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Merged Catalog of Reflection Nebulae
Several catalogs of reflection nebulae have been merged to create a uniform catalog of 913 objects. It contains revised coordinates, cross-identifications of nebulae and stars, as well as identifications with IRAS point sources. The HEASARC has endeavored to render all identifications of the nebulae in the various catalogs according to the styles recommended by the Dictionary of Nomenclature of Celestial Objects. This table was created by the HEASARC in October 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/399/141">CDS Catalog J/A+A/399/141</a> file table1.dat. This is a service provided by NASA HEASARC .
Washington Double Star Catalog
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 .
Spitzer Extragalactic Representative Volume Survey ELAIS-S1 2-band Catalog
The "Spitzer Extragalactic Representative Volume Survey" (SERVS) Exploration Science program conducted deep IRAC 3.6 and 4.5 micron observations of five extragalactic fields (ELAIS-N1, Lockman Hole, XMM, ELAIS-S1, and CDFS).The 2-band high reliability catalogs are matched [3.6] and [4.5] catalogs, with the low coverage areas near the edges of the survey omitted (POLY_12=1). These catalogs should be used if you are using SERVS to select your sample, as objects in this catalog should be highly reliable (>99.9%). To appear in the catalog objects must appear in both bands, and the detection in one band must be > 10-sigma in CSNR, where CSNR is the coverage-weighted signal-to-noise ratio.
ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog
The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L<sub>X</sub>-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L<sub>H-alpha</sub>/L<sub>bol</sub>. The quantities L<sub>H-alpha</sub>/L<sub>bol</sub> and L<sub>X</sub>/L<sub>bol</sub> are linearly related below L<sub>X</sub>/L<sub>bol</sub> ~ 3 x 10<sup>-4</sup>, while L<sub>H-alpha</sub>/L<sub>bol</sub> appears to turn over at larger L<sub>X</sub>/L<sub>bol</sub> values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age. This table was created by the HEASARC in January 2009 based on the electronic version of Tables 2 and 3 from the reference paper which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .
M 31 Bulge Chandra X-Ray Point Source Catalog
The authors explore the population of X-ray point sources in the bulge of M 31 so as to contrast properties of various subpopulations, such as persistent and transient sources and primordial LMXBs and dynamically formed ones. Based on the data from 26 archival Chandra ACIS observations with aim-points within 10 arcminutes of the center of M 31 (J2000 coordinates of 00:42:44.31, +41:16:09.4), the authors study the source content and properties of various subpopulations of X-ray sources to a maximum distance of 12 arcminutes from the center of M 31. To a limiting luminosity of ~10<sup>35</sup> erg s<sup>-1</sup>, the authors find 263 X-ray point sources, with ~1/3 of these being background galaxies. A study of the spatial distribution and the luminosity function of the X-ray sources shows that the distribution of primordial LMXBs is consistent with the distribution of the K-band light and that their luminosity function flattens below ~10<sup>37</sup> erg s<sup>-1</sup> to the dN/dL ~ L<sup>-1</sup> law in agreement with the behavior found earlier for LMXBs in the Milky Way and in Cen A. Within a radius of 12 arcminutes, the luminosity function is independent of distance to the center of M 31, in contrast to earlier Chandra studies. The LMXBs located in globular clusters and within ~1 arcminute from the center of M 31 are presumably created via dynamical interactions. The dynamical origin of the r < 1 arcminute sources is strongly suggested by their radial distribution which follows the rho<sub>*</sub><sup>2</sup> profile rather than the K-band light distribution. Their luminosity function shows a prominent fall-off below log(L<sub>X</sub>) <~ 36.5. Although the statistics are insufficient to claim a genuine low-luminosity cut-off in the luminosity function, the best fit power-law with a slope of -0.6 +/- 0.2 is significantly flatter than the dN/dL ~ L<sup>-1</sup> law. The authors also searched for transients and found 28 sources that varied by a factor larger than 20. Their spatial distribution follows the distribution of the persistent LMXBs within the accuracy allowed by the limited number of transients. This HEASARC table was created in March 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/468/49">CDS catalog J/A+A/468/49</a> file table2.dat. This is a service provided by NASA HEASARC .
