- ID:
- ivo://nasa.heasarc/m31xmm2
- Title:
- M 31 XMM-Newton Spectral Survey X-Ray Point Source Catalog
- Short Name:
- M31XMM2
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L<sub>X</sub> interval 37.0 <~ log L<sub>X</sub> erg s<sup>-1</sup> <~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L<sub>X</sub> ~1.4 x 10<sup>36</sup> erg s<sup>-1</sup>, the observed population is statistically dominated by the point source population of M 31. This table was created by the HEASARC in October 2009 based on the electronic version of Table A1 from the reference paper which was obtained from the CDS (their catalog J/A+A/495/733 file tablea1.dat. This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/m33snrxmm
- Title:
- M 33 XMM-Newton Supernova Remnants Catalog
- Short Name:
- M33SNRXMM
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors of this catalog carried out a study of the X-ray properties of the supernova remnant (SNR) population in M 33 with XMM-Newton, comprising deep observations of eight fields in M 33 covering all of the area within the D<sub>25</sub> contours, and with a typical luminosity of 7.1 x 10<sup>34</sup> erg/s (0.2-2.0keV). With their deep observations and large field of view they have detected 105 SNRs at the 3-sigma level, of which 54 SNRs are newly detected in X-rays, and three are newly discovered SNRs. Combining XMM-Newton data with deep Chandra survey data allowed detailed spectral fitting of 15 SNRs, for which they have measured temperatures, ionization time-scales and individual abundances. This large sample of SNRs allowed the authors to construct an X-ray luminosity function, and compare its shape to luminosity functions from host galaxies of differing metallicities and star formation rates to look for environmental effects on SNR properties. They concluded that while metallicity may play a role in SNR population characteristics, differing star formation histories on short time-scales, and small-scale environmental effects appear to cause more significant differences between X-ray luminosity distributions. In addition, they analyze the X-ray detectability of SNRs, and find that in M 33 SNRs with higher [SII]/H-alpha ratios, as well as those with smaller galactocentric distances, are more detectable in X-rays. This catalog utilized data from a deep survey of M 33 using an 8 field XMM-Newton mosaic that extends out to the D25 isophote. The point source catalog from this survey was published by W15 (Williams+2015, J/ApJS/218/9). In addition to the catalog of W15, the authors utilized high-resolution observations from the Chandra ACIS Survey of M 33 (ChASeM33, Tullmann+2011, J/ApJS/193/31) for the purposes of obtaining X-ray spectral fits. This table was ingested by the HEASARC in October 2019 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/472/308">CDS Catalog J/MNRAS/472/308</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/m101xmm
- Title:
- M 101 XMM-Newton X-Ray Point Source Catalog
- Short Name:
- M101XMM
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D<sub>25</sub> ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D<sub>25</sub> ellipse of M101. This table was created by the HEASARC in October 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/357/401">CDS Catalog J/MNRAS/357/401</a> files table1.dat and table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/m83xmm
- Title:
- M 83 XMM-Newton X-Ray Point Source Catalog
- Short Name:
- M83XMM
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- 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 .
- ID:
- ivo://nasa.heasarc/m33xmm2
- Title:
- M 33 XMM-Newton X-Ray Variability Source Catalog
- Short Name:
- M33XMM2
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M 33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10<sup>-16</sup> to 1.5 x 10<sup>-11</sup> erg/cm<sup>2</sup>/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M 33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M 33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M 33. The relative contribution of the classified XRB and SSS in M 33 is now comparable to M 31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M 33 remains much higher. This table was created by the HEASARC in March 2007 based on the CDS table J/A+A/448/1247 file table4.dat. The CDS has another table which lists the properties of the sources detected on an observation-by-observation basis which is not included as part of this Browse table but is available at <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/448/1247/table5.dat.gz">https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/448/1247/table5.dat.gz</a> This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/dss2
- Title:
- 2nd Digitized Sky Survey (Blue)
- Short Name:
- DSS2
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- <P> The native projection of these data is described as a high-order polynomial distortion of a gnomonic projection using the same terms as the DSS. Provenance: Data taken by ROE, AAO, and CalTech, Compression and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/neat
- Title:
- Near-Earth Asteriod Tracking System Archive
- Short Name:
- NEAT
- Date:
- 29 Apr 2022
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The NEAT/SkyMorph survey provides access to the archives of the Near Earth Asteroid Tracking (NEAT) project. NEAT is designed to look for potentially hazardous asteroids, i.e., those whose orbits cross the Earth's. Over 200,000 images are available in the NEAT archive. <a href=https://skyview.gsfc.nasa.gov/skymorph/skymorph.html>SkyMorph</a> provides a Web interface to the NEAT images and allows users to select all images in which a given fixed or moving object is found. <p> Unlike most <i>SkyView</i> surveys, the NEAT data are extremely irregular in their spatial distribution. <i>SkyView</i>'s algorithms for mosaicking images together to form large images are not adequate for the NEAT data, so mosaicking is surpressed. Only data within a single NEAT image will be displayed. The system attempts to find the most recent image within which has a offset in both RA and Dec of less than 0.8 degrees. If no such image is found, then an image with the minimum offset is returned, or the search may fail altogether if there are no nearby plates. The NEAT telescope uses an array of 4 CCDs. The backgrounds of the CCDs may differ significantly. <p> The NEAT survey covers approximately 30% of the sky. Extreme southern and low-Galactic latitude regions are unsurveyed. Coverage is otherwise particularly dense in the ecliptic plane. <p> NEAT data consists primarily of groups of three images taken with separations of 20 minutes and almost identical positions. <i> SkyView </i> will normally return the last of a 'triplet'. The SkyMorph site can be used to display an overlay of triplets to look for targets which moved during the interval between images. <p> A catalog of objects detected in the NEAT/SkyMorph pages is accessible through the SkyMorph pages. 'Light-curves' from all images during which an object was in the NEAT field of view can also be generated. <P> The NEAT data values are in arbitrary density units. To enhance the display data are transformed such that all pixels below the median values are scaled linearly to values 0-20, while all pixels above the median are shifted (but not scaled) to values greater than 20.
