Master Sources Table
Each distinct X-ray source identified on the sky is represented in the catalog by a single "master source" entry and one or more "per-observation detection" 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 background-subtracted, aperture-corrected broad-band and hard-band energy fluxes, respectively.
Column Name | Type | Units | Description |
---|---|---|---|
acis_hetg_num | integer | total number of ACIS/HETG observations contributing to the Master Sources Table record of the source | |
acis_hetg_time | double | total livetime for all ACIS/HETG observations contributing to the Master Sources Table record of the source | |
acis_letg_num | integer | total number of ACIS/LETG observations contributing to the Master Sources Table record of the source | |
acis_letg_time | double | total livetime for all ACIS/LETG observations contributing to the Master Sources Table record of the source | |
acis_num | integer | total number of ACIS imaging observations contributing to the Master Sources Table record of the source | |
acis_time | double | total livetime for all ACIS imaging observations contributing to the Master Sources Table record of the source | |
apec_abund | double | abundance of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_abund_hilim | double | abundance of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upper confidence limit) | |
apec_abund_lolim | double | abundance of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | |
apec_abund_rhat | double | abundance convergence criterion of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_kt | double | keV | temperature (kT) of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum |
apec_kt_hilim | double | keV | temperature (kT) of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
apec_kt_lolim | double | keV | temperature (kT) of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
apec_kt_rhat | double | temperature (kT) convergence criterion of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_nh | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum |
apec_nh_hilim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
apec_nh_lolim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
apec_nh_rhat | double | N_{H} column density convergence criterion of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_norm | double | amplitude of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_norm_hilim | double | amplitude of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upperer confidence limit) | |
apec_norm_lolim | double | amplitude of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | |
apec_norm_rhat | double | amplitude convergence criterion of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_stat | double | χ^{2} statistic per degree of freedom of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_z | double | redshift of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
apec_z_hilim | double | redshift of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upper confidence limit) | |
apec_z_lolim | double | redshift of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | |
apec_z_rhat | double | redshift convergence criterion Redshift of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
bb_ampl | double | amplitude of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum | |
bb_ampl_hilim | double | amplitude of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% upperer confidence limit) | |
bb_ampl_lolim | double | amplitude of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | |
bb_ampl_rhat | double | amplitude convergence criterion of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum | |
bb_kt | double | keV | temperature (kT) of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum |
bb_kt_hilim | double | keV | temperature (kT) of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
bb_kt_lolim | double | keV | temperature (kT) of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
bb_kt_rhat | double | temperature (kT) convergence criterion of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum | |
bb_nh | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum |
bb_nh_hilim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
bb_nh_lolim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
bb_nh_rhat | double | N_{H} column density convergence criterion of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum | |
bb_stat | double | χ^{2} statistic per degree of freedom of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum | |
brems_kt | double | keV | temperature (kT) of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum |
brems_kt_hilim | double | keV | temperature (kT) of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
brems_kt_lolim | double | keV | temperature (kT) of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
brems_kt_rhat | double | temperature (kT) convergence criterion of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum | |
brems_nh | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum |
brems_nh_hilim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
brems_nh_lolim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
brems_nh_rhat | double | N_{H} column density convergence criterion of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum | |
brems_norm | double | amplitude of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum | |
brems_norm_hilim | double | amplitude of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% upperer confidence limit) | |
brems_norm_lolim | double | amplitude of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | |
brems_norm_rhat | double | amplitude convergence criterion of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum | |
brems_stat | double | χ^{2} statistic per degree of freedom of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum | |
conf_flag | Boolean | source may be confused (source and/or background regions overlap in one or more contributing stacked observations) | |
dec | double | deg | source position, ICRS declination |
