- ID:
- ivo://nasa.heasarc/mashpncat
- Title:
- MASH Catalogs of MASH Planetary Nebulae
- Short Name:
- MASHPNCAT
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The first part of the Macquarie/AAO/Strasbourg H-alpha Planetary Nebula Catalog (MASH) contains 903 new true, likely and possible Galactic planetary nebulae (PNe) discovered in the AAO/UKST H-alpha survey of the southern Galactic Plane. The combination of depth, resolution, uniformity, and areal coverage of the H-alpha survey has opened up an hitherto unexplored region of parameter space permitting the detection of this significant new PN sample. The second part, MASH-II, consists of over 300 true, likely and possible new Galactic PNe found after re-examination of the entire AAO/UKST H-alpha survey of the Southern Galactic Plane in digital form. Over 240 of these new candidates were confirmed as bona fide PNe on the basis of spectroscopic observations. This HEASARC table contains all 1238 objects from the combined MASH and MASH-II catalogs. This table was created by the HEASARC in April 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/V/127A">CDS Catalog V/127A</a> files mash1.dat and mash2.dat. This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/moxc
- Title:
- Massive Star-Forming Regions Omnibus X-Ray Catalog
- Short Name:
- MOXC
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the Massive Star-forming Regions (MSFRs) Omnibus X-ray Catalog (MOXC), a compendium of X-ray point sources from Chandra/ACIS observations of a selection of MSFRs across the Galaxy, plus 30 Doradus in the Large Magellanic Cloud. MOXC consists of 20,623 X-ray point sources from 12 MSFRs with distances ranging from 1.7 kpc to 50 kpc, and comprises Table 3 of the reference paper. In their paper, the authors show the morphology of the unresolved X-ray emission that remains after the cataloged X-ray point sources are excised from the ACIS data, in the context of Spitzer and WISE observations that trace the bubbles, ionization fronts, and photon-dominated regions that characterize MSFRs. In previous work, they have found that this unresolved X-ray emission is dominated by hot plasma from massive star wind shocks. This diffuse X-ray emission is found in every MOXC MSFR, clearly demonstrating that massive star feedback (and the several-million-degree plasmas that it generates) is an integral component of MSFR physics. The Chandra observations used for the Massive Star-forming Regions Omnibus X-ray Catalog (MOXC) are summarized in Table 2 of the reference paper and have dates ranging from 2000-04-03 to 2013-01-31 for the 12 MSFRs: the 7 MYStIX targets NGC 6334, NGC 6357, M 16, M 17, W 3, W 4 and NGC 3576, and the 5 "beyond-MYStIX" targets G333.6-0.2, W 51A, G29.96-0.02, NGC 3603 and 30 Doradus. A similar table to MOXC for other MYStIX targets was presented by Kuhn et al. (2013, ApJS, 209, 27, available as the HEASARC MYSTIXXRAY table). The main difference between that table and the MOXC version is that the present authors have chosen to omit absorption-corrected X-ray source luminosities from the XPHOT algorithm (Getman et al. 2010, ApJ, 708, 1760) herein, because those quantities are given in Broos et al. (2013, ApJS, 209, 32, available as the HEASARC MYSTIXMPCM table) for relevant MYStIX X-ray sources (those classified as pre-main sequence stars). For beyond-MYStIX targets, the authors chose to postpone XPHOT calculations until the X-ray sources were classified, since XPHOT estimates are only appropriate for pre-MS stars. The XPHOT code is available (Getman et al. 2012, Astrophysics Source Code Library, record ascl.soft12002) if others wish to use it on MOXC sources. All photometric quantities in this table are apparent (not corrected for absorption). The HEASARC has used prefixes 'fb_', 'sb_' and 'hb_' (replacing the suffixes '_t', '_s' and '_h' used in the reference paper) on the names of the X-ray photometric quantities which designate the full (total, 0.5 - 8 keV), soft (0.5 - 2.0 keV) and hard (2-8 keV) energy bands. Correction for finite extraction apertures is applied to the ancillary reference file (ARF) calibration products (see Broos et al. 2010, ApJ, 714, 1582, Section 5.3); the total_counts and counts quantities characterize the extraction and are not aperture-corrected. The only calibrated quantities presented are the apparent photon fluxes, in units of photon cm<sup>-2</sup> s<sup>-1</sup> (see Broos et al. 2010, ApJ, 714, 1582, Section 7.4), and estimates for the apparent energy fluxes, in units of erg cm<sup>-2</sup> s<sup>-1</sup> (Getman et al. 2010, ApJ, 708, 1760). This table was created by the HEASARC in October 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/213/1">CDS Catalog J/ApJS/213/1</a> files table3.dat (the MOXC X-ray Source Catalog) and table6.dat (the list of MOXC sources in previously published Chandra catalogs). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixmpcm
