN class, the count rate in two energy bands (3-8 keV and 8-20 keV), the observed and intrinsic (absorption-corrected) luminosity in the 3 - 20keV band, and the intrinsic absorption column density. For the AGN candidates, composed of unidentified XSS sources, the following information is provided: the count rate in two energy bands (3-8 keV and 8-20 keV), the estimated intrinsic absorption column density, and information about RASS Bright Source Catalog and HEAO A-1 X-ray source counterparts. This table was created by the HEASARC in December 2004 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/423/469">CDS Catalog J/A+A/423/469</a>, table1.dat and table2.dat (the corrected version of 01-Dec-2004). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xteassagn.html
bib_reference = 2004A&A...423..469S
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xteassagn&
tap_tablename = xteassagn
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744985
ID = nasa.heasarc/xteasscat
publisher_did = ivo://nasa.heasarc/xteasscat
obs_collection = XTEASSCAT
obs_title = XTE All-Sky Slew Survey Catalog
obs_description = The Rossi X-Ray Timing Explorer (RXTE) All-Sky Survey Slew Catalog contains the results of a serendipitous hard X-ray (3 - 20 keV), nearly all-sky (|b|>10 degrees) survey based on observations by RXTE's Proportional Counter Array (PCA) which were performed during satellite reorientations in the period 1996 - 2002. The survey is 80% (90%) complete to a 4-sigma limiting flux of ~1.8 (2.5)x10<sup>-11</sup> erg/s/cm<sup>2</sup> in the 3 - 20 keV band. The achieved sensitivity in the 3 - 8 keV and 8 - 20 keV subbands is similar to and an order of magnitude higher than that of the previously record HEAO-1 A1 and HEAO-1 A4 all-sky surveys, respectively. A combined 7 x 10<sup>3</sup> square degree area of the sky is sampled to flux levels below 10<sup>-11</sup> erg/s/cm<sup>2</sup> (3 - 20 keV). In total 294 sources are detected and localized to better than ~1 degree; 236 (80%) of these can be confidently associated with a known astrophysical object; 22 of these sources have multiple counterparts (17 have 2 counterparts and 5 have 3 counterparts) with which they have been identified, and as these are listed as separate entries, there are 321 entries in this table. 35 detected sources remain unidentified, although for 12 of these we report a likely soft X-ray counterpart from the ROSAT all-sky survey bright source catalog. Of the reliably identified sources, 63 have a local origin (Milky Way, LMC or SMC), 64 are clusters of galaxies and 100 are active galactic nuclei (AGN). The fact that the unidentified X-ray sources have hard spectra suggests that the majority of them are AGN, including highly obscured ones (hydrogen column density > 10<sup>23</sup> cm<sup>-2</sup>). This dataset enabled the authors to present for the first time a log N - log S diagram for extragalactic sources above 4 x 10<sup>-12</sup> erg/s/cm<sup>2</sup> at 8 - 20 keV. This database table was created by the HEASARC in May 2004 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/418/927">CDS Catalog J/A+A/418/927</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xteasscat.html
bib_reference = 2004A&A...418..927R
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xteasscat&
tap_tablename = xteasscat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845744997
ID = nasa.heasarc/xteindex
publisher_did = ivo://nasa.heasarc/xteindex
obs_collection = RXTE
obs_title = XTE Target Index Catalog
obs_description = The Rossi X-ray Timing Explorer (RXTE) Index table was created for the purpose of providing a concise and easily accessible tracking of RXTE observations, both those already completed and those still scheduled to be done. Each entry in this table corresponds to a specific proposal/target combination or `complete observation', in contrast to the RXTE Master table in which each entry corresponds to a specific proposal/target/ObsID combination or `observing segment'. A complete observation can consist of many (in some cases dozens) observing segments. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xteindex.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xteindex&
