Master Sources Table
Each distinct Xray source identified on the sky is represented in the catalog by a single "master source" entry and one or more "source observation" entries, one for each observation in which the source has been detected. The master source entry records the best estimates of the properties of a source, based on the data extracted from the set of observations in which the source has been detected.
Note: Source properties in the catalog which have a value for each science energy band (type "double[6]" and "integer[6]" in the table below) have the corresponding letters appended to their names. For example, "flux_aper_b" and "flux_aper_h" represent the backgroundsubtracted, aperturecorrected broadband and hardband energy fluxes, respectively.
Column Name  Type  Units  Description 

acis_hetg_num  integer  total number of ACIS/HETG observations contributing to the Master Source Catalog record of the source  
acis_hetg_time  double  total ACIS/HETG observation exposure time (seconds of good time) for all ACIS/HETG observations contributing to the Master Source Catalog record of the source  
acis_letg_num  integer  total number of ACIS/LETG observations contributing to the Master Source Catalog record of the source  
acis_letg_time  double  total ACIS/LETG observation exposure time (seconds of good time) for all ACIS/LETG observations contributing to the Master Source Catalog record of the source  
acis_num  integer  total number of ACIS imaging observations contributing to the Master Source Catalog record of the source  
acis_time  double  total ACIS imaging exposure time (seconds of good time) for all ACIS imaging observations contributing to the Master Source Catalog record of the source  
apec_abund  double  bestfit metal abundances (Abundanc)  
apec_abund_hilim  double  upper confidence limit on "apec_abund"  
apec_abund_lolim  double  lower confidence limit on "apec_abund"  
apec_abund_rhat  double  convergence criterion for "apec_abund"  
apec_kt  double  keV  bestfit APEC plasma temperature (kT) 
apec_kt_hilim  double  keV  upper confidence limit on "apec_kt" 
apec_kt_lolim  double  keV  lower confidence limit on "apec_kt" 
apec_kt_rhat  double  convergence criterion for "apec_kt"  
apec_nh  double  N _{HI atoms} 10^{20} cm^{2}  total neutral Hydrogen absorbing column density, N_{H}, derived from the bestfitting APEC plasma model spectral fits to the PI event data extracted from the source region 
apec_nh_hilim  double  N _{HI atoms} 10^{20} cm^{2}  upper confidence limit on "apec_nh" 
apec_nh_lolim  double  N _{HI atoms} 10^{20} cm^{2}  lower confidence limit on "apec_nh" 
apec_nh_rhat  double  convergence criterion for "apec_nh"  
apec_norm  double  normalization factor of the best fitting APEC plasma model  
apec_norm_hilim  double  upper confidence limit on "apec_norm"  
apec_norm_lolim  double  lower confidence limit on "apec_norm"  
apec_norm_rhat  double  convergence criterion for "apec_norm"  
apec_stat  double  χ^{2} (data variance) statistic per degree of freedom for the bestfitting absorbed APEC spectral fit  
apec_z  double  bestfit APEC redshift (z)  
apec_z_hilim  double  upper confidence limit on "apec_z"  
apec_z_lolim  double  lower confidence limit on "apec_z"  
apec_z_rhat  double  convergence criterion for "apec_z"  
bb_ampl  double  amplitude of the best fitting blackbody model spectral fit to the PI event data extracted from the source region  
bb_ampl_hilim  double  upper confidence limit on "bb_ampl"  
bb_ampl_lolim  double  lower confidence limit on "bb_ampl"  
bb_ampl_rhat  double  convergence criterion for "bb_ampl"  
bb_kt  double  keV  temperature of the bestfitting blackbody model spectral fit to the PI event data extracted from the source region 
bb_kt_hilim  double  keV  upper confidence limit on "bb_kt" 
bb_kt_lolim  double  keV  lower confidence limit on "bb_kt" 
bb_kt_rhat  double  convergence criterion for "bb_kt"  
bb_nh  double  N _{HI atoms} 10^{20} cm^{2}  total neutral Hydrogen absorbing column density, N_{H}, derived from the bestfitting thermal (black body) model spectral fits to the PI event data extracted from the source region 
bb_nh_hilim  double  N _{HI atoms} 10^{20} cm^{2}  upper confidence limit on "bb_nh" 
bb_nh_lolim  double  N _{HI atoms} 10^{20} cm^{2}  lower confidence limit on "bb_nh" 
bb_nh_rhat  double  convergence criterion for "bb_nh"  