- Title:
- MassiveYoungStar-FormingComplexStdyinIR&X-Rays:MYStIXProbComplexMbrs
- Short Name:
- MYSTIXMPCM
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Massive Young Star-forming complex Study in Infrared and X-rays (MYStIX) project requires samples of young stars that are likely members of 20 nearby Galactic massive star-forming regions. Membership is inferred from statistical classification of X-ray sources, from detection of a robust infrared excess that is best explained by circumstellar dust in a disk or infalling envelope and from published spectral types that are unlikely to be found among field stars. This table contains the MYStIX membership lists, which total 31,549 probable complex members. In their reference paper, the authors describe in detail the statistical classification of X-ray sources via a "Naive Bayes Classifier". These membership lists provide the empirical foundation for subsequent MYStIX science studies. The MYStIX project, described by Feigelson et al. (2013, ApJS, 209, 26), seeks to identify and study samples of young stars in 20 nearby (0.4 < D < 3.6kpc) Galactic massive star-forming regions (MSFRs). These samples are derived using X-ray data from the Chandra X-ray Observatory, near-infrared (NIR) photometry from the United Kingdom InfraRed Telescope (UKIRT) and from the Two Micron All Sky Survey (2MASS), mid-infrared (MIR) photometry from the Spitzer Space Telescope, and from published spectroscopically-identified massive stars. The purpose of this study is to describe the authors' efforts to minimize contaminants in the MYStIX catalogs of young stars. They refer to these latter objects as the "MYStIX Probable Complex Members" or MPCMs. This table contains the combined MPCM catalog for all 20 of the MYStIX MSFRs. This MPCM catalog is the union of three sets of probable members identified by three different established methods for identifying young stars (see Feigelson et al. 2013, ApJS, 209, 26, Fig. 3). Most of the X-ray information on the MPCMs (with the exception of the X-ray luminosities and absorbing column densities obtained using XPHOT) was produced by the ACIS Extract (AE) software package (Broos et al. 2010, ApJ, 714, 1582 and 2012, Astrophysics Source Code Library, 1203.001). The AE software and User's Guide are available at <a href="http://www.astro.psu.edu/xray/acis/acis_analysis.html">http://www.astro.psu.edu/xray/acis/acis_analysis.html</a>. X-ray quantities using the 'fb' prefix are for the full or total energy band from 0.5 - 8.0 keV, those using the 'sb' prefix are for the soft band from 0.5 - 2.0 keV, and those using the 'hb' prefix are for the hard band from 2.0 - 8.0 keV. L. K. Townsley and P. S. Broos (2013, in preparation) and Kuhn et al. (2013, ApJS, 209, 27) identify a few very bright X-ray sources in each region that suffer from a type of instrumental non-linearity known as photon pile-up (<a href="http://cxc.harvard.edu/ciao/why/pileup_intro.html">http://cxc.harvard.edu/ciao/why/pileup_intro.html</a>); X-ray properties reported for those sources are biased and should be used with caution. This table was created by the HEASARC in February 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209/32">CDS Catalog J/ApJS/209/32</a> file mpcm.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixires
- Title:
- MassiveYoungStar-FormingComplexStudyinIR&X-Rays:IR-ExcessSources
- Short Name:
- MYSTIXIRES
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Massive Young Star-Forming Complex Study in Infrared and X-rays (MYStIX) project provides a comparative study of 20 Galactic massive star-forming complexes with distances between 0.4 and 3.6 kpc. Probable stellar members in each target complex are identified using X-ray and/or infrared data via two pathways: (1) X-ray detections of young/massive stars with coronal activity/strong winds or (2) infrared excess (IRE) selection of young stellar objects (YSOs) with circumstellar disks and/or protostellar envelopes. In this particular study, the authors present the methodology for the second pathway using Spitzer/IRAC, 2MASS, and UKIRT imaging and photometry. Although IRE selection of YSOs is well-trodden territory, MYStIX presents unique challenges. The target complexes range from relatively nearby clouds in uncrowded fields