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501. Lambda Orionis Cluster XMM-Newton X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/lamorixmm
Title:
Lambda Orionis Cluster XMM-Newton X-Ray Point Source Catalog
Short Name:
LAMORIXMM
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The authors studied the X-ray properties of the young (~1-8M yr) open cluster around the hot (O8 III) star Lambda Ori and compared them with those of the similarly-aged Sigma Ori cluster in order to investigate the possible effects of the different ambient environments. They analyzed an XMM-Newton observation of the cluster using EPIC imaging and low-resolution spectral data. They studied the variability of the detected sources, and performed a spectral analysis of the brightest sources in the field using multi-temperature models. The authors detected 167 X-ray sources above a 5-sigma detection threshold the properties of which are listed in this table, of which 58 are identified with known cluster members and candidates, from massive stars down to low-mass stars with spectral types of ~ M5.5. Another 23 sources were identified with new possible photometric candidates. Late-type stars have a median log L<sub>X</sub>/L<sub>bol</sub> ~ -3.3, close to the saturation limit. Variability was observed in ~ 35% of late-type members or candidates, including six flaring sources. The emission from the central hot star Lambda Ori is dominated by plasma at 0.2 - 0.3 keV, with a weaker component at 0.7 keV, consistent with a wind origin. The coronae of late-type stars can be described by two plasma components with temperatures T<sub>1</sub> ~ 0.3-0.8 keV and T<sub>2</sub> ~ 0.8-3 keV, and subsolar abundances Z ~ 0.1-0.3 Z<sub>sun</sub>, similar to what is found in other star-forming regions and associations. No significant difference was observed between stars with and without circumstellar discs, although the smallness of the sample of stars with discs and accretion does not definitive conclusions to be drawn. The authors concluded that the X-ray properties of Lambda Ori late-type stars are comparable to those of the coeval Sigma Ori cluster, suggesting that stellar activity in Lambda Ori has not been significantly affected by the different ambient environment. The lambda Ori cluster was observed by XMM-Newton from 20:46 UT on September 28, 2006 to 12:23 UT on September 29, 2006 (Obs. ID 0402050101), for a total duration of 56ks, using both the EPIC MOS and PN cameras and the RGS instruments. The EPIC cameras were operated in full frame mode with the thick filter. This table was created by the HEASARC in November 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/530/A150">CDS Catalog J/A+A/530/A150</a> files tablea1.dat ('X-ray sources detected in the Lambda Ori Cluster'), table1,dat ('X-ray and optical properties of sources identified with known cluster members and candidates') and table2.dat ('X-ray sources identified with possible new cluster candidates'). It does not include the objects listed in tablea2.dat ('3-sigma upper limits and optical properties of undetected cluster members and candidates'). This is a service provided by NASA HEASARC .
502. Large Bright Quasar Survey
ID:
ivo://nasa.heasarc/lbqs
Title:
Large Bright Quasar Survey
Short Name:
LBQS
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
Positions, redshifts, and magnitudes for the 1055 quasars in the Large Bright Quasar Survey (LBQS) are presented in a single catalog. Celestial positions have been rederived using the PPM catalog to provide an improved reference frame. Redshifts calculated via cross correlation with a high signal-to-noise ratio composite quasar spectrum are included and the small number of typographic and redshift misidentifications in the discovery papers are corrected. Compared to the discovery papers (references below), 12 quasars that are either fainter than the field magnitude limit or fall outside the final survey area have been deleted, 12 quasars that were discovered subsequent to paper V have been added, 10 redshifts have been corrected, and 13 quasars with either incorrect or degenerate designations (LBQS names) have had their designations corrected. The information in this version of the LBQS Catalog is the same as in Table 4 of the published paper with the following exceptions: (i) the object 0021-0213 has a redshift of 2.348; this value was listed in Table 5 of the paper but was not incorporated in Table 4 of the paper; (ii) the parameter 'Reference' in Table 4 of the published paper (which specified in which paper in the LBQS series the quasar spectrum could be found) has been omitted; and (iii) the parameter 'Notes' in Table 4 of the published paper had two non-blank values: '+' and 'a'; in the HEASARC representation of this catalog we have replaced the Notes value of '+' by 'C', and dropped the Notes value of 'a' (used to indicate objects that had been listed as AGN in earlier papers). This catalog was created by the HEASARC in July 1999 based on a table that was kindly provided by the first author, Paul Hewett, supplemented by documentation created by the CDS/ADC. This is a service provided by NASA HEASARC .