bb_stat  double  χ^{2} (data variance) statistic per degree of freedom for the bestfitting absorbed blackbody spectral fit  
brems_kt  double  keV  bestfit thermal bremsstrahlung temperature (kT) 
brems_kt_hilim  double  keV  upper confidence limit on "brems_kt" 
brems_kt_lolim  double  keV  lower confidence limit on "brems_kt" 
brems_kt_rhat  double  convergence criterion for "brems_kt"  
brems_nh  double  N _{HI atoms} 10^{20} cm^{2}  total neutral Hydrogen absorbing column density, N_{H}, derived from the bestfitting thermal bremsstrahlung model spectral fits to the PI event data extracted from the source region 
brems_nh_hilim  double  N _{HI atoms} 10^{20} cm^{2}  upper confidence limit on "brems_nh" 
brems_nh_lolim  double  N _{HI atoms} 10^{20} cm^{2}  lower confidence limit on "brems_nh" 
brems_nh_rhat  double  convergence criterion for "brems_nh"  
brems_norm  double  normalization factor of the best fitting thermal bremsstrahlung model  
brems_norm_hilim  double  upper confidence limit on "brems_norm"  
brems_norm_lolim  double  lower confidence limit on "brems_norm"  
brems_norm_rhat  double  convergence criterion for "brems_norm"  
brems_stat  double  χ^{2} (data variance) statistic per degree of freedom for the bestfitting absorbed thermal bremsstrahlung spectral fit  
conf_flag  Boolean  Indicates that source is in a confused region. FALSE  the source detection region is not confused [i.e. not found to contain multiple sources, does not overlap other source detection regions, and contains no overlapping source ellipses in all contributing observations]; otherwise, TRUE  
dec  double  deg  Source position, ICRS declination 
dither_warning_flag  boolean  TRUE if the highest statistically significant peak in the power spectrum of the source region count rate for each science energy band occurs either at the dither frequency of the observation or at a beat frequency of the dither frequency. Otherwise, the value is FALSE.  
err_ellipse_ang  double  deg  position angle of the major axis (referenced from local true north) of the 95% confidence level error ellipse 
err_ellipse_r0  double  arcseconds  major radius of the 95% confidence level error ellipse of the source position 
err_ellipse_r1  double  arcseconds  minor radius of the 95% confidence level error ellipse of the source position 
extent_flag  Boolean  Indicates an extended source. TRUE  deconvolved source extent is inconsistent with a point source at the 90% confidence level in any science energy band with a flux significance >= 3.0 in any contributing observation; otherwise, FALSE  
flux_apec  double  ergs s^{1} cm^{2}  integrated 0.57.0 keV flux derived from the bestfitting APEC thermal plasma model spectral fit 
flux_apec_aper  double[6]  ergs s^{1} cm^{2}  APEC model energy flux inferred from the modified source region for each science energy band 
flux_apec_aper90  double[6]  ergs s^{1} cm^{2}  APEC model energy flux inferred from the modified elliptical aperture for each science energy band 
flux_apec_aper90_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_apec_aper90" values 
flux_apec_aper90_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_apec_aper90" values 
flux_apec_aper_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_apec_aper" values 
flux_apec_aper_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_apec_aper" values 
flux_apec_hilim  double  ergs s^{1} cm^{2}  upper confidence limit on "flux_apec" 
flux_apec_lolim  double  ergs s^{1} cm^{2}  lower confidence limit on "flux_apec" 
flux_aper  double[6]  ergs s^{1} cm^{2}  backgroundsubtracted, aperturecorrected energy fluxes for each science energy band, calculated from counts in the source region using the `direct' flux algorithm 
flux_aper90  double[6]  ergs s^{1} cm^{2}  backgroundsubtracted, aperturecorrected energy fluxes for each science energy band, calculated from counts in the elliptical aperture that includes the 90% Encircled Counts Fraction of the PSF at the source location, using the `direct' flux algorithm 
flux_aper90_avg  double[6]  ergs s^{1} cm^{2}  average backgroundsubtracted, aperturecorrected energy fluxes from the 90% Encircled Counts Fraction of the PSF at the source location for each science energy band 
flux_aper90_avg_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits for "flux_aper90_avg" values for each science energy band 
flux_aper90_avg_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits for "flux_aper90_avg" values for each science energy band 
