The following are the columns in the file chandra_point_sources.fits
You can read this file into IDL if you have the astrolib library 
installed, using 
IDL> data = mrdfits("chandra_point_sources.fits", 1)
data will be a structure. You can access, for example, the right
ascension by 
IDL> help, data.ra, data[12].ra

------------------------------------------------------------------------

(recno) Record locators that can be used to cross-correlate 
with other tables.

(source) The source names, which are derived from the coordinates of the
source based on the IAU format, in which least-significant figures are
{\it truncated} (as opposed to rounded). The names should not be used 
as the locations of the sources.

(ra,dec) The right ascensions and declinations of the sources, in degrees
(J2000).

(unc) The 95\% uncertainties in the positions (the error circles).
There are 5810 sources with uncertainties $\le$1\arcsec\ (half of 
which are within 7\arcmin\ of \sgrastar), and 1950 with uncertainties 
$\le$0\farcs5 (85\% of which are within 7\arcmin\ of \sgrastar).

(pos_flag) Flag indicating how the positions were derived. A ``d''
indicates the position is from the mean position of events, a ``c''
indicates it was derived by cross-correlating the image and the PSF,
and a ``w'' indicates it was derived from a wavelet algorithm. Sources
marked with a ``w'' are likely to be confused with a nearby source, or 
in a region of high background.

(field) The images in which the sources were identified. The tags
``full'', ``2002'', ``2004'', and ``2005'' indicate a source
was found in composite images of the \sgrastar\ field. All other values
are the observations in which a source was detected. Two sources added
manually are tagged with ``hand''.
 
(band) Additional information about how the sources were detected.
The tag ``full'' refers to any source detected with {\tt wavdetect}
in the 0.5--8.0~keV 
band; ``soft'' sources were detected in the 0.5--2.0~keV but not the 
full band; ``hard'' sources were detected in the 4--8~keV band but 
neither of the other two bands. The tag ``tile'' indicates that the 
source was detected in a composite 0.5--8.0~keV image with {\tt wvdecomp}.

(offset) The offsets ($\theta$) from the aim point, in arcmin. If a source 
position was estimated from a composite image, $\theta$ is the mean 
offset weighted by the exposure. If a position was taken from a single
observation, $\theta$ is the offset for that observation. 

(nobs) The number of observations used to compute the photometry 
for each source.

(exp) The exposure times in seconds.

(fpsf) The fractions of the PSF enclosed by the source extraction
regions.

(epsf) The fiducial energies of the PSFs used to construct the source
extraction regions.

(src_rad) The smallest radius for the extraction region that was
used for a source, in arcseconds. This is determined from the
observation in which the source was closest to the aim point. It is 
also an absolute upper bound to the positional uncertainty for a
source.

(pks) The log of the probabilities that the source and background spectra are
derived from the same distribution, according to a
KS test. Large negative values indicate
that the source and background spectra are distinct, and therefore
that the source is most likely real.

(s_src) The total numbers of counts in the 0.5--2.0 keV band.

(s_back) The estimated numbers of background counts in the 0.5--2.0 keV 
band. 

(s_net) The net numbers of counts in the 0.5--2.0 keV band.

(snet_l) Lower uncertainty on the numbers of counts in the 0.5--2.0 keV band.
If the lower uncertaint is greater than or equal to the net counts, then 
the source was not detected in this band. 

(snet_h) Upper uncertainty (90% confidence) on the 0.5--2.0 keV net
counts. If the source is a non- detection, this is the 90% upper
limit.  

(c_src) The total numbers of counts in the 2--8 keV band.

(c_back) The estimated numbers of background counts in the 2--8 keV 
band. 

(c_net) The net numbers of counts in the 2--8 keV band.

(cnet_l) Lower uncertainty on the numbers of counts in the 2--8 keV band.
If the lower uncertaint is greater than or equal to the net counts, then 
the source was not detected in this band. 

(cnet_h) Upper uncertainty (90% confidence) on the 2--8 keV net
counts. If the source is a non- detection, this is the 90% upper
limit.  

(s_flux) The fluxes in the 0.5--2.0 keV band, in units of \phcms.

(c_flux) The fluxes in the 2--8 keV band, in units of \phcms.

(meane) The mean energy of photons in the source region, statistically 
corrected for the background. 