tap_tablename = xteindex
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845745005
ID = nasa.heasarc/xtemaster
publisher_did = ivo://nasa.heasarc/xtemaster
obs_collection = RXTE
obs_title = XTE Master Catalog
obs_description = This database table was created for the purpose of providing a comprehensive, accurate, and easily accessible tracking of Rossi X-Ray Timing Explorer (RXTE) pointed observations. It does not list observations made during slews: those are listed in the <a href="/W3Browse/xte/xteslew.html">XTESLEW</a> database table. The XTEMASTER table includes both observations that have already completed and those still scheduled to be done. The XTEMASTER table is regenerated automatically on a quasi-regular basis whenever the RXTE Science Operations Facility (SOF) updates their short-term or long-term schedules and transfers the new version(s) to the HEASARC. At that time, it will also incorporate all the latest information on which targets have been observed (using the daily RXTE ObsCats at <a href="https://heasarc.gsfc.nasa.gov/FTP/xte/timelines/obscat/">https://heasarc.gsfc.nasa.gov/FTP/xte/timelines/obscat/</a>) and which observations have been archived in the public RXTE Data Archive at <a href="https://heasarc.gsfc.nasa.gov/FTP/xte/data/archive/">https://heasarc.gsfc.nasa.gov/FTP/xte/data/archive/</a>. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xtemaster.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xtemaster&
tap_tablename = xtemaster
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
ssa_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/ssa?table=xtemaster&
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845745017
ID = nasa.heasarc/xtemlcat
publisher_did = ivo://nasa.heasarc/xtemlcat
obs_collection = XTEMLCAT
obs_title = XTE Mission-Long Source Catalog
obs_description = This table contains the RXTE Mission-Long Source Catalog. It is generated from the RXTE Mission-Long Data Products, which are based on the standard data products (StdProds) from the PCA and HEXTE, for over 200 sources that have been observed many times with RXTE during its mission. Please refer to the <a href="/docs/xte/recipes/mllc_start.html">RXTE GOF documentation</a> for more information. This database table, first created in April 2008, contains the RXTE Mission-Long Source Catalog created by <a href="/docs/xte/xte_1st.html">RXTE GOF</a>. The catalog is updated by the RXTE GOF on a monthly basis; this HEASARC Browse table will be updated within one week of any updates made by the RXTE GOF. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xtemlcat.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xtemlcat&
tap_tablename = xtemlcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845745025
ID = nasa.heasarc/xteslew
publisher_did = ivo://nasa.heasarc/xteslew
obs_collection = XTESLEW
obs_title = XTE Archived Public Slew Data
obs_description = This database table is a catalog of all the RXTE slew observations and is based on information culled from the RXTE Data Archive's latest top-level FMI (FITS Master Index) file that is created when data products are made publicly available each week. ObsIDs listed in this table are available for download from <a href="https://heasarc.gsfc.nasa.gov/FTP/xte/data/archive/">https://heasarc.gsfc.nasa.gov/FTP/xte/data/archive/</a>. See the parameter 'data_loc' for the relative location of specific ObsIDs. The XTESLEW database table is updated automatically, usually on a weekly basis whenever the RXTE GOF updates the top-level FMI for the public data archive and notifies the HEASARC. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xteslew.html
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xteslew&
tap_tablename = xteslew
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845745033
ID = nasa.heasarc/xwas
publisher_did = ivo://nasa.heasarc/xwas
obs_collection = XWAS
