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CSCSTACK - Chandra Source Catalog Stacked Observation Detections, v2.1.1 |
HEASARC Archive |
Overview
The Chandra Source Catalog's Stacked Observation Detections Table (CSCSTACK) includes 493,236 detections (855,402 total entries consisting of detections plus photometric upper limits) based on 10,034 stacks of X-ray observations. Exploiting the unique resolution and very low background of Chandra data, the limiting sensitivity of the catalog is enhanced significantly by stacking (co-adding) multiple observations of the same field prior to source detection. To minimize the impact of the variation in the Chandra point spread function (PSF) with off-axis angles, source detection is constrained to run on stacks of observations that have telescope pointings that are co-located within 60 arcseconds and that were obtained using the same instrument (ACIS or HRC-I). Formally, the observations are matched using a tree clustering algorithm with complete linkage. This means that the pointing direction of every observation in the stack is co-aligned with the pointing direction of every other observation in the stack within 60 arcseconds.The stacked-observation level allows composite properties to be reported from the co-added observations for detections that would otherwise not be visible or have poor S/N in individual observations, while for higher S/N detections the per-observation properties facilitate analysis of variable sources.
CSCSTACK is related to the Chandra Source Catalog (CSC) catalog, which is the definitive catalog of X-ray sources detected by the Chandra X-ray Observatory. The CSC contains 407,806 unique compact and extended X-ray sources. By combining Chandra's sub-arcsecond on-axis spatial resolution and low instrumental background with consistent data processing, the CSC delivers a wide variety of uniformly calibrated properties and science ready data products for detected sources over four decades of flux.
Each identified distinct X-ray source on the sky is represented in the catalog by one or more "stack detection" entries -- one for each stack in which the source has been detected -- and a single "master source" entry. The individual stack entries record all of the properties about a detection extracted from a single stack, as well as associated file-based data products, which are stack-specific.
If a source is detected in one or more stacked-observations, photometric upper limits that are useful for temporal variability analyses are calculated for any overlapping stacked- and individual-observations in which the source is not detected.
Catalog Bibcode
2024ApJS..274...22EReferences
The Chandra Source Catalog
Evans I.N., Primini F.A., Glotfelty C.S., Anderson C.S., Bonaventura N.R.,
Chen J.C., Davis J.E., Doe S.M., Evans J.D., Fabbiano G., Galle E.C.,
Gibbs D.G., Grier J.D., Hain R.M., Hall D.M., Harbo P.N., He X.,
Houck J.C., Karovska M., Kashyap V.L., Lauer J., McCollough M.L.,
McDowell J.C., Miller J.B., Mitschang A.W., Morgan D.L., Mossman A.E.,
Nichols J.S., Nowak M.A., Plummer D.A., Refsdal B.L., Rots A.H.,
Siemiginowska A., Sundheim B.A., Tibbetts M.S., Van Stone D.W.,
Winkelman S.L., Zografou P.
<Astrophys. J. Suppl. Ser. 189, 37 (2010)>
=2010ApJS..189...37E
Provenance
This database table was ingested by the HEASARC in July 2026 and is based on a download of the online version of the "Stacked Observation Detections" Table v. 2.1.1, at the CXC using the CLI. Refer to https://cxc.harvard.edu/csc/cli/ for details.Parameters
Detect_Stack_ID
The detect stack identifier (designation of observation stack used for source
detection) in the format '{acis|hrc}fJhhmmsss{p|m}ddmmss_nnn' where
Jhhmmss{p|m}ddmmss is the J2000 coordinates in sexagesimal units with hh, mm,
ss providing hours, minutes and seconds for the RA component and p/m gives
the '+/-' along with the dd, mm, ss for the decimal degrees for the
Declination component. The nnn designates the catalog version id and may be
'001' or '002' for the stacks. Stacks that end in '_002' are ones that have
extra observations compared to CSC 2.0, whereas a stack that ends in '_001'
either was in CSC 2.0 and has now new data, or was not in CSC 2.0.
RA_Stack
The ICRS Right Ascension corresponding to the stack tangent plane reference
position.
Dec_Stack
The ICRS Declination corresponding to the stack tangent plane reference
position.