SpIES 3.6 micron-only Catalog
The Spitzer IRAC Equatorial Survey (SpIES) is a large-area survey of 115 sq. degrees in the Equatorial SDSS Stripe 82 field. SpIES achieves 5 sigma depths of 6.13 microJy (21.93 AB magnitude) and 5.75 microJy (22.0 AB magnitude) at 3.6 and 4.5 microns, respectively.The 3.6 micron catalog contains the 6.1 million sources that are only detected at 3.6 microns, the 4.5 micron catalog contains the 6.4 million sources that are only detected at 4.5 microns, and the Dual-band catalog contains the 5.4 million sources that are detected in both bands.
Westerbork in the Southern Hemisphere (WISH) Source Catalog
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 .
Ritter Cataclysmic Binaries Catalog (7.21 Edition)
This HEASARC database table contains information on cataclysmic binaries only, as taken from the Catalog of Cataclysmic Binaries, Low-Mass X-ray Binaries, and Related Objects (7th Edition, Release 7.21, March 2014) of Ritter & Kolb. The complete catalog lists coordinates, apparent magnitudes, orbital parameters, stellar parameters of the components, and other characteristic properties of 1166 cataclysmic binaries, 105 low-mass X-ray binaries, and 500 related objects with known or suspected orbital periods. The HEASARC has for simplicity split this catalog into three Browse database tables, one for each class of objects: the present table (RITTERCV) containing the cataclysmic binaries' data, a second one (<a href="/W3Browse/star-catalog/ritterlmxb.html">RITTERLMXB</a>) containing the low-mass X-ray binaries' data, and a third one (<a href="/W3Browse/star-catalog/ritterrbin.html">RITTERRBIN</a>) containing the related binaries' data. The literature published before 1 January 2014 has, as far as possible, been taken into account. Cataclysmic binaries are semi-detached binaries consisting of a white dwarf (or a white dwarf precursor) primary and a low-mass secondary which is filling its critical Roche lobe. The secondary is not necessarily unevolved, it may even be a highly evolved star, as, for example, in the case of the AM CVn-type stars. This table was last updated by the HEASARC in April 2014 based on the cbdata.dat file from the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/B/cb">CDS Catalog B/cb</a>. This is a service provided by NASA HEASARC .
XMM-Newton 2XMMi-DR3 Selected Source Detections Catalog
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 .
M 83 XMM-Newton X-Ray Point Source Catalog
This database table contains results obtained from the analysis of three XMM-Newton observations of the grand-design barred spiral galaxy M 83. The aims of this study were to study the X-ray source populations in M 83 and to calculate the X-ray luminosity functions of X-ray binaries for different regions of the galaxy. The authors detected 189 sources in the XMM-Newton field of view in the energy range of 0.2-12 keV. They constrained their nature by means of spectral analysis, hardness ratios, studies of the X-ray variability, and cross-correlations with catalogs in X-ray, optical, infrared, and radio wavelengths. The authors identified and classified 12 background objects, five foreground stars, two X-ray binaries, one supernova remnant candidate, one super-soft source candidate and one ultra-luminous X-ray source. Among these sources, they classified for the first time three active galactic nuclei (AGN) candidates. the authors derived X-ray luminosity functions for the X-ray sources in M 83 in the 2-10 keV energy range, within and outside the D<sub>25</sub> ellipse, correcting the total X-ray luminosity function for incompleteness and subtracting the AGN contribution. The X-ray luminosity function inside the D25 ellipse is consistent with that previously observed by Chandra. The Kolmogorov-Smirnov test shows that the X-ray luminosity function of the outer disc and the AGN luminosity distribution are uncorrelated with a probability of ~99.3%. The authors also found that the X-ray sources detected outside the D<sub>25</sub> ellipse and the uniform spatial distribution of AGNs are spatially uncorrelated with a significance of 99.5%. They interpret these results as an indication that part of the observed X-ray sources are X-ray binaries in the outer disc of M 83. The authors analyzed the public archival XMM-Newton data of M 83 (PIs: Watson, Kuntz). Three observations were analyzed, one pointing at the center of the galaxy (obs.1) and two in the south, which covered the outer arms with a young population of stars discovered with GALEX. The details of these observations are given in Table 1 of the reference paper (summarized below): <pre> EPIC EPIC EPIC No ObsID Date RA DE PN MOS1 MOS2 Mode F Texp F Texp F Texp PN MOS 1 0110910201 2003-01-27 13:37:05.16 -29:51:46.1 t 21.2 m 24.6 m 24.6 EFF FF 2 0503230101 2008-01-16 13:37:01.09 -30:03:49.9 m 15.4 m 19.0 m 19.0 EFF FF 3 0552080101 2008-08-16 13:36:50.87 -30:03:55.2 m 25.0 m 28.8 m 28.8 EFF FF </pre> where F is the filter (t for thin, m for medium), T<sub>exp</sub> is the exposure time in ks, EFF = extended full frame imaging mode, and FF = full frame imaging mode. This table was created by the HEASARC in April 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/553/A7">CDS Catalog J/A+A/553/A7</a> files tableb1.dat and tableb2.dat. This is a service provided by NASA HEASARC .