located toward the outer Galaxy (e.g., NGC 2264, the Flame Nebula) to more distant, massive complexes situated along complicated, inner Galaxy sightlines (e.g., NGC 6357, M 17). The authors combine IR spectral energy distribution (SED) fitting with IR color cuts and spatial clustering analysis to identify IRE sources and to isolate probable YSO members in each MYStIX target field from the myriad types of contaminating sources that can resemble YSOs: extragalactic sources, evolved stars, nebular knots, and even unassociated foreground/background YSOs. Applying their methodology consistently across 18 of the target complexes, they produce the MYStIX IRE Source (MIRES) Catalog comprising 20,719 sources, including 8,686 probable stellar members of the MYStIX target complexes. They also classify the SEDs of 9,365 IR counterparts to MYStIX X-ray sources to assist the first pathway, the identification of X-ray-detected stellar members. The MYStIX project, described by Feigelson et al. (2013, ApJS, 209, 26), provides a comprehensive, parallel study of 20 Galactic massive star-forming regions. The basic input data for the MIRES Catalog were near-IR (NIR) and mid-IR (MIR) photometric catalogs. The authors also used NIR and MIR images and mosaics for visualizing the point-source populations with respect to various nebular structures. They provide high-level descriptions of each input catalog in section 2 of the reference paper. This table contains the MYStIX IRE Source (MIRES) Catalog comprising IR data on 20,719 sources, including 8,686 probable stellar members of the MYStIX target complexes, viz., massive star-forming regions (MSFRs), which was given in Table 2 of the reference paper. It does not include the IR data of the above-mentioned 9,365 IR counterparts to MYStIX X-ray sources (the SED Classification of IR Counterparts to MYStIX X-ray sources (SCIM-X Catalog) that were listed in Table 7 of the reference paper. This table was created by the HEASARC in February 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209/31">CDS Catalog J/ApJS/209/31</a> file table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixmidi
- Title:
- MassiveYoungStar-FormingComplexStudyinIR&X-Rays:Mid-IRSourceCatalogs
- Short Name:
- MYSTIXMIDI
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Spitzer IRAC observations and stellar photometric catalogs are presented for the Massive Young star-forming complex Study in the Infrared and X-ray (MYStIX). MYStIX is a multi-wavelength census of young stellar members of 20 nearby (distances < 4 kpc), Galactic, star-forming regions (SFRs) that contain at least one O-type star. All regions have data available from the Spitzer Space Telescope consisting of GLIMPSE or other published catalogs for 11 regions and results of the authors' own photometric analysis of archival data for the remaining 9 regions. The authors also reduced the GLIMPSE data for the W 3 SFR using the aperture photometry method in order to compare the results obtained using the two methods (see Section 3.4.2 of the reference paper). The reference paper seeks to construct deep and reliable catalogs of sources from the Spitzer images. Mid-infrared study of these regions faces challenges of crowding and high nebulosity. These new catalogs typically contain fainter sources than existing Spitzer studies, which improves the match rate to Chandra X-ray sources that are likely to be young stars, but increases the possibility of spurious point-source detections, especially peaks in the nebulosity. IRAC color-color diagrams help distinguish spurious detections of nebular polycyclic aromatic hydrocarbon (PAH) emission from the infrared excess associated with dusty disks around young stars. The distributions of sources on the mid-infrared color-magnitude and color-color diagrams reflect differences between MYStIX regions, including astrophysical effects such as stellar ages and disk evolution. The GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) Survey is a Legacy Science Program of the Spitzer Space Telescope to study star formation in the disk of the Milky Way Galaxy. It contains six MYStIX regions - the Lagoon Nebula, the Trifid Nebula, NGC 6334, the Eagle Nebula, M 17, and NGC 6357 - within the 2-degree wide strip along the Galactic equator (GLIMPSE I and II data releases). Furthermore, Spitzer images and photometry for RCW 38 and NGC 3576 come from the Vela-Carina survey (Majewski et al. 2007, Spitzer Proposal 40791), using a similar observing strategy with mosaicking and photometric analysis as performed with the GLIMPSE pipeline. The authors obtained publicly