503. Large Magellanic Cloud Extended Objects Catalog
ID:
ivo://nasa.heasarc/lmcextobj
Title:
Large Magellanic Cloud Extended Objects Catalog
Short Name:
LMCEXTOBJ
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
A survey of extended objects in the Large Magellanic Cloud (LMC) was carried out on the ESO/SERC R and J Sky Survey Atlases, checking entries in previous catalogs and searching for new objects. The census provided 6659 objects including star clusters, emission-free associations, and objects related to emission nebulae. Each of these classes contains three subclasses with intermediate properties, which are used to infer total populations. The survey includes cross-identifications among catalogs, and includes 3246 new objects (~49% of the unified catalog). The authors have provided accurate positions, classification, and homogeneous measurements of sizes and position angles, as well as information on cluster pairs and hierarchical relation for superimposed objects. This unification and enlargement of catalogs is important for future searches of fainter and smaller new objects. The present catalog together with its previous counterpart for the SMC and the inter-Cloud region provide a total population of 7847 extended objects in the Magellanic System. The angular distribution of the ensemble reveals important clues on the interaction between the LMC and SMC. This table was created by the HEASARC in March 2007 based on the CDS table J/AJ/117/238, file table2.dat and contains the 6659 extended objects found in this LMC survey. This is a service provided by NASA HEASARC .
504. Large Quasar Astrometric Catalog, 3rd Release
ID:
ivo://nasa.heasarc/lqac
Title:
Large Quasar Astrometric Catalog, 3rd Release
Short Name:
LQAC
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
Since the release of the original Large Quasar Astrometric Catalog (LQAC: Souchay et al. 2009, A&A, 494, 815), a large number of quasars have been discovered through very dense observational surveys. Following the same procedure as in the first release of the LQAC, the authors aim is to compile all the quasars recorded up until the present date, with the best determination of their ICRS equatorial coordinates, i.e., with respect to the newly established ICRF2 (the second realization of the International Celestial Reference Frame) and with the maximum of information concerning their physical properties, e.g., redshifts, photometry, absolute magnitudes. In the second paper, the authors first of all made a substantial review of the definitions and properties of quasars and AGN (Active Galactic Nuclei), the differentiation of these objects being unclear in the literature and even for specialists. This served their purpose when deciding which kinds of objects would be taken into account in this compilation. Then, they carried out the cross-identification between the 9 catalogs of quasars chosen for their accuracy and their huge number of objects, using a flag for each of them, and including all the available data related to magnitudes (infrared and optical), radio fluxes and redshifts. They also performed cross identification with external catalogs 2MASS, B1.0 and GSC2.3 in order to complete photometric data for the objects. Moreover, they computed the absolute magnitude of their extragalactic objects by taking into account recent studies concerning Galactic absorption. In addition, substantial improvements were brought with respect to the first release of the LQAC. First, an LQAC name was given for each object based on its equatorial coordinates with respect to the ICRS, following a procedure which creates no ambiguity for identification. Secondly, the equatorial coordinates of the objects were recomputed more accurately according to the algorithms used for the elaboration of the Large Quasar Reference Frame (LQRF) (Andrei et al., 2009, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/I/313">CDS Cat. I/313</a>). Thirdly, the authors introduced a morphological classification for the objects which enabled them in particular to define clearly if the