HerMES Band-merged Catalog (24 micron positions)
The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme (KPGT_soliver1) designed to map a set of nested fields totalling 380 sq. deg. Fields range in size from 0.01 to 20 sq. deg., using SPIRE at 250, 350 and 500 microns. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution.
Chandra Deep Field North 2-Megasecond Catalog
The Chandra Deep Field North (CDFN) 2-Megasecond Catalog contains the point sources found in the ~2 Megasecond (Ms) exposure of the Chandra Deep Field North, currently the deepest X-ray observation of the universe in the 0.5 -8.0 keV band. Five hundred and three (503) X-ray sources were detected over an ~448 square arcminute area in up to seven X-ray bands. Twenty (20) of these X-ray sources lie in the central ~5.3 square arcminute Hubble Deep Field North (13600 (+3800,-3000) sources/deg<sup>2</sup>). The on-axis sensitivity limits are ~2.5x10<sup>-17</sup> ergs/cm<sup>2</sup>/s (0.5 - 2.0 keV) and 1.4x10<sup>-16</sup> ergs/cm<sup>2</sup>/s (2 - 8 keV). Source positions are determined using matched-filter and centroiding techniques; the median positional uncertainty is ~0.3". The X-ray colors of the detected sources indicate a broad variety of source types, although absorbed AGN (including a small number of possible Compton-thick sources) are clearly the dominant type. The average backgrounds in the 0.5 - 2.0 keV and 2 - 8 keV bands are 0.056 and 0.135 counts Ms<sup>-1</sup> pixel<sup>-1</sup>, respectively. The background count distributions are very similar to Poisson distributions. This 2 Ms exposure is approximately photon limited in all seven X-ray bands for regions close to the aim point. This observation does not suffer from source confusion within ~6 arcminutes of the aim point. This table was created by the HEASARC in April 2004 based on CDS catalog table J/AJ/126/539/cdfn.dat. This is a service provided by NASA HEASARC .
WMAP Nine-Year CMB-Free QVW Point Source Catalog
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 .
Bolocam Galactic Plane Survey Catalog v1
The Version 2 release (hereafter v2) of the BGPS data includes images and a catalog. It is described in Ginsburg et al (2013).The new images have improved fidelity and more uniform noise. The fields include all those in the original v1 release and some new data. There are new fields included in the BGPS v2 release, primarily in the outer galaxy but including some expansions in the inner galaxy. These include M17, IRAS 22172, a significant expansion in l and b around the l=110 region, Mon R2, NGC 2264, parts of the Orion A and B clouds, Sharpless 235, and scattered IRAS+CO selected fields at longitude 119, 123, 126, 129, 154, 169, 181, 182, 195, 201, and 217. IRSA provides a coverage map.There is a new catalog associated with the v2 images. The sources were extracted using Bolocat with parameters set in the same way as for the v1 catalog. There are many sources in v1 that are not in v2 and vice-versa. These discrepancies occur primarily for faint sources with low signal-to-noise. Objects in both catalogs are likely to be real since catalog parameters were selected to minimize false positives. Changing the quality of the images and the structure of the noise highlights some new objects and obscures others. The v2 catalog has about a 75% overlap with the v1 catalog. The differences are explored in more detail in the Ginsburg et al (2013).The flux calibration offset identified in the version 1 data is now understood. The version 2 data are brighter, on average, by approximately a factor 1.5, but the factor varies from source to source. The v2 catalog should be used instead of the v1 catalog. The source of the error was the incorrect application of a flux calibration solution.Contreras et al (2013) noted a 4.7 arcsecond offset between the BGPS v1 catalog and the ATLASGAL catalog. We believe this is caused by an offset of that magnitude (~3-4 arcseconds) in a few fields that have an inordinate number of sources extracted; the pointing accuracy in the vast majority of the BGPS fields, based on a comparison to Herschel Hi-Gal images, is better than 4 arcseconds, but the mean offset is within 2 arcseconds of zero.
