- ID:
- ivo://nasa.heasarc/wisehspcat
- Title:
- 2WHSP Catalog of High Synchrotron Peaked Blazars and Candidates
- Short Name:
- WISEHSPCAT
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
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Search Results
- ID:
- ivo://nasa.heasarc/warps
- Title:
- Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)
- Short Name:
- ROSAT/WARPS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
- ID:
- ivo://nasa.heasarc/warps2
- Title:
- Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog
- Short Name:
- WARPS2
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
- ID:
- ivo://nasa.heasarc/wibrals
- Title:
- WISE Blazar-like Radio-Loud Source (WIBRaLS) Catalog
- Short Name:
- WIBRALS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 (µm). 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 .
- ID:
- ivo://nasa.heasarc/w2ragncat
- Title:
- WISE/2MASS/RASS (W2R) AGN Sample Catalog
- Short Name:
- W2RAGNCAT
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
- ID:
- ivo://nasa.heasarc/skyview/wise
- Title:
- WISE 3\.4 Micron All-Sky Survey>: All-WISE data release
- Short Name:
- WISE
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- From the <a href="https://wise2.ipac.caltech.edu/docs/release/allsky">WISE mission site:</a>. <hr> 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. <p> 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 <hr> <p> 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.
- ID:
- ivo://nasa.heasarc/wmapcmbfps
- Title:
- WMAP Nine-Year CMB-Free QVW Point Source Catalog
- Short Name:
- WMAPCMBFPS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
- ID:
- ivo://nasa.heasarc/wmapptsrc
- Title:
- WMAP Nine-Year Five-Band Point Source Catalog
- Short Name:
- WMAPPTSRC
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
- ID:
- ivo://nasa.heasarc/skyview/wmap
- Title:
- WMAP Nine Year Galaxy Removed
- Short Name:
- WMAP
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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. <p> The original data are available at the <https://lambda.gsfc.nasa.gov>LAMBDA archive</a>. <p> 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. </p> Provenance: WMAP Mission/LAMBDA archive. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/wmapitnpts
- Title:
- WMAP 7-Year Internal Templates and Needlets New Source Catalog
- Short Name:
- WMAPITNPTS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