available raw IRAC images from the Spitzer Heritage Archive for nine MYStIX regions without GLIMPSE coverage. The target list and details of the Astronomical Observation Requests (AORs) are provided in Table 1 of the reference paper. The camera spatial resolutions are FWHM = 1.6" to 1.9" from 3.6 to 8.0um. This table contains the combined IRAC source lists from the GLIMPSE photometry of W 3 and the aperture photometry of the 9 SFRs listed in Table 4, part 1 of the reference paper. This table was created by the HEASARC in February 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209/29">CDS Catalog J/ApJS/209/29</a> files table2.dat and table3.dat. To distinguish from which table a source originated, the HEASARC has added a parameter called table_number listing the number of the source table, 2 or 3. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixxray
- Title:
- MassiveYoungStar-FormingComplexStudyinIR&X-Rays:X-RaySourceCatalog
- Short Name:
- MYSTIXXRAY
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Massive Young Star-forming complex Study in Infrared and X-ray (MYStIX) uses data from the Chandra X-Ray Observatory to identify and characterize the young stellar populations in 20 Galactic (d < 4 kpc) massive star-forming regions. In this present study, the X-ray analysis for Chandra ACIS-I observations of 10 of the MYStIX fields is described, and a catalog of > 10,000 X-ray sources is presented in this table. In comparison to other published Chandra source lists for the same regions, the number of MYStIX-detected faint X-ray sources in a region is often doubled. While the higher catalog sensitivity increases the chance of false detections, it also increases the number of matches to infrared stars. X-ray emitting contaminants include foreground stars, background stars, and extragalactic sources. The X-ray properties of sources in these classes are discussed in the reference paper. The X-ray observations were made with the imaging array on the Advanced CCD Imaging Spectrometer (ACIS-I) on board the Chandra X-Ray Observatory. This array of four CCD detectors subtends 17' x 17' on the sky. The number of different Chandra pointings for each region, the total exposures for these pointings, and details of how the observations were taken are provided in Table 1 of the reference paper. Overall, 29 Chandra ObsIDs are included with typical integration times for a pointing of 40 - 100 ks, sufficient to detect most OB stars and lower-mass pre-main-sequence stars down to ~ 0.5 - 1 solar masses for the MYStIX regions. The 10 MYStIX MSFRs treated herein are listed in Table 2 of the reference paper. The data were acquired from the Chandra Data Archive from 2001 Jan to Mar 2008 for 10 MYStIX fields (the Flame Nebula, RCW 36, NGC 2264, the Rosette Nebula, the Lagoon Nebula, NGC 2362, DR 21, RCW 38, Trifid Nebula and NGC 1893). The X-ray photometry is from Broos et al. (2010, ApJ, 714, 1582; ACIS Extract); see also the CCCP, Broos et al. (2011, ApJS, 194, 2). The source significance quantities (fb_prob_no_src, sb_prob_no_src, hb_prob_no_src and prob_no_src_min) are computed using a subset of each source's extractions chosen to maximize significance (Broos et al. 2010, ApJ, 714, 1582, Section 6.2). The source position and positional uncertainty quantities are computed using a subset of each source's extractions chosen to minimize the position uncertainty (Broos et al. 2010, ApJ, 714, 1582, Sections 6.2 and 7.1). All other quantities are computed using a subset of each source's extractions chosen to balance the conflicting goals of minimizing photometric uncertainty and of avoiding photometric bias (Broos et al. 2010, ApJ, 714, 1582, Sections 6.2 and 7). The observed and absorption-corrected energy fluxes and their associated errors and the estimated hydrogen column densities and their uncertainties are derived using non-parametric procedures (XPHOT, Getman et al. 2010, ApJ, 708, 1760). XPHOT assumes the X-ray spectral shapes of young, low-mass stars, which come from coronal X-ray emission. XPHOT quantities will therefore be unreliable for high-mass stars, for which X-ray emission is associated with the stellar wind. This table was created by the HEASARC in January 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209">CDS Catalog J/ApJS/209</a> 27 file xmystix.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/twomassrsc
- Title:
- 2MASS Redshift Survey (2MRS) Catalog
- Short Name:
- TWOMASSRSC
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
498. Master EUV Catalog
- ID:
- ivo://nasa.heasarc/euv
- Title:
- Master EUV Catalog
- Short Name:
