M31CXOXRAY - M31 Central Region Chandra X-Ray Point Source Catalog
All sources in the catalog have S/N > 2.5 and only five have S/N < 3.0. The detection limit for the sources varies across the image due to the variation of exposure time, background, and instrumental PSF, and is highest near the edges, where the PSF broadens rapidly and the exposure time is lowest. Over the inner 4' of the field, the detection limit is 2.1 x 10^-4 ct/s, which is equivalent to an X-ray luminosity of about 2 x 10^35 erg/s.
Additional information about optical identifications and cross-correlated ROSAT X-ray sources not provided in this HEASARC table is available in the published paper (Tables 4 and 5) and/or the CDS at ftp://cdsarc.u-strasbg.fr/pub/cats/J/ApJ/577/738/ (table4.dat & table5.dat).
X-ray point sources in the central region of M31 as seen by Chandra. Kong A.K.H., Garcia M.R., Primini F.A., Murray S.S., di Stefano R., McClintock J.E. <Astrophys. J. 577, 738 (2002)> =2002ApJ...577..738K
The catalog source number, using a nomenclature scheme based on optical studies (Morton et al. 1977, ApJ, 212, 13: a similar classification was also used by Trinchieri and Fabbiano 1991, ApJ, 382, 82). The source numbers have a prefix of either 'r1', 'r2', or 'r3'. The 'r1' sources are located in the central 2'x2' or `inner bulge' region. The 'r2' sources are located in the central 8'x8' region, excluding the inner bulge region; the authors refer to this annular region as the `outer bulge'. The 'r3' sources are located outside the central 8'x8' region in the `disk' region.
The IAU-approved name for a Chandra X-ray source in M 31, of the form CXOM31 JHHMMSS.s+DDMMSS.
The Right Ascension of the X-ray source in the selected equinox. This was given in J2000 coordinates and to a precision of 0.001 seconds of time in the original form of the catalog.
The Declination of the X-ray source in the selected equinox. This was given in J2000 coordinates and to a precision of 0.01 arcseconds in the original form of the catalog.
The Galactic Longitude of the X-ray source.
The Galactic Latitude of the X-ray source.
The positional error, in arcseconds.
The net counts in the X-ray source.
The count rate of the X-ray source, in ct/s, corrected for exposure, background variation and instrumental point spread function. Source count rates were determined via aperture photometry. The radius of the aperture was varied with average off-axis angle in order to match the 90% encircled energy function. The average off-axis angle was computed for each source based on the off-axis angles of the 8 observations weighted by their exposure times. The extraction radius varied from ~1" near the aimpoint to ~17" for the sources with the largest off-axis angles. Background was extracted from an annulus centered on each source. In some cases, for example in the nuclear region, the extraction region was modified to avoid nearby sources. It was also necessary to modify the extraction radius for some faint sources that were close to more liminous sources.
The one-sigma error in the count rate, in ct/s.
The medium-soft hardness ratio HR1 = (M-S)/(M+S) of the X-ray source, where S is the counts in the 0.3-1.0 keV energy band and M is the counts in the 1-2 keV energy band.
The error in the hardness ratio HR1.
The hard-soft hardness ratio HR2 = (H-S)/(H+S) of the X-ray source, where S is the counts in the 0.3-1.0 keV energy band and H is the counts in the 2-7 keV energy band.
The error in the hardness ratio HR2.
The 0.3-7 keV luminosity of the X-ray source, in erg/s. The conversion into X-ray luminosity assumed an absorbed power-law spectrum with a photon index of 1.7 and a hydrogen column density of 10^21 atoms/cm^2, which is the typical spectrum of a point source in M 31 according to Shirey et al. (2001, A&A, 365, L195).
A parameter containing notes codes as follows:
Value Meaning e = Extragalactic object f = Foreground star g = Globular Cluster p = Planetary nebula r = ROSAT HRI source s = Supernova remnant v = Variable sv = Spectral variable t = Transient