dither_warning_flag | boolean | highest statistically significant peak in the power spectrum of the source region count rate occurs at the dither frequency or at a beat frequency of the dither frequency in one or more observations | |
err_ellipse_ang | double | deg | position angle (referenced from local true north) of the major axis of the 95% confidence level error ellipse |
err_ellipse_r0 | double | arcseconds | major radius of the 95% confidence level position error ellipse |
err_ellipse_r1 | double | arcseconds | minor radius of the 95% confidence level position error ellipse |
extent_flag | Boolean | source is extended, or deconvolved source extent is inconsistent with a point source at the 90% confidence level in one or more observations and science energy bands | |
flux_apec | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum |
flux_apec_aper | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed APEC model [N_{H} = N_{H}(Gal); kT = 6.5 keV] for each science energy band |
flux_apec_aper90 | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed APEC model [N_{H} = N_{H}(Gal); kT = 6.5 keV] for each science energy band |
flux_apec_aper90_hilim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed APEC model [N_{H} = N_{H}(Gal); kT = 6.5 keV] (68% upper confidence limit) |
flux_apec_aper90_lolim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed APEC model [N_{H} = N_{H}(Gal); kT = 6.5 keV] (68% lower confidence limit) |
flux_apec_aper_hilim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed APEC model [N_{H} = N_{H}(Gal); kT = 6.5 keV] (68% upper confidence limit) for each science energy band |
flux_apec_aper_lolim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed APEC model [N_{H} = N_{H}(Gal); kT = 6.5 keV] (68% lower confidence limit) for each science energy band |
flux_apec_hilim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
flux_apec_lolim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
flux_aper | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the source region aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events for each science energy band |
flux_aper90 | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events for each science energy band |
flux_aper90_avg | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events for each science energy band |
flux_aper90_avg_hilim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
flux_aper90_avg_lolim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
flux_aper90_hilim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
flux_aper90_lolim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
flux_aper_avg | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the source region aperture, averaged over all contributing observations, and calculated by counting X-ray events for each science energy band |
flux_aper_avg_hilim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the source region aperture, averaged over all contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
flux_aper_avg_lolim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the source region aperture, averaged over all contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
flux_aper_hilim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the source region aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
flux_aper_lolim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy flux inferred from the source region aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
flux_bb | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum |
flux_bb_aper | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed black body model [N_{H} = N_{H}(Gal); kT = 0.75 keV] for each science energy band |
flux_bb_aper90 | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed black body model [N_{H} = N_{H}(Gal); kT = 0.75 keV] for each science energy band |
flux_bb_aper90_hilim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed black body model [N_{H} = N_{H}(Gal); kT = 0.75 keV] (68% upper confidence limit) for each science energy band |
flux_bb_aper90_lolim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed black body model [N_{H} = N_{H}(Gal); kT = 0.75 keV] (68% lower confidence limit) for each science energy band |
flux_bb_aper_hilim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed black body model [N_{H} = N_{H}(Gal); kT = 0.75 keV] (68% upper confidence limit) for each science energy band |
flux_bb_aper_lolim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed black body model [N_{H} = N_{H}(Gal); kT = 0.75 keV] (68% lower confidence limit) for each science energy band |
flux_bb_hilim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
flux_bb_lolim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
flux_brems | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum |
flux_brems_aper | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed bremsstrahlung model [N_{H} = N_{H}(Gal); kT = 3.5 keV] for each science energy band |
flux_brems_aper90 | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed bremsstrahlung model [N_{H} = N_{H}(Gal); kT = 3.5 keV] for each science energy band |
flux_brems_aper90_hilim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed bremsstrahlung model [N_{H} = N_{H}(Gal); kT = 3.5 keV] (68% upper confidence limit) for each science energy band |
flux_brems_aper90_lolim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed bremsstrahlung model [N_{H} = N_{H}(Gal); kT = 3.5 keV] (68% lower confidence limit) for each science energy band |
flux_brems_aper_hilim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed bremsstrahlung model [N_{H} = N_{H}(Gal); kT = 3.5 keV] (68% upper confidence limit) for each science energy band |
flux_brems_aper_lolim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed bremsstrahlung model [N_{H} = N_{H}(Gal); kT = 3.5 keV] (68% lower confidence limit) for each science energy band |
flux_brems_hilim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
flux_brems_lolim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
