0X  A18     ---   CXOU     X-ray source name; CXOU J(HHMMSS.ss+DDMMSS.s) (Name)
1X  A7      ---   Label   Source name generated by ACIS Extract (Label) (1)
1X  F10.6   deg   RAdeg    Right Ascension in decimal degrees (J2000) (RAdeg)
1X  F10.6   deg   DEdeg    Declination in decimal degrees (J2000) (DEdeg)
1X  F8.6   arcsec  ePos     1{sigma} error circle around (RAdeg, DEdeg) (PosErr)
1X  A17     ---   PosType   Algorithm used to estimate position (Broos et al. 2010ApJ...714.1582B, Section 7.1) (PosType)
1X  E12.7 --- no-m         Smallest of no-t, no-s and no-h (ProbNoSrc_min) (2)
1X  E12.7   --- no-t    p-value for no-source hypothesis in the total (0.5-8 keV) energy band (Broos et al. 2010ApJ...714.1582B, Section 4.3) (ProbNoSrc_t) (2)
1X  E12.7   --- no-s  ? p-value for 0.5-2 keV no-source hypothesis in the soft (0.5-2 keV) energy band (ProbNoSrc_s) (2)
1X  E12.7   --- no-h  ? p-value for 2-8 keV no-source hypothesis in the hard (2-8 keV) energy band (ProbNoSrc_h) (2)
1X  E12.7 --- KS-s ? Smallest p-value for the one-sample Kolmogorov-Smirnov statistic under the no-variability null hypothesis within a single observation (ProbKS_single) (3)
1X  E12.7  --- KS-m ? Smallest p-value for the one-sample Kolmogorov-Smirnov statistic under the no-variability null hypothesis over merged observations (ProbKS_merge) (3)
1X  F8.1  s ExpNom Total exposure time in merged observations (ExposureTimeNominal)
1X  F8.6  --- ExpFrac  Fraction of ExpNom that source was observed (ExposureFraction) (4)
1X  I1  --- Nobs  Total number of observations extracted (NumObservations)
1X  I1      ---   Nph  Number of observations merged to estimate photometry properties (NumMerged)
1X  F8.6    ---   Fdis  Fraction of exposure discarded in merge (MergeBias)
1X  F9.6   arcmin theta-m     Smallest off-axis angle for merged observations (Theta_Lo)
1X  F9.6   arcmin theta       Average off-axis angle {theta} for merged observations (Theta)
1X  F9.6   arcmin theta-M    Largest off-axis angle for merged observations (Theta_Hi)
1X  F8.6    --- PSFf  Average PSF fraction (at 1.5 keV) for merged observations (PsfFraction)
1X  F10.5 ---  Area   Average aperture area for merged observations (in units of (0.492arcsec)^2^) (SrcArea)
1X  F7.5  --- aglow ? Suspected afterglow fraction (AfterglowFraction) (5)
1X  I4      ct  Oct-t  Observed 0.5-8 keV counts in merged apertures (SrcCounts_t)
1X  I4      ct  Oct_s  Observed 0.5-2 keV counts in merged apertures (SrcCounts_s)
1X  I3      ct  Oct-h   Observed 2-8 keV counts in merged apertures (SrcCounts_h)
1X  F10.6   ---  bgScl      Scaling of the background extraction (Broos et al. 2010ApJ...714.1582B, Section 5.4) (BkgScaling)
1X  I4      ct  bgct-t   Observed 0.5-8 keV counts in merged background regions (BkgCounts_t)
1X  I4      ct  bgct-s Observed 0.5-2 keV counts in merged background regions (BkgCounts_s)
1X  I3      ct  bgct-h  Observed 2-8 keV counts in merged background regions (BkgCounts_h)
1X  F10.5   ct  Nct-t  Net 0.5-8 keV counts in merged apertures (NetCounts_t)
1X  F10.5   ct  Nct-s   Net 0.5-2 keV counts in merged apertures (NetCounts_s)
1X  F9.5    ct  Nct-h   Net 2-8 keV counts in merged apertures (NetCounts_h)
1X  F10.5 ct b_Nct-t    1{sigma} lower bound on Nct-t (NetCounts_Lo_t) (6)
1X  F10.5 ct B_Nct-t  1{sigma} upper bound on Nct-t (NetCounts_Hi_t) (6)
1X  F10.5 ct b_Nct-s ? 1{sigma} lower bound on Nct-s (NetCounts_Lo_s) (6)
1X  F10.5 ct B_Nct-s 1{sigma} upper bound on Nct-s (NetCounts_Hi_s) (6)
1X  F9.5  ct  b_Nct-h ? 1{sigma} lower bound on Nct-h (NetCounts_Lo_h) (6)
1X  F9.5  ct B_Nct-h   1{sigma} upper bound on Nct-h (NetCounts_Hi_h) (6)
1X  F8.4  cm2.ct/ph Area-t Mean 0.5-8 keV ARF value (MeanEffectiveArea_t) (7)
1X  F8.4  cm2.ct/ph Area-s Mean 0.5-2 keV ARF value (MeanEffectiveArea_s) (7)
1X  F8.4  cm2.ct/ph Area-h Mean 2-8 keV ARF value (MeanEffectiveArea_h)(7)
1X  F6.4  keV E-t    Median 0.5-8 keV energy, observed spectrum (MedianEnergy_t) (8)