object is point-like or extended. The authors adopted a cosmology with H<sub>0</sub> = 70 km s<sup>-1</sup> Mpc<sup>-1</sup>, Omega<sub>M</sub> = 0.3, Omega<sub>Lambda</sub> = 0.7, and q<sub>0</sub> = -0.65 in LQAC-3 (which is slightly different from that adopted for LQAC-2, notice). The final catalog, called LQAC-2, contained 187,504 quasars. This was roughly 65% larger than the 113,666 quasars recorded in the first version of the LQAC (Souchay et al. 2009, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/494/799">CDS Cat. J/A+A/494/799</a>) and a little more than the number of quasars recorded in the up-dated version of the Veron-Cetty and Veron (2010, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/258">CDS Cat. VII/258</a>, HEASARC VERONCAT table) catalog, which was the densest compilation of quasars up to the present one. In addition to the quantitative and qualitative improvements implemented in this compilation, the authors discussed the homogeneity of the data and carried out a statistical analysis concerning the spatial density and the distance to the nearest neighbor in their published paper. The authors adopted a cosmology with H<sub>0</sub> = 72 km s<sup>-1</sup> Mpc<sup>-1</sup> and q<sub>0</sub> = -0.58 in this study. From an astrometric point of view, quasars constitute quasi-ideal reference objects in the celestial sphere, with an a priori absence of proper motion. Since the second release of the LQAC, a large number of quasars have been discovered, in particular with the upcoming new release of the SDSS quasars catalog. Following the same procedure as in the two previous releases of the LQAC, The authors' aim for LQAC-3 was to compile all the quasars recorded until the present date, with accurate recomputation of their equatorial coordinates in the ICRS and with the maximum of information concerning their physical properties, such as the redshift, the photometry, and the absolute magnitudes. The authors carried out the cross-identification between the 9 catalogs of quasars chosen for their huge number of objects, including all the available data related to magnitudes, radio fluxes, and redshifts. This cross identification was particularly delicate because of a slight change in coordinates between the objects common to two successive releases of the SDSS and the elimination of some of them. Equatorial coordinates were recomputed more accurately according to the algorithms used for the elaboration of the Large Quasar Reference Frame (LQRF). Moreover, absolute magnitudes and morphological indexes of the new objects were given, following the same method as in the LQAC-2. The final catalog, called LQAC-3, contains 321,957 objects including a small proportion of AGNs (14,128) and BL Lac objects (1,183). This is roughly 70% more than the number of objects recorded in the LQAC-2. The LQAC-3 will be useful for the astronomical community since it gives the most complete information available about the whole set of already recorded quasars, with emphasis on the precision and accuracy of their coordinates with respect to the ICRF2. This table was created by the HEASARC in June 2016 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/583/A75">CDS Catalog J/A+A/583/A75</a>, file lqac3.dat. This is a service provided by NASA HEASARC .
505. Las Campanas Redshift Survey Catalog
ID:
ivo://nasa.heasarc/lcrscat
Title:
Las Campanas Redshift Survey Catalog
Short Name:
LCRSCAT
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg<sup>2</sup> in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s<sup>-1</sup>. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s<sup>-1</sup>, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: <a href="http://qold.astro.utoronto.ca/~lin/lcrs.html">http://qold.astro.utoronto.ca/~lin/lcrs.html</a>. This table was created by the HEASARC in May 2010 based on the electronic version of Table 3 from the above reference which was obtained from the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/203">CDS Catalog VII/203</a> file catalog.dat. This is a service provided by NASA HEASARC .
