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XMM-Newton M 31 Survey Source Catalog
This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10<sup>34</sup> erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogs and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein. This table was originally created by the HEASARC in May 2005 based on the CDS table J/A+A/434/483/ file table2.dat (sources numbered 1 to 856). It was updated by the HEASARC in June 2008 by adding the 39 sources from the CDS table J/A+A/480/599/ file table3.dat (sources numbered 857 to 895). This is a service provided by NASA HEASARC .
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XMM-Newton M 33 Survey Catalog
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This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 1035 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33. This table was created by the HEASARC in October 2004 based on CDS table J/A+A/426/11/table3.dat This is a service provided by NASA HEASARC .
M 31 XMM-Newton Spectral Survey X-Ray Point Source Catalog
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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 LX interval 37.0 <~ log LX erg s-1 <~ 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 LX ~1.4 x 1036 erg s-1, 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 .
M 31 Deep XMM-Newton Survey X-Ray Source Catalog
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The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~1035erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D25 ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources. This table was created by the HEASARC in October 2011 based on CDS Catalog J/A+A/534/A55 files table5.dat and table8.dat. This is a service provided by NASA HEASARC .
M 101 XMM-Newton X-Ray Point Source Catalog
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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 D25 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 D25 ellipse of M101. This table was created by the HEASARC in October 2011 based on CDS Catalog J/MNRAS/357/401 files table1.dat and table2.dat. This is a service provided by NASA HEASARC .
M 33 XMM-Newton X-Ray Variability Source Catalog
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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 10-16 to 1.5 x 10-11 erg/cm2/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 https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/448/1247/table5.dat.gz This is a service provided by NASA HEASARC .
M 33 Deep XMM-Newton Survey X-Ray Source Catalog
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The authors have obtained a deep 8-field XMM-Newton mosaic of M33 covering the galaxy out to the D25 isophote and beyond to a limiting 0.2-4.5 keV unabsorbed flux of 5 x 10-16 erg cm-2 s-1 (L > 4 x 1034 erg s-1 at the 817 kpc distance of M33). These data allow complete coverage of the galaxy with high sensitivity to soft sources such as diffuse hot gas and supernova remnants (SNRs). In the reference paper, the authors describe the methods they used to identify and characterize 1296 point sources in the 8 fields. They compare their resulting source catalog to the literature, note variable sources, construct hardness ratios, classify soft sources, analyze the source density profile, and measure the X-ray luminosity function (XLF). As a result of the large effective area of XMM-Newton below 1 keV, the survey contains many new soft X-ray sources. The radial source density profile and XLF for the sources suggest that only ~15% of the 391 bright sources with L > 3.6 x 1035 erg s-1 are likely to be associated with M33, and more than a third of these are known SNRs. The log(N)-log(S) distribution, when corrected for background contamination, is a relatively flat power law with a differential index of 1.5, which suggests that many of the other M33 sources may be high-mass X-ray binaries. Finally, the authors note the discovery of an interesting new transient X-ray source, which they are unable to classify. The list of XMM-Newton observations used for this survey is given in Table 1 of the reference paper. The data reduction and source detection techniques are described in Section 3 of this same reference. The unabsorbed energy conversion factors (ECF) values for different energy bands and instruments that were used in this paper are as follows (the units are 1011 counts cm2 erg-1): 
 HEASARC Energy Band MOS1 MOS2 PN band prefix (keV) Med Filter Med Filter Thin Filter sb0_ 0.2-0.5 0.5009 0.4974 2.7709 sb1_ 0.5-1.0 1.2736 1.2808 6.006 mb_ 1.0-2.0 1.8664 1.8681 5.4819 hb_ 2.0-4.5 0.7266 0.7307 1.9276 fb_ 0.2-4.5
This table was created by the HEASARC in July 2015 based on an electronic version of Table 3 of the reference paper, the list of XMM-Newton X-ray point sources detected in a deep 8-field mosaic of M33, which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .
M 83 XMM-Newton X-Ray Point Source Catalog
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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 D25 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 D25 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): 
 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
where F is the filter (t for thin, m for medium), Texp 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 CDS Catalog J/A+A/553/A7 files tableb1.dat and tableb2.dat. This is a service provided by NASA HEASARC .
M 81 Chandra X-Ray Discrete Source Catalog
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A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 1036 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions. This table was created by the HEASARC in March 2007 based on the CDS table J/ApJS/144/213, files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
M 51 Chandra X-Ray Discrete Source Catalog
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This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 1039 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 1038 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively. This table was created by the HEASARC in March 2007 based on CDS catalog J/ApJ/601/735 files table2.dat, table3.dat and table4.dat. This is a service provided by NASA HEASARC .
NGC 2547 XMM-Newton X-Ray Point Source Catalog
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This table contains a list of point sources detected by XMM-Newton EPIC in a pointing towards the young open cluster NGC 2547, made in order to allow the authors to characterize coronal activity in solar-type stars, and stars of lower mass, at an age of 30 Myr. X-ray emission was seen from stars at all spectral types, peaking among G stars at luminosities (0.3 - 3 keV) of Lx ~= 1030.5 erg/s and declining to Lx <= 1029 erg/s among M stars with masses >=0.2 solar masses. Coronal spectra show evidence for multi-temperature differential emission measures and low coronal metal abundances of Z~= 0.3. Most of the solar-type stars in NGC 2547 exhibit saturated or even supersaturated X-ray activity levels. The median levels of Lx and Lx/Lbol in the solar-type stars of NGC 2547 are very similar to those in T-Tauri stars of the Orion Nebula cluster (ONC), but an order of magnitude higher than in the older Pleiades. The spread in X-ray activity levels among solar-type stars in NGC 2547 is much smaller than in older or younger clusters. This table contains the properties of those X-ray sources which are correlated with optical cluster members (see Section 2.2 of the reference paper for details on the correlation procedure that was adopted), as well as the properties of those X-ray sources which are uncorrelated with any optical cluster members. The table lists the cross-identifications with optical catalogs for the candidate cluster sources along with their X-ray luminosities and X-ray to bolometric flux ratios, as well as the correlations between cluster members which were detected by XMM-Newton and those detected 7 years earlier by the ROSAT HRI instrument, along with the X-ray luminosities and flux ratios as determined by the HRI. This table was created by the HEASARC in February 2007 based on CDS Catalog J/MNRAS/367/781 files table1.dat, table2.dat, table3.dat and table7.dat. This is a service provided by NASA HEASARC .
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