- ID:
- ivo://nasa.heasarc/nuvbemdcat
- Title:
- Near-UV Detected Bright Early-M Dwarf Star Catalog
- Short Name:
- NUVBEMDCAT
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Planets orbiting within the close-in habitable zones of M dwarf stars will be exposed to elevated high-energy radiation driven by strong magnetohydrodynamic dynamos during stellar youth. Near-ultraviolet (NUV) irradiation can erode and alter the chemistry of planetary atmospheres, and a quantitative description of the evolution of NUV emission from M dwarfs is needed when modeling these effects. The authors investigated the NUV luminosity evolution of early M-type dwarfs by cross-correlating the Lepine & Gaidos (LG11: 2011, AJ, 142, 138) catalog of bright M dwarfs (available at the HEASARC as the MDWARFASC table) with the Galaxy Evolution Explorer (GALEX) catalog of NUV (1771-2831 Angstrom) sources. Of the 4,805 sources with GALEX counterparts, 797 have NUV emission significantly (> 2.5 sigma) in excess of an empirical basal level. The authors inspected these candidate active stars using visible-wavelength spectra, high-resolution adaptive optics imaging, time-series photometry, and literature searches to identify cases where the elevated NUV emission is due to unresolved background sources or stellar companions; they estimated the overall occurrence of these "false positives" (FPs) as ~ 16%. The authors constructed an NUV luminosity function that accounted for FPs, detection biases of the source catalogs, and GALEX upper limits. They found the NUV luminosity function to be inconsistent with predictions from a constant star-formation rate and simplified age-activity relation defined by a two-parameter power law. This table was created by the HEASARC in March 2015 based on an electronic versions of Table 4 from the reference paper which was obtained from the ApJ web site. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/wbhgp6cm
- Title:
- New Catalog of Compact 6cm Sources in the Galactic Plane
- Short Name:
- WBH6cmGP
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the New Catalog of Compact Radio (6-cm) Sources in the Galactic Plane of White et al. (2005). Archival data were combined with more recent observations of the Galactic plane using the Very Large Array to create two new catalogs of compact centimetric radio sources. The 20-cm source catalog (available in the HEASARC Browse system as the table WBHGP20CM) covers a longitude range from -20 to +120 degrees in Galactic longitude l; the latitude coverage varies from b = +/- 0.8 to +/- 2.7 degrees. The total survey area is about 331 square degrees; coverage is 90% complete at a flux density threshold of about 14 mJy, and over 5000 sources are recorded. The 6-cm catalog described here covers 43 square degrees in the region -10 degrees < l <42 degrees, |b| < 0.4 degrees to a 90% completeness threshold of 2.9 mJy; over 2700 sources are found. Both surveys have an angular resolution of about 6". These catalogs provide a 30% (at 20 cm) to 50% (at 6 cm) increase in the number of high-reliability compact sources in the Galactic plane, as well as greatly improved astrometry, uniformity, and reliability; they should prove useful for comparison with new mid- and far-infrared surveys of the Milky Way. The images from which this catalog was constructed are available at the MAGPIS web site, <a href="http://third.ucllnl.org/gps">http://third.ucllnl.org/gps</a> This table was created by the HEASARC in July 2006 based on the combination of CDS tables J/AJ/130/586 table5.dat and table6.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/wbhgp20cm
- Title:
- New Catalog of Compact 20cm Sources in the Galactic Plane
- Short Name:
- WBH20cmGP
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the New Catalog of Compact Radio (20-cm) Sources in the Galactic Plane of White et al. (2005). Archival data were combined with more recent observations of the Galactic plane using the Very Large Array to create two new catalogs of compact centimetric radio sources. The 20-cm source catalog contained here covers a longitude range from -20 to +120 degrees in Galactic longitude l; the latitude coverage varies from b = +/- 0.8 to +/- 2.7 degrees. The total survey area is about 331 square degrees; coverage is 90% complete at a flux density threshold of about 14 mJy, and over 5000 sources are recorded. The 6-cm catalog (also available in the HEASARC Browse system as the table WBHGP6CM) covers 43 square degrees in the region -10 degrees < l <42 degrees, |b| < 0.4 degrees to a 90% completeness threshold of 2.9 mJy; over 2700 sources are found. Both surveys have an angular resolution of about 6". These catalogs provide a 30% (at 20 cm) to 50% (at 6 cm) increase in the number of high-reliability compact sources in the Galactic plane, as well as greatly improved astrometry, uniformity, and reliability; they should prove useful for comparison with new mid- and far-infrared surveys of the Milky Way. The images from which this catalog was constructed are available at the MAGPIS web site, <a href="http://third.ucllnl.org/gps">http://third.ucllnl.org/gps</a> This table was created by the HEASARC in July 2006 based on the combination of CDS tables J/AJ/130/586 table3.dat and table4.dat. This is a service provided by NASA HEASARC .