Instrument
The instrument used for the stacked observations, either 'ACIS' or 'HRC'.
Grating
The transmission grating used for the stacked observations: 'NONE', 'HETG',
or 'LETG.
X_Offset
The SKY coordinate system X translation correction required to co-align the
observation stack astrometric frame with the Gaia-CRF3 realization of the
ICRF.
Y_Offset
The SKY coordinate system Y translation correction required to co-align the
observation stack astrometric frame with the Gaia-CRF3 realization of the
ICRF.
Rot_Offset
The SKY coordinate system roll angle correction required to co-align the
observation stack astrometric frame with the Gaia-CRF3 realization of the
ICRF.
Dscale
The SKY coordinate system scale factor correction required to co-align the
observation stack astrometric frame with the Gaia-CRF3 realization of the
ICRF.
Man_Astrom_Flag
A flag that designates that the observation stack astrometric transform was
manually modified via human review.
ASCDSver
The CIAO software version used to create the Level 3 detect stack event data
file.
CalDBver
The calibration database version used to calibrate the Level 3 detect stack
event data file.
Create_Date
The creation date/time of the Level 3 detect stack event data file, UTC.
Region_ID
The detection region identifier (component number).
RA
The Right Ascension of the detected source position in the selected equinox.
The source positions are determined from the maximum likelihood estimator
(MLE) fits to the detections' X-ray event distributions, as described in
detail in the How and Why topic 'Source Position Errors in the Master Sources
Table' at https://cxc.harvard.edu/csc/why/err_ellipse_msc.html.
Dec
The Declination of the detected source position in the selected equinox. The
source positions are determined from the maximum likelihood estimator (MLE)
fits to the detections' X-ray event distributions, as described in detail in
the How and Why topic 'Source Position Errors in the Master Sources Table' at
https://cxc.harvard.edu/csc/why/err_ellipse_msc.html.
LII
The Galactic Longitude (equinox J2000.0, epoch J2000.0) of the X-ray source.
BII
The Galactic Longitude (equinox J2000.0, epoch J2000.0) of the X-ray source.
Error_Ellipse_R0
The radius of the semi-major axis corresponding to the 95% confidence level
position error ellipse. The error ellipse is typically the best-fitting
ellipse to the position-uncertainty-fit-statistic surface computed from the
MLE's Markov chain Monte Carlo draws. If the MCMC draws do not converge, then
an error circle, rather than error ellipse, is used.
Error_Ellipse_R1
The radius of the semi-minor axis corresponding to the 95% confidence level
position error ellipse. The error ellipse is typically the best-fitting
ellipse to the position-uncertainty-fit-statistic surface computed from the
MLE's Markov chain Monte Carlo draws. If the MCMC draws do not converge, then
an error circle, rather than error ellipse, is used.
Error_Ellipse_Angle
Position angle (ref. local true North) of the major axis of the 95%
confidence level error ellipse The position angle, with respect to local true
north, corresponding to the 95% confidence level position error ellipse. The
error ellipse is typically the best-fitting ellipse to the
position-uncertainty-fit-statistic surface computed from the MLE's Markov
chain Monte Carlo draws. If the MCMC draws do not converge, then an error
circle, rather than error ellipse, is used.
Theta_Mean
The mean source region aperture off-axis angle computed by averaging the
off-axis angles from all observations in a stack.
B_Likelihood
The log likelihood of the stacked-observation detection computed by the Maximum Likelihood Estimator fit to the photon counts distribution in the ACIS broad (0.5-7.0 keV) energy band.
H_Likelihood
The log likelihood of the stacked-observation detection computed by the Maximum Likelihood Estimator fit to the photon counts distribution in the ACIS hard (2.0-7.0 keV) energy band.
M_Likelihood
The log likelihood of the stacked-observation detection computed by the Maximum Likelihood Estimator fit to the photon counts distribution in the ACIS medium (1.2-2.0 keV) energy band.
S_Likelihood
The log likelihood of the stacked-observation detection computed by the Maximum Likelihood Estimator fit to the photon counts distribution in the ACIS soft (0.5-1.2 keV) energy band.