(hr0) The soft colors, 0.5--2.0 keV band vs. 2.0--3.3 keV band. Bounded
by [-1,1]. Values of -9 correspond to non-detection in both bands.
For the hardness ratios, HR = (h-s)/(h+s) where for HR0 h=0.5-2.0 keV
and s=2.0-3.3 keV, and for HR2 h=4.7-8.0 keV and s = 3.3-4.7 keV.
A value of -9 is used if the source is not detected in either band. 
For the uncertainties, -9 indicates either than the source is not detected 
in one or both of the relevant bands. 

To select foreground sources (N_H <~ 10^21 cm^-2; d<2 kpc), choose -1.0 <= HR0
< -0.5.  To select Galactic center sources (N_H > 4e22 cm^-2; D>4 kpc), 
choose HR0 > -0.175 or HR0 = -9. Sources with HR0 in between are probably at
intermediate distances.

(hr0_l) Lower error (90\%) on the soft color. Values of -9 correspond
to non-detections in the 0.5--2.0 keV band. 

(hr0_h) Upper error (90\%) on the hard color. Values of -9 correspond
to non-detections in the 2.0--3.3 keV band. 

(hr1) The soft colors, 2.0--3.3 keV band vs. 3.3--4.7 keV band. Bounded
by [-1,1]. Values of -9 correspond to non-detection in both bands.

(hr1_l) Lower error (90\%) on the soft color. Values of -9 correspond
to non-detections in the 2.0--3.3 keV band. 

(hr1_h) Upper error (90\%) on the hard color. Values of -9 correspond
to non-detections in the 3.3--4.7 keV band. 

(hr2) The soft colors, 3.3--4.7 keV band vs. 4.7--8.0 keV band. Bounded
by [-1,1]. Values of -9 correspond to non-detection in both bands.

(hr2_l) Lower error (90\%) on the soft color. Values of -9 correspond
to non-detections in the 3.3--4.7 keV band. 

(hr2_h) Upper error (90\%) on the hard color. Values of -9 correspond
to non-detections in the 4.7--8.0 keV band. 

(flags) Quality flags: ``c'' for sources confused with another nearby source;
``g'' for sources that fell near the edge of a detector in one or more 
observations; ``b'' for sources four which the source and background 
spectra have a $>$10\% chance of being drawn from the same distribution 
according to a KS test; ``s'' for sources variable on short time scales, 
as indicated by probabilities of $<$1\% that the
event arrival times for at least one observation were consistent with
a uniform distribution according to the KS test; ``l'' for sources that were
variable on long time scales, as indicated by a probability of $<$1\% 
that the fluxes for all observations were consistent with a uniform 
distribution according to the KS test; ``e'' for sources that may be 
part of an extended, diffuse feature \citep{m-diff}; ``x'' for sources
for which the 0.5--2.0~keV band photometry is inaccurate because the 
satellite was programmed to omit photons below 1~keV from the telemetry.
[NOTE: The final tables contain a few extra sourcecs with the ``e'' flag,
and sources flagged as ``p'' beecause they suffered from photon pile-up.
They are not here, because I had to add these flags by hand.]

(p0) Probability that the source is real in the 2-8.0 keV band, 
according to the Poisson test in Weisskopf et al. (2007, ApJ, 657, 1026). 

(p1) Probability that the source is real in the 0.5-2.0 keV band, 
according to the Poisson test in Weisskopf et al. (2007, ApJ, 657, 1026). 

(p2) Probability that the source is real in the 2.0-3.3 keV band, 
according to the Poisson test in Weisskopf et al. (2007, ApJ, 657, 1026). 

(p3) Probability that the source is real in the 3.3-4.7 keV band, 
according to the Poisson test in Weisskopf et al. (2007, ApJ, 657, 1026). 

(p4) Probability that the source is real in the 4.7-8.0 keV band, 
according to the Poisson test in Weisskopf et al. (2007, ApJ, 657, 1026). 

(fsens) The 50\% completeness limit at the position of the source. Sources
brighter than these completeness limits can be used to compute spatial
and flux distributions, although the sensitivity map (Fig.~\ref{fig:sens})
is need to compute the corresponding survey area. 

(snet_flag) Has value "<" if the net counts in the 0.5--2.0 keV band are an 
upper limit.

(cnet_flag) Has value "<" if the net counts in the 2--8 keV band are an upper 
limit.

(sflux_flag) Has value "<" if the net counts in the 0.5--2.0 keV band are an 
upper limit.

(flux_flag) Has value "<" if the net counts in the 2--8 keV band are an upper 
limit.