flux_aper90_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits for "flux_aper90" values for each science energy band 
flux_aper90_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits for "flux_aper90" values for each science energy band 
flux_aper_avg  double[6]  ergs s^{1} cm^{2}  average source region aperturecorrected photon fluxes for each science energy band 
flux_aper_avg_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits for "flux_aper_avg" values for each science energy band 
flux_aper_avg_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits for "flux_aper_avg" values 
flux_aper_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits for "flux_aper" values for each science energy band 
flux_aper_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits for "flux_aper" values 
flux_bb  double  ergs s^{1} cm^{2}  integrated 0.57.0 keV flux of the bestfitting absorbed blackbody model spectral fit 
flux_bb_aper  double[6]  ergs s^{1} cm^{2}  backgroundsubtracted, aperturecorrected energy fluxes for each science energy band, calculated from counts in the source region by scaling a fixed blackbody spectral model 
flux_bb_aper90  double[6]  ergs s^{1} cm^{2}  backgroundsubtracted, aperturecorrected energy fluxes for each science energy band, calculated from counts in an elliptical aperture that includes the 90% Encircled Counts Fraction of the PSF at the source location, by scaling a fixed blackbody spectral model 
flux_bb_aper90_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_bb_aper90" values 
flux_bb_aper90_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_bb_aper90" values 
flux_bb_aper_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_bb_aper" values 
flux_bb_aper_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_bb_aper" values 
flux_bb_hilim  double  ergs s^{1} cm^{2}  upper confidence limit on "flux_bb" 
flux_bb_lolim  double  ergs s^{1} cm^{2}  lower confidence limit on "flux_bb" 
flux_brems  double  ergs s^{1} cm^{2}  integrated 0.57.0 keV flux derived from the bestfitting thermal bremsstrahlung spectral fit 
flux_brems_aper  double[6]  ergs s^{1} cm^{2}  bremsstrahlung model energy flux inferred from the modified source region for each science energy band 
flux_brems_aper90  double[6]  ergs s^{1} cm^{2}  bremsstrahlung model energy flux inferred from the modified elliptical aperture for each science energy band 
flux_brems_aper90_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_brems_aper90" values 
flux_brems_aper90_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_brems_aper90" values 
flux_brems_aper_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_brems_aper" values 
flux_brems_aper_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_brems_aper" values 
flux_brems_hilim  double  ergs s^{1} cm^{2}  upper confidence limit on "flux_brems" 
flux_brems_lolim  double  ergs s^{1} cm^{2}  lower confidence limit on "flux_brems" 
flux_powlaw  double  ergs s^{1} cm^{2}  integrated 0.57.0 keV energy flux for best fit powerlaw model spectral fit to the PI event data extracted from the source region 
flux_powlaw_aper  double[6]  ergs s^{1} cm^{2}  backgroundsubtracted, aperturecorrected energy fluxes for each science energy band, calculated from counts in the source region by scaling a fixed powerlaw spectral model 
flux_powlaw_aper90  double[6]  ergs s^{1} cm^{2}  backgroundsubtracted, aperturecorrected energy fluxes for each science energy band, calculated from counts in an elliptical aperture that includes the 90% Encircled Counts Fraction of the PSF at the source location by scaling a fixed powerlaw spectral model 
flux_powlaw_aper90_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_powlaw_aper90" values 
flux_powlaw_aper90_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_powlaw_aper90" values 
flux_powlaw_aper_hilim  double[6]  ergs s^{1} cm^{2}  upper confidence limits on "flux_powlaw_aper" values 
flux_powlaw_aper_lolim  double[6]  ergs s^{1} cm^{2}  lower confidence limits on "flux_powlaw_aper" values 
flux_powlaw_hilim  double  ergs s^{1} cm^{2}  upper confidence limit on "flux_powlaw" 
flux_powlaw_lolim  double  ergs s^{1} cm^{2}  lower confidence limit on "flux_powlaw" 
gal_b  double  deg  Source position, galactic latitude (equinox J2000.0, epoch J2000.0) 
gal_l  double  deg  Source position, galactic longitude (equinox J2000.0, epoch J2000.0) 
hard_hm  double  hardness ratio of the hard to medium ACIS science energy bands  