- EUV
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The EUV database table is the Extreme Ultraviolet (EUV) Master Catalog and contains a compendium of EUV sources. It is comprised of selected fields from the following HEASARC EUV database tables: <pre> * <a href="/W3Browse/all/euvebsl.html">EUVEBSL</a> - First Extreme UltraViolet Explorer Bright Source List * <a href="/W3Browse/all/euvecat2.html">EUVECAT2</a> - Second Extreme UltraViolet Explorer Source Catalog * <a href="/W3Browse/all/roswfc2re.html">ROSWFC2RE</a> - ROSAT Wide Field Camera 2RE Catalog * <a href="/W3Browse/all/rosatxuv.html">ROSATXUV</a> - ROSAT Wide Field Camera Pointed Phase Catalog of XUV Sources * <a href="/W3Browse/all/euverap1.html">EUVERAP1</a> - First Extreme UltraViolet Explorer Right Angle Program Catalog * <a href="/W3Browse/all/euverap2.html">EUVERAP2</a> - Second Extreme UltraViolet Explorer Right Angle Program Catalog * <a href="/W3Browse/all/euverap3.html">EUVERAP3</a> - Third Extreme UltraViolet Explorer Right Angle Program Catalog * <a href="/W3Browse/all/euvexrtcat.html">EUVEXRTCAT</a> - All-Sky Catalog of Faint EUV Sources </pre> Notice that we have not included EUVECAT1 (First Extreme UltraViolet Explorer Source Catalog) and WFCBSC (ROSAT Wide Field Camera Bright Source Catalog), as these are obsolete catalogs superceded by EUVECAT2 and ROSWFC2RE, respectively. The EUVEBSL database table contains a detailed list of verified bright EUVE sources detected during the survey phase of the EUVE mission (calibration targets are also included). Two distinct surveys, the all-sky and deep surveys, were conducted by the four EUVE telescopes during the first six months of the mission. EUVEBSL contains 356 sources. EUVECAT2 is the 2nd Catalog of EUV objects detected by the Extreme Ultraviolet Explorer (EUVE) and published by Bowyer et al. in 1996 (ApJS, 102, 129). The data include (i) all-sky survey detections from the initial 6-months scanner survey phase, (ii) additional scanner detections made later during specially programmed observations designed to fill in low-exposure sky areas of the initial survey, (iii) sources detected with deep-survey telescope observations along the ecliptic plane, (iv) objects detected by the scanner telescopes during targeted spectroscopy observations, and (v) other observations. Plausible optical, X-ray, radio, and/or UV identifications are available for about 65% of the EUV sources. EUVECAT2 contains 801 sources. ROSWFC2RE is the ROSAT Wide Field Camera 2RE Source Catalog. It contains 479 EUV sources found during the ROSAT all-sky survey of July 1990 to January 1991. The information in this database is based on what has been published by Pye et al. (1995, MNRAS, 274, 1165). It supersedes the earlier WFC Bright Source Catalog (WFCBSC), but we have retained the latter in the EUV database for reasons of completeness The ROSATXUV database table is a catalog of XUV sources (Kreysing H.C., Brunner H., and Staubert, R. 1995, A&AS, 114, 465), extracted from observations by the ROSAT Wide Field Camera during the pointed phase. The 5916 WFC pointed observations that were included are from the calibration and verification phase in June 1990 and from the period of pointed observations from February 9, 1991 to July 15, 1994. The catalog contains 1022 independent source detections corresponding to 4 different filters (S1, S2, P1 and P2) and 328 individual sources, many of which were observed repeatedly. Only ROSATXUV detections in the S1 filter band are included in the EUV table. If there are multiple observations of a single source/position in ROSATXUV, then only one entry for that source will be present in the EUV Master Catalog. The EUVERAP1 database table contains the detections of 114 extreme-ultraviolet (EUV; 58 - 740 Angstrom) sources, of which 99 are new serendipitous sources, based on observations covering approximately 8% of the sky which were made with the imaging telescopes on board the Extreme Ultraviolet Explorer (EUVE) during the Right Angle Program (RAP). These data were obtained using the survey scanners and the Deep Survey instrument during the first year of the spectroscopic guest observer phase of the mission, from January 1993 to January 1994. The data set consists of 162 discrete pointings whose exposure times are typically two orders of magnitude longer than the average exposure times during the EUVE all-sky survey. The EUVERAP2 database table is a catalog of 235 extreme ultraviolet (EUV) sources, of which 169 are new detections, using the EUVE Observatory's Right Angle Program (RAP) data obtained with the A, B and C