obs_title = XMM-Newton Wide Angle Survey
obs_description = This table contains results from the XMM-Newton Wide Angle Survey (XWAS), viz., a new catalog of almost a thousand X-ray sources that have been spectroscopically identified through optical observations. The sources lie in high-galactic latitude (|b| > 20 degrees) XMM-Newton fields mainly in the southern hemisphere. A sample of X-ray sources detected in 68 XMM-Newton pointed observations was selected for optical multi-fiber spectroscopy. Optical counterparts and corresponding photometry of the X-ray sources were obtained from the SuperCOSMOS Sky Survey. Candidates for spectroscopy were initially selected with magnitudes down to R ~ 21, with preference for X-ray sources having a flux F<sub>0.5-4.5keV</sub> >= 10<sup>-14</sup> erg/s/cm<sup>2</sup>. Optical spectroscopic observations were made using the Two Degree Field of the Anglo-Australian Telescope, and the resulting spectra were classified based on optical emission lines. The authors have identified through optical spectroscopy 940 X-ray sources over a solid angle Omega ~ 11.8 deg<sup>2</sup> of the sky. Source populations in their sample can be summarized as 65% broad-line active galactic nuclei (BLAGN), 16% narrow emission-line galaxies (NELGs), 6% absorption-line galaxies (ALGs) and 13% stars. An active nucleus is also likely to be present in the large majority of the X-ray sources spectroscopically classified as NELGs or ALGs. Optical images are available for all of the XWAS fields in the SuperCOSMOS Sky Survey (Hambly et al., 2001, MNRAS, 326, 1279). This table was created by the HEASARC in May 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/557/A123">CDS Catalog J/A+A/557/A123</a> file xwas_cat.dat. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/xwas.html
bib_reference = 2013A&A...557A.123E
obs_regime = x-ray
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=xwas&
tap_tablename = xwas
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845745045
ID = nasa.heasarc/zcat
publisher_did = ivo://nasa.heasarc/zcat
obs_collection = CFAZ
obs_title = CfA Redshift Catalog (June 1995 Version)
obs_description = The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues. The original HEASARC version was constructed based on an earlier version of the catalog and was released on November 15, 1996. The HEASARC created the current version of ZCAT in February 2001 based on CDS/ADC Catalog VII/193, "The CfA Redshift Catalogue", Version June 1995, tables <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/193/zcat.dat">https://cdsarc.cds.unistra.fr/ftp/cats/VII/193/zcat.dat</a> and zbig.dat. The former table contains the main body of the CFA Redshift Catalog (57536 objects) and entries from it are distinguishable in the current database by having either listed radial velocity values but not redshifts or neither, while the latter table contains 1202 high-redshift galaxies (distinguishable in the current database by their having listed redshift values but not radial velocities). This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/zcat.html
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=zcat&
tap_tablename = zcat
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845745053
ID = nasa.heasarc/zwclusters
publisher_did = ivo://nasa.heasarc/zwclusters
obs_collection = Zwicky
obs_title = Zwicky Clusters
obs_description = The ZWCLUSTERS database is based upon the Catalogue of Zwicky Clusters of Galaxies. The Zwicky clusters were identified by F. Zwicky in 560 POSS fields. They are rich clusters, each having at least 50 members within 3 magnitudes of the brightest member. This is a service provided by NASA HEASARC .
obs_description_url = https://heasarc.gsfc.nasa.gov/W3Browse/all/zwclusters.html
bib_reference = 1961CGCG..C......0Z
obs_regime = optical
cs_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=zwclusters&
tap_tablename = zwclusters
tap_service_url = https://heasarc.gsfc.nasa.gov/xamin/vo/tap
client_category = Catalog/nasa.heasarc
TIMESTAMP = 1714845745069