hard_hm_hilim  double  upper confidence limit on "hard_hm" value  
hard_hm_lolim  double  lower confidence limit on "hard_hm" value  
hard_hs  double  hardness ratio of the hard to soft ACIS science energy bands  
hard_hs_hilim  double  upper confidence limit on "hard_hs" value  
hard_hs_lolim  double  lower confidence limit on "hard_hs" value  
hard_ms  double  hardness ratio of the medium to soft ACIS science energy bands  
hard_ms_hilim  double  upper confidence limit on "hard_ms" value  
hard_ms_lolim  double  lower confidence limit on "hard_ms" value  
hrc_hetg_num  integer  total number of HRC/HETG observations contributing to the Master Source Catalog record of the source  
hrc_hetg_time  double  total HRC/HETG observation exposure time (seconds of good time) for all HRC/HETG observations contributing to the Master Source Catalog record of the source  
hrc_letg_num  integer  total number of HRC/LETG observations contributing to the Master Source Catalog record of the source  
hrc_letg_time  double  total HRC/LETG observation exposure time (seconds of good time) for all HRC/LETG observations contributing to the Master Source Catalog record of the source  
hrc_num  integer  total number of HRC imaging observations contributing to the Master Source Catalog record of the source  
hrc_time  double  total HRC imaging exposure time (seconds of good time) for all HRC imaging observations contributing to the Master Source Catalog record of the source  
kp_intra_prob  double[6]  Intraobservation Kuiper's test variability probability, i.e. probability that the source is variable within an observation, in each of the science energy bands, using Kuiper's test. (Highest value among contributing observations used).  
ks_intra_prob  double[6]  Intraobservation KolmogorovSmirnov variability probability, i.e. probability that the source is variable within an observation, in each of the science energy bands, using the KS test. (Highest value among contributing observations used).  
likelihood  double  highest source detection loglikelihood across all stacked observations and science energy bands  
likelihood_class  string  highest detection likelihood classification across all stacked observations and science energy bands  
major_axis  double[6]  arcseconds  1σ radius along the major axis of the ellipse defining the deconvolved source extent for each science energy band 
major_axis_hilim  double[6]  arcseconds  upper limit on the 68% confidence interval of the deconvolved source extent major axis for each science energy band 
major_axis_lolim  double[6]  arcseconds  lower limit on the 68% confidence interval of the deconvolved source extent major axis for each science energy band 
man_add_flag  Boolean  Indicates a source added manually. TRUE  the source region was manually added by human review; otherwise, FALSE  
man_inc_flag  Boolean  Indicates a source identified manually (automatic detection failed). TRUE  the source region was manually included in all of the contributing observations by human review; otherwise, FALSE  
man_match_flag  Boolean  Indicates that source observations were manually merged. TRUE  the set of individual source observations contributing to the current master source observation region was manually selected and modified by human review; otherwise, FALSE  
man_pos_flag  Boolean  Indicates that source position were manually adjusted. TRUE  the source region position were manually modified in all of the contributing observations by human review; otherwise, FALSE  
man_reg_flag  Boolean  Indicates that source parameters were manually adjusted due to pileup. TRUE  the source region parameters were manually modified in all of the contributing observations by human review [in the event of extreme pileup]; otherwise, FALSE  
minor_axis  double[6]  arcseconds  1σ radius along the minor axis of the ellipse defining the deconvolved source extent for each science energy band 
minor_axis_hilim  double[6]  arcseconds  upper limit on the 68% confidence interval of the deconvolved source extent minor axis for each science energy band 
minor_axis_lolim  double[6]  arcseconds  lower limit on the 68% confidence interval of the deconvolved source extent minor axis for each science energy band 
name  string  source name in the form "2CXO Jhhmmss.s{+}ddmmss" [Chandra source names use the ICRS position to an accuracy of 0.1s in RA and 1.0s in Dec.]  