506. Lepine and Shara Northern Stars Proper Motion (LSPM-North) Catalog
ID:
ivo://nasa.heasarc/lspmnorth
Title:
Lepine and Shara Northern Stars Proper Motion (LSPM-North) Catalog
Short Name:
LSPMNORTH
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The LSPM catalog is a comprehensive list of 61,977 stars north of the J2000 celestial equator that have proper motions larger than 0.15" yr<sup>-1</sup> (local-background-stars frame). The catalog has been generated primarily as a result of the authors' systematic search for high-proper-motion stars in the Digitized Sky Surveys using their SUPERBLINK software (note that this catalog is consequently also sometimes referred to as the SUPERBLINK Catalog). At brighter magnitudes, the catalog incorporates stars and data from the Tycho-2 Catalog and also, to a lesser extent, from the All-Sky Compiled Catalogue of 2.5 million stars (ASCC-2.5: Kharchenko 2001). The LSPM catalog considerably expands over the old Luyten (Luyten Half-Second (LHS) and New Luyten Two-Tenths (NLTT) catalogs, superseding them for northern declinations. Positions are given with an accuracy of <~ 100 milliarcseconds (mas) at the 2000.0 epoch, and absolute proper motions are given with an accuracy of ~ 8 mas/yr. Corrections to the local-background-stars proper motions have been calculated, and absolute proper motions in the extragalactic frame are given. Whenever available, the authors also give optical B<sub>T</sub> and V<sub>T</sub> magnitudes (from Tycho-2, ASCC-2.5), photographic B<sub>J</sub>, R<sub>F</sub>, and I<sub>N</sub> magnitudes (from the USNO-B1 catalog), and infrared J, H, and K<sub>s</sub> magnitudes (from 2MASS). An estimated V magnitude and V-J color is also provided for nearly all catalog entries, which is useful for initial classification of the stars. The catalog is estimated to be over 99% complete at high Galactic latitudes (|b| > 15 degrees) and over 90% complete at low Galactic latitudes (|b| < 15 degrees), down to a magnitude of V = 19.0, and has a limiting magnitude V = 21.0. All the northern stars listed in the LHS and NLTT catalogs have been re-identified, and their positions, proper motions, and magnitudes reevaluated. The catalog also lists a large number of completely new objects, which promise to expand very significantly the census of red dwarfs, sub-dwarfs, and white dwarfs in the vicinity of the Sun. All of Luyten's NLTT stars north of the J2000 celestial equator that do NOT appear in the LSPM Catalog are listed in Table 3 of the published paper, together with the explanations as to why they were not included in the LSPM Catalog. This table was created by the HEASARC in June 2013 based on an electronic version of Table 1 from the reference paper which was obtained from the CDS web site (their catalog I/298). This is a service provided by NASA HEASARC .
507. LISA Pathfinder Archive Data Summary
ID:
ivo://nasa.heasarc/lpffiles
Title:
LISA Pathfinder Archive Data Summary
Short Name:
LPFFILES
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table provides an index for a time ordered set of files containing the telemetry from the the DRS system on the LISA Pathfinder mission. It gives the time in a variety of spacecraft modes for each file. Note that not all modes were explored during the LISA Pathfinder mission. The Disturbance Reduction System (DRS) was an experiment package aboard the European Space Agency (ESA) LISA Pathfinder spacecraft. LISA Pathfinder (LPF) launched from Kourou, French Guiana, on December 3, 2015. LPF successfully demonstrated the disturbance-free motion of two test masses at a noise level acceptable for a future gravitational wave (GW) observatory. Designated ST7, DRS is the NASA contribution to LPF with the goal of operating disturbance reduction technology in space applicable to GW missions and other future missions with challenging stability requirements. DRS flew two clusters of four, low-noise, colloid micro-thrusters (eight total) and a computer which implemented drag-free control laws. At specific times during the LPF mission, DRS operated as alternative to the ESA provided thrusters and control laws. The location of the test masses relative to the spacecraft and the attitude of the spacecraft were measured by ESA subsystems and provided to DRS as its sensors. The displacement and attitude of the spacecraft relative to the two test masses was controlled using the colloid thrusters and electrostatic forces on the TMs provided by the LPF systems. The key requirements for DRS were to show that the thrust noise was less than 0.1 micro-N, and the spacecraft position noise was less than 10nm/sqrt( Hz) in the measurement frequency band of 1 to 30 micro-Hz. ST7 also recorded the relative acceleration noise (delta-g) between the two test masses, a key metric for the GW application, but had no