ID = nexsci.ipac/exoplanetarchive/confirmedplanets
publisher_did = ivo://nexsci.ipac/exoplanetarchive/confirmedplanets
obs_collection = ConfirmedPlanets
obs_title = NASA Exoplanet Archive
obs_description = Exoplanet and host star published parameters.
obs_description_url = https://exoplanetarchive.ipac.caltech.edu/
cs_service_url = https://exoplanetarchive.ipac.caltech.edu/cgi-bin/nstedAPI/nph-nstedAPI?table=exoplanets&format=vo&
TIMESTAMP = 1714845735469
ID = ov-gso/P/COMPTEL
hips_initial_fov = 58.6323014283504
hips_initial_ra = 270.0
hips_initial_dec = -25.0
creator_did = ivo://ov-gso/P/COMPTEL
hips_creator = D. Paradis (IRAP/CADE)
obs_title = COMPTEL 0.8-30 MeV
obs_collection = COMPTEL 0.8-30 MeV
obs_description = Allsky survey (0.8-30 MeV)obtained with the imaging Gamma-ray Telescope COMPTEL aboard Nasa's Compton Gamma Ray Observatory. Units of the map are cts/s/cm^2/sr and the angular resolution is of the order of 1 degree. Healpix map built by D. Paradis (IRAP/CADE)
obs_copyright = IRAP/CADE
obs_copyright_url = http://cade.irap.omp.eu
t_min = 48351.0
t_max = 51699.0
obs_regime = Gamma-ray
em_min = 4.133e-14
em_max = 1.55e-11
hips_builder = Aladin/HipsGen v10.131
hips_version = 1.4
hips_release_date = 2019-10-08T12:51Z
hips_frame = galactic
hips_order = 3
hips_order_min = 0
hips_tile_width = 32
hips_service_url = http://cade.irap.omp.eu/documents/Ancillary/4Aladin/COMPTEL
hips_status = public master unclonable
hips_tile_format = png jpeg fits
hips_pixel_bitpix = -32
hips_pixel_cut = 1.0E-7 0.002
hips_data_range = -0.01653 0.04964
hips_pixel_scale = 0.01431
dataproduct_type = image
moc_sky_fraction = 1
hips_estsize = 1149036
hips_creation_date = 2019-01-14T14:10Z
hipsgen_date = 2019-01-14T14:10Z
hipsgen_params = in=/Users/paradis/For_Aladin/COMPTEL_1_256.fits out=/Users/paradis/For_Aladin/COMPTEL/ id=ivo://ov-gso/P/COMPTEL/ -blank=-32768 "pixelcut=1E-7 0.002"
hipsgen_date_1 = 2019-01-14T14:10Z
hipsgen_params_1 = in=/Users/paradis/For_Aladin/COMPTEL_1_256.fits out=/Users/paradis/For_Aladin/COMPTEL/ id=ivo://ov-gso/P/COMPTEL/ -blank=-32768 "pixelcut=1E-7 0.002"
hipsgen_date_2 = 2019-01-14T14:11Z
hipsgen_params_2 = in=/Users/paradis/For_Aladin/COMPTEL_1_256.fits out=/Users/paradis/For_Aladin/COMPTEL/ id=ivo://ov-gso/P/COMPTEL/ -blank=-32768 "pixelcut=1E-7 0.002" jpeg
hipsgen_date_3 = 2019-10-03T08:56Z
hipsgen_params_3 = in=/data1/ancillary/missions/COMPTEL/HiPS creator_did=ivo://ov-gso/P/COMPTEL out=/data1/ancillary/missions/COMPTEL/HiPS "hips_pixel_cut=1.0E-7 0.002" -blank=-32768 UPDATE
hipsgen_date_4 = 2019-10-03T11:41Z
hipsgen_params_4 = in=/data1/ancillary/missions/COMPTEL/HiPS creator_did=ivo://ov-gso/P/COMPTEL out=/data1/ancillary/missions/COMPTEL/HiPS "hips_pixel_cut=1.0E-7 0.002" -blank=-32768 UPDATE
hipsgen_date_5 = 2019-10-03T12:16Z
hipsgen_params_5 = in=/data1/ancillary/missions/COMPTEL/HiPS creator_did=ivo://ov-gso/P/COMPTEL out=/data1/ancillary/missions/COMPTEL/HiPS "hips_pixel_cut=1.0E-7 0.002" -blank=-32768 UPDATE
hipsgen_date_6 = 2019-10-08T12:51Z
hipsgen_params_6 = in=/data1/ancillary/missions/COMPTEL/HiPS creator_did=ivo://ov-gso/P/COMPTEL out=/data1/ancillary/missions/COMPTEL/HiPS "hips_pixel_cut=1.0E-7 0.002" -blank=-32768 UPDATE
hips_service_url_1 = https://alasky.cds.unistra.fr/IRAP/ov-gso_P_COMPTEL
hips_status_1 = public mirror unclonable
hips_service_url_2 = https://alaskybis.cds.unistra.fr/IRAP/ov-gso_P_COMPTEL
hips_status_2 = public mirror unclonable
client_category = Image/Gamma-ray
client_application = AladinDesktop
moc_type = stmoc
moc_time_order = 25
moc_time_range = 1
moc_order = 7
obs_initial_ra = 270.0
obs_initial_dec = -25.0
obs_initial_fov = 0.4580648549089874
TIMESTAMP = 1709810566665
ID = padc.obspm.maser/voyager_pra/epn/epn_core
publisher_did = ivo://padc.obspm.maser/voyager_pra/epn/epn_core
obs_collection = Voyager PRA
obs_title = Voyager PRA Datasets
obs_description = Voyager PRA (Planetary Radio Astronomy) Datasets catalog. The dataset are originally published by several data centers: NASA/PDS, NASA/NSSDC, NASA/GSFC, Univ. Iowa and CNES/SERAD.
