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-stack detection" entries, one for each stack in which the source has been detected and by one or more "per-observation detection" entries, one for each observation contribution to the stack in which the source has been detected. Many of the master source properties are populated from the properties of the Best Block (the one with the largest total exposure) from the Bayesian Block Analysis (e.g., aperture photometry).
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.
Context | Column Name | Type | Units | Description |
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Source Name | name | string | source name in the form "2CXO Jhhmmss.s{+|-}ddmmss" | |
Position and Position Errors | ra | double | deg | source position, ICRS right ascension |
dec | double | deg | source position, ICRS declination | |
gal_l | double | deg | source position, galactic longitude (equinox J2000.0, epoch J2000.0) | |
gal_b | double | deg | source position, Galactic latitude (equinox J2000.0, epoch J2000.0) | |
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 | |
err_ellipse_ang | double | deg | position angle (referenced from local true north) of the major axis of the 95% confidence level error ellipse | |
Source Significance | significance | double | highest flux significance across all stacked observations and science energy bands | |
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 | ||
Source Flags | conf_flag | Boolean | source may be confused (source and/or background regions overlap in one or more contributing stacked observations) | |
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 | ||
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 | ||
pileup_flag | Boolean | ACIS pile-up fraction exceeds ~10% in all observations; source properties may be affected | ||
sat_src_flag | Boolean | source is saturated in all observations; source properties are unreliable | ||
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 | ||
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 | ||
Source Extent and Errors | For column names listed in this section, sources have at least one or as many as six filled (non-null) entries in the Master Source Catalog, corresponding to the six CSC energy bands (five ACIS bands, one HRC band). |
ACIS science energy bands (keV): b (0.5-7.0), u (0.2-0.5), s (0.5-1.2), m (1.2-2.0), h (2.0-7.0) HRC source detection and science energy band (keV): w (~0.1-10.0) |
||
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_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 | |
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 | |
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_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 | |
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 | |
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_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 | |
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 | |
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 | |
Aperture Photometry | For column names listed in this section, sources have at least one or as many as six filled (non-null) entries in the Master Source Catalog, corresponding to the six CSC energy bands (five ACIS bands, one HRC band). |
ACIS science energy bands (keV): b (0.5-7.0), u (0.2-0.5), s (0.5-1.2), m (1.2-2.0), h (2.0-7.0) HRC source detection and science energy band (keV): w (~0.1-10.0) |
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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_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 | |
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_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_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_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 | |
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_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_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_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_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_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 | |
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_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_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_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_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_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 | |
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_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_avg | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy 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 | |
flux_aper90_avg_lolim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy 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 | |
flux_aper90_avg_hilim | double[6] | ergs s^{-1} cm^{-2} | aperture-corrected net energy 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 | |
phot_nsrcs | long | number of sources simultaneously fit to compute aperture photometry quantitites | ||
Model Energy Fluxes | 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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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_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) | |
nh_gal | double | N _{HI atoms} 10^{20} cm^{-2} | Galactic N_{H} column density in direction of source | |
Hardness Ratios | hard_hm | double | ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio | |
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_hm_hilim | double | ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio (68% upper confidence limit) | ||
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_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 | ||
hard_hs | double | ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio | ||
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_hs_hilim | double | ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% upper confidence limit) | ||
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_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 | ||
hard_ms | double | ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio | ||
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) | ||
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) | ||
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_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 | ||
Spectral Properties | 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_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) | |
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) | |
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_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_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_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_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_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_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_ampl | double | amplitude of the best fitting absorbed power-law model spectrum to the source region aperture PI spectrum | ||
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_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_rhat | double | amplitude 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 | ||
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_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_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) | |
bb_kt | double | keV | temperature (kT) of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum | |
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_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_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_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_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_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_ampl | double | amplitude of the best fitting absorbed black body model spectrum to the source region aperture PI spectrum | ||
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_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_rhat | double | amplitude 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 | ||
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_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_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) | |
brems_kt | double | keV | temperature (kT) of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum | |
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_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_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_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_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_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_lolim | double | amplitude of the best fitting absorbed bremsstrahlung model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | ||
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_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 | ||
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_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_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) | |
apec_kt | double | keV | temperature (kT) of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | |
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_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_rhat | double | temperature (kT) convergence criterion of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | ||
apec_abund | double | abundance of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | ||
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_hilim | double | abundance of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upper 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_z | double | redshift of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum | ||
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_hilim | double | redshift of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% upper 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 | ||
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_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_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_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_lolim | double | amplitude of the best fitting absorbed APEC model spectrum to the source region aperture PI spectrum (68% lower confidence limit) | ||
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_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 | ||
Source Variability | 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 | ||
ks_intra_prob | double[6] | intra-observation Kolmogorov-Smirnov test variability probability (highest value across all observations) for each science energy band | ||
kp_intra_prob | double[6] | intra-observation Kuiper's test variability probability (highest value across all observations); ACIS for each science energy band | ||
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 | |
Observation Summary | acis_num | integer | total number of ACIS imaging observations contributing to the Master Sources Table record of the source | |
acis_hetg_num | integer | total number of 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 | ||
hrc_num | integer | total number of HRC imaging observations contributing to the Master Sources Table record of the source | ||
hrc_hetg_num | integer | total number of 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 | ||
acis_time | double | total livetime for all ACIS imaging 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_time | double | total livetime for all ACIS/LETG 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 | ||
hrc_hetg_time | double | total livetime for all HRC/HETG 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 | ||