requirement did not optimize the delta-g performance because this is primarily dependent on the (ESA) inertial sensor. ST7 executed a primary mission in which the thrust noise of the thrusters and the performance of the drag free control were measured and a short extended mission which was used to optimize the performance and expand the operating range of the thrusters and control laws. This table was created by the HEASARC in February 2018 based on data files provided by Jacob Slutsky and Leonid Petrov, which were reformatted from the base files at the LISA Pathfinder archive at ESA. The reformatted data files are available at <a href="https://heasarc.gsfc.nasa.gov/FTP/lpf/data/fits/">https://heasarc.gsfc.nasa.gov/FTP/lpf/data/fits/</a> with summaries of the instrument mode intervals available in summary files in <a href="https://heasarc.gsfc.nasa.gov/FTP/lpf/data/summ/">https://heasarc.gsfc.nasa.gov/FTP/lpf/data/summ/</a>. This is a service provided by NASA HEASARC .
508. LkH-alpha 101 Star Formation Region Chandra X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/lkha101cxo
Title:
LkH-alpha 101 Star Formation Region Chandra X-Ray Point Source Catalog
Short Name:
LKHA101CXO
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains some of the results from a multi-wavelength study of a partially embedded region of star formation centered on the Herbig Be star LkH-alpha 101. Using two 40 ks Chandra observations, The authors have detected 213 X-ray sources in the ~ 17' x 17' ACIS-I field. They combine the X-ray data with Two Micron All Sky Survey (2MASS) near-IR observations and Spitzer Space Telescope (SST) IRAC and MIPS 24-micron observations to obtain a complete picture of the cluster. A total of 158 of the X-ray sources have infrared counterparts. Of these, the authors find nine protostars, 48 Class II objects, five transition objects, and 72 Class III objects. From the Spitzer data, they identify an additional 10 protostars, 53 Class II objects, and four transition disk candidates which are not detected by Chandra. (These objects are not included in this HEASARC table which contains the multi-wavelength data for only the 213 detected X-ray sources). The authors obtained optical spectra of a sample of both X-ray-detected and non-X-ray-detected objects. Combining the X-ray, Spitzer, and spectral data, they obtain independent estimates of cluster distance and the total cluster size - excluding protostars. The authors obtain consistent distance estimates of 510 (+100,-40) pc and a total cluster size of 255 (+50,-25) stars. They find the Class II:III ratio is about 5:7 with some evidence that the Class III sources are spatially more dispersed. The cluster appears very young with three sites of active star formation and a median age of about 1 Myr. The field was observed by Chandra on 2005 March 6 starting at 17:16 UT for 40.2 ks of total time and 39.6 ks of the so-called good time (Chandra ObsID 5429). It was observed again on 2005 March 8 starting at 17:43 UT for essentially the same duration (Chandra ObsID 5428). The ACIS was used in the nominal imaging array (chips I0-I3) which provides a field of view of approximately 17' x 17'. The aimpoint was at RA, Dec = 04:30:14.4, +35:16:22.2 (J2000.0) with a roll angle of 281 degrees. In addition, the S2 and S3 chips were active; however, the analysis of these data is not presented here. For purposes of point-source detection, the data from the two observations were merged into a single event list following established CIAO procedures to create a merged event list. To identify point sources, photons with energies below 300 eV and above 8.0 keV were filtered out from this merged event list. This excluded energies which generally lack a stellar contribution. By filtering the data as described, contributions from hard, non-stellar sources such as X-ray binaries and active galactic nuclei (AGNs) are attenuated, as is noise. A monochromatic exposure map was generated in the standard way using an energy of 1.49 keV which is a reasonable match to the expected peak energy of the stellar sources and the Chandra mirror transmission. The CIAO tool WavDetect was then run on a series of flux-corrected images binned by 1, 2, and 4 pixels. The output source lists were combined and this resulted in the detection of 231 sources. The authors defined false detections as any sources with < 4 net counts or any sources more than 5' off-axis with < 7 net counts. By this definition, 18 of the 231 detections were rejected as false detections. A post facto check confirmed that none of these (spurious) sources had an infrared counterpart. This table was created by the HEASARC in July 2010 based on the versions of Tables 1, 2, 3, 7 and 9 from the paper which were obtained from the electronic ApJ web site. This is a service provided by NASA HEASARC .