obs_description_url = http://voparis-tap-maser.obspm.fr/tableinfo/voyager_pra.epn_core
tap_service_url = http://voparis-tap-maser.obspm.fr/tap
tap_tablename = voyager_pra.epn_core
client_category = Solar system/Tabular data
client_application = AladinDesktopBeta>=10.040 AladinDesktop>=11.125
TIMESTAMP = 1714845732273
ID = padc.obspm.planeto/spectro_stars/q/epn_core
publisher_did = ivo://padc.obspm.planeto/spectro_stars/q/epn_core
obs_collection = spectro_stars.ep
obs_title = Stellar spectra
obs_description = The stellar spectra service is a compilation of several libraries distributed by large observatories, which are intended to calibrate telescopic observations. It currently provides access to two libraries of reference stars distributed by ESO (composite spectra: https://www.eso.org/sci/observing/tools/standards/IR_spectral_library.html) and NASA IRTF (observations from SpeX: http://irtfweb.ifa.hawaii.edu/~spex/IRTF_Spectral_Library/References_files/All.html).
obs_description_url = http://voparis-tap-planeto.obspm.fr/tableinfo/spectro_stars.epn_core
obs_regime = infrared
obs_regime = optical
obs_regime = ultraviolet
tap_service_url = http://voparis-tap-planeto.obspm.fr/tap
tap_tablename = spectro_stars.epn_core
client_category = Solar system/Tabular data
client_application = AladinDesktopBeta>=10.040 AladinDesktop>=11.125
TIMESTAMP = 1714845752065
ID = pds-ppi/cassini_caps_fitted_parameters/ppi/epn_core
publisher_did = ivo://pds-ppi/cassini_caps_fitted_parameters/ppi/epn_core
obs_collection = CO-CAPS-FIT
obs_title = Cassini CAPS Moments Data Collection
obs_description = This data collection contains fits (both good and bad) that were found during R. J. Wilson et al's grant from NASA's Cassini Data Analysis Program (NNX12AG90G).
obs_description_url = https://vo-pds-ppi.igpp.ucla.edu/tableinfo/cassini_caps_fitted_parameters.epn_core
bib_reference = 2000asqu.book.....C
obs_regime = optical
tap_service_url = https://vo-pds-ppi.igpp.ucla.edu/tap
tap_tablename = cassini_caps_fitted_parameters.epn_core
client_category = Solar system/Tabular data
client_application = AladinDesktopBeta>=10.040 AladinDesktop>=11.125
TIMESTAMP = 1714845731745
ID = wfau.roe.ac.uk/galexgr6-dsa
publisher_did = ivo://wfau.roe.ac.uk/galexgr6-dsa
obs_title = GALEX Release 6
obs_description = The Galaxy Evolution Explorer (GALEX) satellite is a NASA mission led by the California Institute of Technology to investigate how star formation in galaxies evolved from the early Universe up to the present. GALEX uses microchannel plate detectors to obtain direct images in the near-UV (NUV) and far-UV (FUV) and a grism to disperse light for low resolution spectroscopy
obs_description_url = http://galex.stsci.edu/GR6/
obs_regime = uv
cs_service_url = http://wfaudata.roe.ac.uk/galexgr6-dsa/DirectCone?DSACAT=GALEXGR6&DSATAB=photoobjall&
TIMESTAMP = 1714845742185
ID = wfau.roe.ac.uk/wise-dsa
publisher_did = ivo://wfau.roe.ac.uk/wise-dsa
obs_title = WISE (Wide-field Infrared Survey Explorer)
obs_description = NASA's Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) mapped the sky at 3.4, 4.6, 12, and 22 μm (W1, W2, W3, W4) in 2010 with an angular resolution of 6.1", 6.4", 6.5", & 12.0" in the four bands. WISE achieved 5Ï? point source sensitivities better than 0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic in the four bands. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodiacal background.
obs_description_url = http://wise2.ipac.caltech.edu/docs/release/allsky/
obs_regime = infrared
cs_service_url = http://wfaudata.roe.ac.uk/wise-dsa/DirectCone?DSACAT=WISE&DSATAB=wise_allskysc&
TIMESTAMP = 1714845743141