Swift Gamma Ray Bursts Catalog
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 .
Spitzer Wide-area InfraRed Extragalactic Survey ELAIS-N1 MIPS 70 micron Catalog
The Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), the largest Spitzer Legacy program, is a wide-area, imaging survey to trace the evolution of dusty, star-forming galaxies, evolved stellar populations, and AGN as a function of environment, from redshifts z~3 to the current epoch. SWIRE surveys 6 high-latitude fields, totaling ~50 sq. deg. in all 7 Spitzer bands: 3.6, 4.5, 5.8, and 8 microns with IRAC and 24, 70, and 160 microns with MIPS (Lonsdale et al. 2003). The SWIRE Legacy Extragalactic Source Catalogs will eventually contain in excess of 2 million IR-selected galaxies, from those dominated by the light of stellar populations detected primarily by IRAC, to starbursts, ultra-luminous infrared galaxies and AGN detected also by MIPS.
AEGIS-X Deep Survey Chandra X-Ray Point Source Catalog
This table is based on the results of deep Chandra imaging of the central region of the Extended Groth Strip, the AEGIS-X Deep (AEGIS-XD) survey. When combined with previous Chandra observations of a wider area of the strip, AEGIS-X Wide (AEGIS-XW), these provide data to a nominal exposure depth of 800ks in the three central ACIS-I fields, a region of approximately 0.29 deg<sup>2</sup>. This is currently the third deepest X-ray survey in existence; a factor ~2-3 shallower than the Chandra Deep Fields (CDFs), but over an area ~3 times greater than each CDF. This table contains a catalog of 937 point sources detected in the deep Chandra observations, along with identifications of the X-ray sources from deep ground-based, Spitzer, GALEX, and Hubble Space Telescope imaging. Using a likelihood ratio analysis, the authors associate multiband counterparts for 929/937 of their X-ray sources, with an estimated 95% reliability,making the identification completeness approximately 94% in a statistical sense. Reliable spectroscopic redshifts for 353 of the X-ray sources are available predominantly from Keck (DEEP2/3) and MMT Hectospec, so the current spectroscopic completeness is ~38%. For the remainder of the X-ray sources, the authors compute photometric redshifts based on multiband photometry in up to 35 bands from the UV to mid-IR. Particular attention is given to the fact that the vast majority of the X-ray sources are active galactic nuclei and require hybrid templates. The photometric redshifts have a mean accuracy sigma = 0.04 and an outlier fraction of approximately 5%, reaching sigma = 0.03 with less than 4% outliers in the area covered by CANDELS. The new AEGIS-XD Chandra data were taken at three nominal pointing positions, which the authors have designated AEGIS-1, AEGIS-2, and AEGIS-3. These observations were all taken in the time period 2007 December 11 to 2009 June 26 using the ACIS-I instrument. The centers of the 3 AEGIS fields correspond fairly closely to those of the EGS-3, EGS-4, and EGS-5 fields of Laird et al. (2009, ApJS, 180, 102). The Rainbow Cosmological Surveys Database (<a href="http://rainbowx.fis.ucm.es/Rainbow_Database/Home.html">http://rainbowx.fis.ucm.es/Rainbow_Database/Home.html</a>; see Section 4 of the reference paper for more details) contains many multiwavelength photometric datasets giving information on optical and infrared sources in these fields. The characteristics of these datasets are given in Table 7 of the reference paper. This table was created by the HEASARC in February 2016 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/220/10">CDS catalog J/ApJS/220/10</a> files table11.dat, table12.dat, table13.dat, table14.dat and table15.dat. This is a service provided by NASA HEASARC .
Faust Far-UV Point Source Catalog
This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10<sup>-14</sup> ergs/s/cm<sup>2</sup>/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts). This catalog was created at the HEASARC in September 1998 based on CDS/ADC Catalog J/ApJS/96/461. This is a service provided by NASA HEASARC .
GLIMPSE Proper Catalog
The GLIMPSE Proper project re-images about 43 square degrees of the Galactic center to measure the proper motions of millions of sources within 5 degrees of the Galactic center over the last decade.
VLA A2390 Cluster of Galaxies 1.4-GHz Source Catalog
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 .
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.