flux_powlaw | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum |
flux_powlaw_aper | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed power law model [N_{H} = N_{H}(Gal); γ = 2.0] for each science energy band |
flux_powlaw_aper90 | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed power law model [N_{H} = N_{H}(Gal); γ = 2.0] for each science energy band |
flux_powlaw_aper90_hilim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed power law model [N_{H} = N_{H}(Gal); γ = 2.0] (68% upper confidence limit) for each science energy band |
flux_powlaw_aper90_lolim | double[6] | ergs s^{-1} cm^{-2} | PSF 90% ECF aperture model energy flux inferred from the canonical absorbed power law model [N_{H} = N_{H}(Gal); γ = 2.0] (68% lower confidence limit) for each science energy band |
flux_powlaw_aper_hilim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed power law model [N_{H} = N_{H}(Gal); γ = 2.0] (68% upper confidence limit) for each science energy band |
flux_powlaw_aper_lolim | double[6] | ergs s^{-1} cm^{-2} | source region aperture model energy flux inferred from the canonical absorbed power law model [N_{H} = N_{H}(Gal); γ = 2.0] (68% lower confidence limit) for each science energy band |
flux_powlaw_hilim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
flux_powlaw_lolim | double | ergs s^{-1} cm^{-2} | net integrated 0.5-7.0 keV energy flux of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
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 | ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio | |
hard_hm_hilim | double | ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio (68% upper confidence limit) | |
hard_hm_lolim | double | ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio (68% lower confidence limit) | |
hard_hs | double | ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio | |
hard_hs_hilim | double | ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% upper confidence limit) | |
hard_hs_lolim | double | ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% lower confidence limit) | |
hard_ms | double | ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio | |
hard_ms_hilim | double | ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% upper confidence limit) | |
hard_ms_lolim | double | ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% lower confidence limit) | |
hrc_hetg_num | integer | total number of HRC/HETG observations contributing to the Master Sources Table record of the source | |
hrc_hetg_time | double | total livetime for all HRC/HETG observations contributing to the Master Sources Table record of the source | |
hrc_letg_num | integer | total number of HRC/LETG observations contributing to the Master Sources Table record of the source | |
hrc_letg_time | double | total livetime for all HRC/LETG observations contributing to the Master Sources Table record of the source | |
hrc_num | integer | total number of HRC imaging observations contributing to the Master Sources Table record of the source | |
hrc_time | double | total livetime for all HRC imaging observations contributing to the Master Sources Table record of the source | |
kp_intra_prob | double[6] | intra-observation Kuiper's test variability probability (highest value across all observations); ACIS for each science energy band | |
ks_intra_prob | double[6] | intra-observation Kolmogorov-Smirnov test variability probability (highest value across all observations) for each science energy band | |
likelihood | double | highest detection log-likelihood 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 | 1σ radius along the major axis of the ellipse defining the deconvolved source extent (68% upper confidence limit) for each science energy band |
major_axis_lolim | double[6] | arcseconds | 1σ radius along the major axis of the ellipse defining the deconvolved source extent (68% lower confidence limit) for each science energy band |
man_add_flag | Boolean | source was manually added in the catalog via human review | |
man_inc_flag | Boolean | source was manually included in the catalog via human review (detection was rejected by automated criteria) | |
man_match_flag | Boolean | source detections were manually matched between overlapping stacked observations via human review | |
man_pos_flag | Boolean | best fit source position was manually modified via human review | |
man_reg_flag | Boolean | source region parameters (dimensions, initial guess position input to the Maximum Likelihood Estimator fit) were manually modified via human review | |
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 | 1σ radius along the minor axis of the ellipse defining the deconvolved source extent (68% upper confidence limit) for each science energy band |
minor_axis_lolim | double[6] | arcseconds | 1σ radius along the minor axis of the ellipse defining the deconvolved source extent (68% lower confidence limit) 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 N_{H} column density in direction of source |
phot_nsrcs | long | number of sources simultaneously fit to compute aperture photometry quantitites | |
photflux_aper | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the source region aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events for each science energy band |
photflux_aper90 | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events for each science energy band |
photflux_aper90_avg | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the PSF 90% ECF aperture, averaged over all contributing observations, and calculated by counting X-ray events for each science energy band |
photflux_aper90_avg_hilim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the PSF 90% ECF aperture, averaged over all contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
photflux_aper90_avg_lolim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the PSF 90% ECF aperture, averaged over all contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
photflux_aper90_hilim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