scanners and the Deep Survey (DS) instrument in the period from January 1994 through November 1998. The EUVE RAP used the all-sky survey telescopes (also known as the "scanners"), which were mounted at right angles to the Deep Survey and Spectrometer (DS/S) instruments, in order to obtain photometric data in four wavelength bands centered at 100 Angstroms (Lexan/B), 200 A (Al/Ti/C), 400 A (Ti/Sb/Al or Dagwood), and 550 A (Sn/SiO). The EUVERAP2 catalog covers 17% of the sky and includes observations that were made subsequent to the publication of the first EUVE RAP catalog (EUVERAP1, which listed RAP data that had been obtained up until 1994 January); the data from EUVERAP1, together with additional RAP data obtained through 1994 December, are contained in the EUVECAT2 database table (The Second EUVE All-Sky Catalog of Bowyer et al. 1996, ApJS, 102, 129). Thus, RAP sources detected in 1994 will be contained in both EUVECAT2 and EUVERAP2, albeit different selection criteria were used in the two catalogs. The EUVERAP3 database table is a catalog of 76 extreme ultraviolet (EUV) sources, of which 63 are new detections, using the EUVE's RAP data. This catalog concentrates on observations made in the last years of the RAP, 1999 and 2000, with a sky coverage of 7% of the sky. The EUVEXRTCAT database table is a catalog of 534 objects detected jointly in the Extreme Ultraviolet Explorer (EUVE) (100 Angstrom (AA) band) All-Sky Survey and in the ROSAT X-ray Telescope (XRT) (0.25 keV band) All-Sky Survey. The joint selection criterion within a 1.5 arcminute positional tolerance permitted the use of a low count rate threshold in each survey. This low threshold was roughly 60% of the threshold used in the previous EUVE all-sky surveys, and 166 of the objects listed in this table were new EUV sources, appearing neither in the Second EUVE Source Catalog nor in the ROSAT Wide Field Camera Second Catalog. Preliminary identifications are offered for 105 of the 166 sources not previously reported in any EUV catalog: by far the most numerous (81) of the identifications are late-type (F-M) stars, while 18 are other stellar types, only 5 are white dwarfs, and none are extragalactic. The paucity of WDs and extragalactic objects may be explained by a strong horizon effect wherein interstellar absorption strongly limits the effective new-source search volume, and, thereby, selectively favors low-luminosity nearby sources over more luminous but distant objects. Notice that, with the adopted 1.5 arcminute acceptance criterion, about 50 spurious detections are expected. This database is periodically updated by the HEASARC 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 .
499. Master Radio Catalog
- ID:
- ivo://nasa.heasarc/radio
- Title:
- Master Radio Catalog
- Short Name:
- Radio
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The RADIO database table is a periodically revised master catalog that contains selected parameters from a number of the HEASARC database tables that have information on radio source flux densities. The contents of this RADIO master catalog are listed in alphabetical order in the References section of this document. Each entry in RADIO has a parameter called `database_table` which indicates the originating database table from which the entry was copied. Users should check out the original database table if they want to examine all of the parameters that are available in that particular database table for the particular source(s) in which they are interested. Two of the component database tables of RADIO, DIXON and KUEHR, are compilations of radio observations, and individual sources can have multiple entries, representing either observations at different frequencies or multiple observations at the same frequency. In the latter case, notice, the flux density quoted in the RADIO database is an average of the individual flux densities at that particular frequency in the originating database. To see all of the individual entries for a source in RADIO from either of these two component databases, the corresponding entries in the DIXON and KUEHR database tables should be examined. The HEASARC in certain instances has included radio 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 RADIO master source list. This database table is periodically updated by the HEASARC 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 .
500. Master X-Ray Catalog
- ID:
- ivo://nasa.heasarc/xray
- Title:
- Master X-Ray Catalog
- Short Name:
- X-ray
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- 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 .