nh_gal  double  N _{HI atoms} 10^{20} cm^{2}  Galactic neutral Hydrogen column density, N_{H}, in the direction of the source [determined from the interpolation data of Dickey and Lockman (1990; Ann. Rev. Astron. Astrophys., 28, 215)] 
phot_nsrcs  long  number of sources simultaneously fit to compute aperture photometry quantitites  
photflux_aper  double[6]  photons s^{1} cm^{2}  backgroundsubtracted, aperturecorrected photon fluxes for each science energy band, calculated from counts in the source region using the `direct' flux algorithm 
photflux_aper90  double[6]  photons s^{1} cm^{2}  backgroundsubtracted, aperturecorrected photon fluxes for each science energy band, calculated from counts in the elliptical aperture that includes the 90% Encircled Counts Fraction of the PSF at the source location using the `direct' flux algorithm 
photflux_aper90_avg  double[6]  photons s^{1} cm^{2}  average backgroundsubtracted, aperturecorrected photon fluxes from the 90% Encircled Counts Fraction of the PSF at the source location for each science energy band 
photflux_aper90_avg_hilim  double[6]  photons s^{1} cm^{2}  upper confidence limits for "photflux_aper90_avg" values for each science energy band 
photflux_aper90_avg_lolim  double[6]  photons s^{1} cm^{2}  lower confidence limits for "photflux_aper90_avg" values for each science energy band 
photflux_aper90_hilim  double[6]  photons s^{1} cm^{2}  upper confidence limits for "photflux_aper90" values for each science energy band 
photflux_aper90_lolim  double[6]  photons s^{1} cm^{2}  lower confidence limits for "photflux_aper90" values for each science energy band 
photflux_aper_avg  double[6]  photons s^{1} cm^{2}  average source region aperturecorrected photon fluxes for each science energy band 
photflux_aper_avg_hilim  double[6]  photons s^{1} cm^{2}  upper confidence limits for "photflux_aper_avg" values for each science energy band 
photflux_aper_avg_lolim  double[6]  photons s^{1} cm^{2}  lower confidence limits for "photflux_aper_avg" values 
photflux_aper_hilim  double[6]  photons s^{1} cm^{2}  upper confidence limits for "photflux_aper" values for each science energy band 
photflux_aper_lolim  double[6]  photons s^{1} cm^{2}  lower confidence limits for "photflux_aper" values for each science energy band 
pileup_flag  Boolean  Indicates that the source properties may be affected by ACIS pileup. FALSE  the pileup fraction does not exceed ~10% for all contributing ACIS observations and source detection energy bands; otherwise, TRUE  
pos_angle  double[6]  deg  position angle of the major axis of the ellipse defining the deconvolved source extent for each science energy band (referenced from local true north) 
pos_angle_hilim  double[6]  deg  upper limit on the 68% confidence interval of the deconvolved source extent position angle for each science energy band 
pos_angle_lolim  double[6]  deg  lower limit on the 68% confidence interval of the deconvolved source extent position angle for each science energy band 
powlaw_ampl  double  amplitude of the best fitting powerlaw model spectral fit to the PI event data extracted from the source region  
powlaw_ampl_hilim  double  upper confidence limit on "powlaw_ampl"  
powlaw_ampl_lolim  double  lower confidence limit on "powlaw_ampl"  
powlaw_ampl_rhat  double  convergence criterion for "powlaw_ampl"  
powlaw_gamma  double 
photon index (γ, defined as F_{E}~E^{γ})
for bestfit powerlaw model
spectral fit to the PI event data extracted from the
source region 

powlaw_gamma_hilim  double  upper confidence limit for "powlaw_gamma"  
powlaw_gamma_lolim  double  lower confidence limit for "powlaw_gamma"  
powlaw_gamma_rhat  double  convergence criterion for "powlaw_gamma"  
powlaw_nh  double  N _{HI atoms} 10^{20} cm^{2}  total neutral Hydrogen absorbing column density, N_{H}, of the best fitting powerlaw model spectral fit to the PI event data extracted from the source region 