photflux_aper90_lolim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the PSF 90% ECF aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
photflux_aper_avg | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the source region aperture, averaged over all contributing observations, and calculated by counting X-ray events for each science energy band |
photflux_aper_avg_hilim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the source region aperture, averaged over all contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
photflux_aper_avg_lolim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the source region aperture, averaged over all contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
photflux_aper_hilim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the source region aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% upper confidence limit) for each science energy band |
photflux_aper_lolim | double[6] | photons s^{-1} cm^{-2} | aperture-corrected net photon flux inferred from the source region aperture, best estimate derived from the longest block of a multi-band, flux-ordered Bayesian Block analysis of the contributing observations, and calculated by counting X-ray events (68% lower confidence limit) for each science energy band |
pileup_flag | Boolean | ACIS pile-up fraction exceeds ~10% in all observations; source properties may be affected | |
pos_angle | double[6] | deg | position angle (referenced from local true north) of the major axis of the ellipse defining the deconvolved source extent for each science energy band |
pos_angle_hilim | double[6] | deg | position angle (referenced from local true north) of the major axis of the ellipse defining the deconvolved source extent (68% upper confidence limit) for each science energy band |
pos_angle_lolim | double[6] | deg | position angle (referenced from local true north) of the major axis of the ellipse defining the deconvolved source extent (68% lower confidence limit) for each science energy band |
powlaw_ampl | double | amplitude of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum | |
powlaw_ampl_hilim | double | amplitude of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% upper confidence limit) | |
powlaw_ampl_lolim | double | amplitude of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | |
powlaw_ampl_rhat | double | amplitude convergence criterion of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum | |
powlaw_gamma | double | photon index, defined as F_{E} ∝ E^{-γ}, of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum | |
powlaw_gamma_hilim | double | photon index, defined as F_{E} ∝ E^{-γ}, of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% upper confidence limit) | |
powlaw_gamma_lolim | double | photon index, defined as F_{E} ∝ E^{-γ}, of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | |
powlaw_gamma_rhat | double | photon index convergence criterion of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum | |
powlaw_nh | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum |
powlaw_nh_hilim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% upper confidence limit) |
powlaw_nh_lolim | double | N _{HI atoms} 10^{20} cm^{-2} | N_{H} column density of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum (68% lower confidence limit) |
powlaw_nh_rhat | double | N_{H} column density convergence criterion of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum | |
powlaw_stat | double | χ^{2} statistic per degree of freedom of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum | |
ra | double | deg | source position, ICRS right ascension |
sat_src_flag | Boolean | source is saturated in all observations; source properties are unreliable | |
significance | double | highest flux significance 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 | source is located on an ACIS readout streak in all observations; source properties may be affected | |
var_flag | Boolean | source displays flux variability within one or more observations, or between observations, in one or more energy bands | |
var_inter_hard_flag | Boolean | source hardness ratios are statistically inconsistent between two or more observations | |
var_inter_hard_prob_hm | double | inter-observation ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio variability probability | |
var_inter_hard_prob_hs | double | inter-observation ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability probability | |
var_inter_hard_prob_ms | double | inter-observation ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability probability | |
var_inter_index | integer[6] | inter-observation variability index in the range [0, 10]: indicates whether the source region photon flux is constant between observations for each science energy band | |
var_inter_prob | double[6] | inter-observation variability probability, calculated from the chi^2 distribution of the photon fluxes of the individual observations for each science energy band | |
var_inter_sigma | double[6] | photons s^{-1} cm^{-2} | inter-observation flux variability standard deviation; the spread of the individual observation photon fluxes about the error weighted mean for each science energy band |
var_inter_sigma_prob_hm | double | inter-observation ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio variability standard deviation | |
var_inter_sigma_prob_hs | double | inter-observation ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability standard deviation | |
var_inter_sigma_prob_ms | double | inter-observation ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability standard deviation | |
var_intra_index | integer[6] | intra-observation Gregory-Loredo variability index in the range [0, 10]: indicates whether the source region photon flux is constant within an observation (highest value across all observations) for each science energy band | |
var_intra_prob | double[6] | intra-observation Gregory-Loredo variability probability (highest value across all observations) for each science energy band |