509. LMC Clusters Catalog
ID:
ivo://nasa.heasarc/lmcclustrs
Title:
LMC Clusters Catalog
Short Name:
LMC/Cluster
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
A new catalogue of clusters in the Large Magellanic Cloud has been constructed from searches of the IIIa-J component of the ESO/SERC Southern Sky Atlas. The catalogue contains coordinate and diameter measurements of 1762 clusters in a 25 deg x 25 deg area of sky centered on the LMC, but excluding the very crowded 3.5 square deg region around the Bar. The distribution of these clusters appears as two superimposed elliptical systems. The higher density inner system extends over about 8 deg; the lower density outer system can be represented by 13 deg X 10 deg disc inclined at 42 deg to the line of sight. There are suggestions of two weak "arms" in the latter. This is a service provided by NASA HEASARC .
510. LMC 30 Doradus Complex Chandra X-Ray Point Source Catalog
ID:
ivo://nasa.heasarc/lmc30drcxo
Title:
LMC 30 Doradus Complex Chandra X-Ray Point Source Catalog
Short Name:
LMC30DRCXO
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This table contains the results of a study of the X-ray point-source population of the 30 Doradus (30 Dor) star-forming complex in the Large Magellanic Cloud (LMC) using high spatial-resolution X-ray images and spatially-resolved spectra obtained with the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. The observation of ~21 ks was made on 1999 September 21 and placed the cluster R136 at the aim point of the ACIS Imaging Array (ACIS-I). This table lists the the X-ray sources detected in the 17' x 17' field centered on R136, the massive star cluster which lies at the center of the main 30 Dor nebula. 20 of the 32 Wolf-Rayet stars in the ACIS field are detected. The cluster R136 is resolved at the sub-arcsecond level into almost 100 X-ray sources, including many typical O3-O5 stars, as well as a few bright X-ray sources which had been previously reported. Over 2 orders of magnitude of scatter in the X-ray luminosity L<sub>x</sub> (calculated assuming a distance of 50 kpc) is seen among R136 O stars, suggesting that X-ray emission in the most massive stars depends critically on the details of wind properties and the binarity of each system, rather than reflecting the widely reported characteristic value L<sub>x</sub>/L<sub>bol</sub> ~ 10<sup>-7</sup>. Such a canonical ratio may exist for single massive stars in R136, but these data are too shallow to confirm this relationship. Through this and more recent X-ray studies of 30 Dor, the complete life cycle of a massive stellar cluster can be revealed. This HEASARC table contains both the primary high-significance X-ray sources as well as some lower-significance tentative X-ray sources. The latter sources should not be considered definitive. A subsequent Chandra observation of this field, with several times the exposure of this observation, will result in a longer, more complete list of point sources than that given in this paper. This table was created by the HEASARC in February 2007 based on the merger of electronic versions of Tables 1, 2 and 5 from the above reference which were obtained from the AJ website. It does not include the results from the spectral analysis of 49 of the X-ray sources having a photometric significance (signal-to-noise ratio) greater than 2 which are presented in Tables 3 and 4 of the reference paper. This is a service provided by NASA HEASARC .