powlaw_nh_hilim  double  N _{HI atoms} 10^{20} cm^{2}  upper confidence limit on "powlaw_nh" 
powlaw_nh_lolim  double  N _{HI atoms} 10^{20} cm^{2}  lower confidence limit on "powlaw_nh" 
powlaw_nh_rhat  double  convergence criterion for "powlaw_nh"  
powlaw_stat  double  χ^{2} (data variance) statistic per degree of freedom for the bestfitting absorbed power law spectral fit  
ra  double  deg  Source position, ICRS right ascension 
sat_src_flag  Boolean  Indicates a saturated source (strong ACIS pileup). TRUE  all of the contributing observations are ACIS observations that are significantly piledup [to the extent that the source image may be flattened or have a central hole]; otherwise, FALSE.  
significance  double  highest value of source flux significance (S/N) across all stacked observations and science energy bands  
src_area  double[6]  sq. arcseconds  area of the deconvolved source extent ellipse, or area of the source polygon for extended sources for each science energy band 
streak_src_flag  Boolean  Indicates that source lies on an ACIS readout streak. TRUE  all of the contributing observations are ACIS observations and contain source regions that overlap a defined region enclosing an identified readout streak; otherwise, FALSE  
var_flag  Boolean  FALSE  variability is not detected within any single observation or between any pair of observations, in any science energy band; otherwise, TRUE  
var_inter_hard_flag  Boolean  Indicates that the source hardness ratios are variable. TRUE  the hardness ratios of at least one of the contributing individual source observations are statistically inconsistent with the corresponding hardness ratios of all of the other contributing individual source observations; otherwise, FALSE  
var_inter_hard_prob_hm  double  interObI hardness ratio variability probability of the hard to medium ACIS science energy bands  
var_inter_hard_prob_hs  double  interObI hardness ratio variability probability of the hard to soft ACIS science energy bands  
var_inter_hard_prob_ms  double  interObI hardness ratio variability probability of the medium to soft ACIS science energy bands  
var_inter_index  integer[6]  Interobservation variability index in the range [0,10] that indicates if the source region photon flux is constant between the contributing observations, in each of the science energy bands.  
var_inter_prob  double[6]  Interobservation source variability probability, i.e. the probability that the source region photon flux varied between the contributing observations, in each of the science energy bands, using the χ^{2} distribution of the photon fluxes and the standard deviations of the individual observations.  
var_inter_sigma  double[6]  photons s^{1} cm^{2}  Interobservation flux variability, i.e. the spread of the source region photon flux densities of the individual observations about the error weighted mean source region photon flux density, in each of the science energy bands. (Highest value of flux variability among contributing observations used). 
var_inter_sigma_prob_hm  double  interObI hardness ratio variability standard deviation of the hard to medium ACIS science energy bands  
var_inter_sigma_prob_hs  double  interObI hardness ratio variability standard deviation of the hard to soft ACIS science energy bands  
var_inter_sigma_prob_ms  double  interObI hardness ratio variability standard deviation of the medium to soft ACIS science energy bands  
var_intra_index  integer[6]  Intraobservation variability index in the range [0,10] that indicates if the source region flux is uniform throughout an observation, in each of the science energy bands, using a GregoryLoredo analysis. (Highest value among contributing observations used).  
var_intra_prob  double[6]  Intraobservation GregoryLoredo variability probability, i.e. probability that the source is variable within an observation, in each of the science energy bands, using a GregoryLoredo analysis. (Highest value among contributing observations used). 