1X  F6.4  keV E-s ? Median 0.5-2 keV energy, observed spectrum (MedianEnergy_s) (8) 
1X  F6.4  keV E-h ? Median 2-8 keV energy, observed spectrum (MedianEnergy_h) (8)
1X  F8.5   [ph/cm2/s] XFlx-t  Log incident 0.5-8 keV photon flux (PhotonFlux_t) (9)
1X  F8.5   [ph/cm2/s] XFlx-s ? Log incident 0.5-2 keV photon flux (PhotonFlux_s) (9)
1X  F9.5   [ph/cm2/s] XFlx-h ? Log incident 2-8 keV photon flux (PhotonFlux_h) (9)
1X  E12.7   mW/m2 Flux-h        ? 2-8 keV X-ray flux (in erg/cm^2^/s) (FH)
1X  E12.7   mW/m2 Flxc-h       ? Absorption-corrected 2-8 keV X-ray flux (in erg/cm^2^/s) (FHC)
1X  E12.7  mW/m2 e_Flxc-h ? 1{sigma} statistical uncertainty on Flxc-h (in erg/cm^2^/s) (SF_HC_STAT)
1X  E12.7  mW/m2 s_Flxc-h  ? 1{sigma} systematic uncertainty on F_HC (in erg/cm^2^/s) (SF_HC_SYST)
1X  E12.7  mW/m2  Flux-t        ? 0.5-8 keV X-ray flux (in erg/cm^2^/s) (FT)
1X  E12.7  mW/m2  Flxc-t       ? Absorption-corrected 0.5-8 keV X-ray flux (in erg/cm^2^/s) (FTC)
1X  E12.7  mW/m2 e_Flxc-t ? 1{sigma} statistical uncertainty on Flxc-t (in erg/cm^2^/s) (SF_TC_STAT)
1X  E12.7  mW/m2 s_Flxc-t ? 1{sigma} systematic uncertainty on Flxc-t (in erg/cm^2^/s) (SF_TC_SYST)
1X  F6.3   [cm-2]   logNH    ? Gas column density (LOG_NH)
1X  F6.4  cm-2 e_logNH ? 1{sigma} statistical uncertainty on logNH (SLOG_NH_STAT)
1X  F6.4  cm-2 s_logNH ? 1{sigma} systematic uncertainty on logNH (SLOG_NH_SYST)
1X  F7.4 [10-7W]    logLX-t   ? Log X-ray (0.5-8 keV) luminosity (in erg/s) (LOG_LTC)
1X  F7.4 [10-7W]    logLX-s   ? Log X-ray (0.5-2 keV) luminosity (in erg/s) (LOG_LHC)
1X  F6.4 [10-7W]  e_logLX-t  ? 1{sigma} statistical uncertainty on logLX-t (in erg/s) (ERR_LOG_LTC)
1X  F6.4 [10-7W]  e_logLX-s  ? 1{sigma} statistical uncertainty on logLX-s (in erg/s) (ERR_LOG_LHC)


Note (1): Source labels identify a Chandra pointing; they do not convey 
  membership in astrophysical clusters.
Note (2): Source significance quantities (noSrc-t, noSrc-s, noSrc-h, noSrc-m) 
  are computed using a subset of each source's extractions chosen to maximize 
  significance (Broos et al. 2010ApJ...714.1582B, Section 6.2).
  In statistical hypothesis testing, the p-value is the probability of obtaining
  a test statistic at least as extreme as the one that was actually observed 
  when the null hypothesis is true.
Note (3): See Broos et al. (2010ApJ...714.1582B, Section 7.6) for a description
  of the variability metrics and caveats regarding possible spurious indications
  of variability using the ProbKS_merge metric.
Note (4): Due to dithering over inactive portions of the focal plane, a Chandra
  source is often not observed during some fraction of the nominal exposure 
  time. (See http://cxc.harvard.edu/ciao/why/dither.html.) The reported quantity
  is FRACEXPO produced by the CIAO tool mkarf.
Note (5): Some background events arising from an effect known as "afterglow" 
  (http://cxc.harvard.edu/ciao/why/afterglow.html) may contaminate source 
  extractions, despite careful procedures to identify and remove them during 
  data preparation (Broos et al. 2010ApJ...714.1582B, Section 3). After 
  extraction, we attempt to identify afterglow events using the tool 
  ae_afterglow_report and report the fraction of extracted events attributed to
  afterglow; see the ACIS Extract manual 
  (http://www.astro.psu.edu/xray/acis/acis_analysis.html).
Note (6): Confidence intervals (68%) for NetCounts quantities are estimated by 
  the CIAO tool aprates (http://asc.harvard.edu/ciao/ahelp/aprates.html).
Note (7): The ancillary response file (ARF) in ACIS data analysis represents 
  both the effective area of the observatory and the fraction of the observation
  for which data were actually collected for the source (ExposureFraction).
Note (8): MedianEnergy is the ME of extracted events, corrected for background 
  (Broos et al. 2010ApJ...714.1582B, Section 7.3). 
Note (9): XFlx=(NCt/Area/ExpNom); Broos et al. 2010ApJ...714.1582B, Section 7.4.