ETGALCXO - Early-Type Galaxies Chandra X-Ray Point Source Catalog
This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D25 restriction should mitigate against contamination by background AGNs.
Low-Mass X-Ray Binaries and Globular Clusters in Early-Type Galaxies. I. Chandra Observations Humphrey P. J., Buote D. A. <Astrophys. J. 689, 983-1004 (2008) =2008ApJ...689..983H
The Chandra X-ray Observatory (CXO) X-ray designation, using the standard 'CXOU J' prefix and the J2000.0 equatorial source position.
The name of the host galaxy in which the Chandra X-ray source is located.
The Right Ascension of the Chandra X-ray source in the selected equinox. This was constructed from the positional part of the X-ray source name, and so has a precision of 0.1 seconds of time.
The Declination of the Chandra X-ray source in the selected equinox. This was constructed from the positional part of the X-ray source name, and so has a precision of 1 arcsecond.
The Galactic Longitude of the Chandra X-ray source.
The Galactic Latitude of the Chandra X-ray source.
The background-subtracted total-band X-ray counts in the Chandra source.
The X-ray (0.3 - 7 keV) luminosity of the Chandra point source, in erg/s, calculated from the observed X-ray flux and assuming that it is at the distance of its host galaxy (see Table 1 of the reference paper). The authors adopted a simple power-law model, with Gamma = 1.55 , which has been shown to fit adequately the composite spectra of detected LMXBs (see also Section 3.3 of the reference paper and Irwin et al. 2003, ApJ, 587, 356) and modified by photoelectric absorption due to the Galactic ISM along the line of sight (Dickey & Lockman 1990, ARAA, 28, 215). Such a model is broadly consistent with the source hardness ratios (see Section 3.1 of the reference paper), and models of a similar shape have also been fitted to the spectra of LMXBs within the Milky Way. This model was folded through the response matrices generated at each source position, and used to infer a counts-to-flux conversion ratio in the 0.3 - 7.0 keV band. The 0.3 - 7.0 keV background-subtracted flux of each source was extracted from the same region that was defined from which to extract the spectrum.
The uncertainty in the Chandra X-ray source (0.3 - 7 keV) luminosity, in erg/s.
The X-ray source spectral hardness ratio HR1 = (S - M)/(S + M), where S is the background-subtracted count rate in the band from 0.3 - 1.5 keV, and M is the count rate in the band from 1.5 - 3.0 keV.
The uncertainty in the X-ray source spectral hardness ratio HR1.
The X-ray source spectral hardness ratio HR2 = (M - H)/(M + H), where M is the background-subtracted count rate in the band from 1.5 - 3.0 keV, and H is the count rate in the band from 3.0 - 5.0 keV.
The uncertainty in the X-ray source spectral hardness ratio HR2.
The projected distance of the X-ray source from the galaxy center, in arcminutes.
For those LMXBs within the appropriate WFPC2 field, the authors list here the GC catalog number given in Humphrey (2009, ApJ, 690, 512: Paper II) for any which match GCs. If the source has no match, the authors report "none" for this field, and if the source is not in the WFPC2 field, it is left blank.