U_Likelihood
The log likelihood of the stacked-observation detection computed by the Maximum Likelihood Estimator fit to the photon counts distribution in the ACIS ultrasoft (0.2-0.5 keV) energy band.
W_Likelihood
The log likelihood of the stacked-observation detection computed by the Maximum Likelihood Estimator fit to the photon counts distribution in the HRC wide (~0.1-10.0 keV) energy band.
Likelihood_Class
The highest detection likelihood classification across all of the energy bands.
B_Detect_Significance
The detection significance of the stacked-observation detection computed by the stacked-observation detection algorithm for the ACIS broad (0.5-7.0 keV) energy band.
H_Detect_Significance
The detection significance of the stacked-observation detection computed by the stacked-observation detection algorithm for the ACIS hard (2.0-7.0 keV) energy band.
M_Detect_Significance
The detection significance of the stacked-observation detection computed by the stacked-observation detection algorithm for the ACIS medium (1.2-2.0 keV) energy band.
S_Detect_Significance
The detection significance of the stacked-observation detection computed by the stacked-observation detection algorithm for the ACIS soft (0.5-1.2 keV) energy band.
U_Detect_Significance
The detection significance of the stacked-observation detection computed by the stacked-observation detection algorithm for the ACIS ultrasoft (0.2-0.5 keV) energy band.
W_Detect_Significance
The detection significance of the stacked-observation detection computed by the stacked-observation detection algorithm for the HRC wide (~0.1-10.0 keV) energy band.
B_Flux_Significance
The flux significance of the stacked-observation detection, determined from the ratio of the stacked-observation detection photon flux to the estimated error in the photon flux, for the ACIS broad (0.5-7.0 keV) energy band.
H_Flux_Significance
The flux significance of the stacked-observation detection, determined from the ratio of the stacked-observation detection photon flux to the estimated error in the photon flux, for the ACIS hard (2.0-7.0 keV) energy band.
M_Flux_Significance
The flux significance of the stacked-observation detection, determined from the ratio of the stacked-observation detection photon flux to the estimated error in the photon flux, for the ACIS medium (1.2-2.0 keV) energy band.
S_Flux_Significance
The flux significance of the stacked-observation detection, determined from the ratio of the stacked-observation detection photon flux to the estimated error in the photon flux, for the ACIS soft (0.5-1.2 keV) energy band.
U_Flux_Significance
The flux significance of the stacked-observation detection, determined from the ratio of the stacked-observation detection photon flux to the estimated error in the photon flux, for the ACIS ultrasoft (0.2-0.5 keV) energy band.
W_Flux_Significance
The flux significance of the stacked-observation detection, determined from the ratio of the stacked-observation detection photon flux to the estimated error in the photon flux, for the HRC wide (~0.1-10.0 keV) energy band.
Extent_Code
The code indicating that the detection is extended, or deconvolved compact
detection extent is inconsistent with a point source at the 90% confidence
level in one or more of the stacked observations and energy bands. The code
bit values are encoded as follows:
1: Deconvolved compact detection extent is not consistent with point
source at the 90% confidence level in the ACIS ultrasoft energy band
2: Deconvolved compact detection extent is not consistent with point
source at the 90% confidence level in the ACIS soft energy band
4: Deconvolved compact detection extent is not consistent with point
source at the 90% confidence level in the ACIS medium energy band
8: Deconvolved compact detection extent is not consistent with point
source at the 90% confidence level in the ACIS hard energy band
16: Deconvolved compact detection extent is not consistent with point
source at the 90% confidence level in the ACIS broad energy band
32: Deconvolved compact detection extent is not consistent with point
source at the 90% confidence level in the HRC wide energy band
256: Extended detection
Conf_Code
The code indicating that the compact detection may be confused. All bits are
set to zero if the detection's source and background region ellipses do not
overlap another source or background region in any source detection energy
band, and the compact detection does not overlay an extended (convex hull)
detection. Otherwise, the code bit values are encoded as follows:
1: Background region overlaps another background region
2: Background region overlaps another source region
4: Source region overlaps another background region
8: Source region overlaps another source region
256: Compact detection is overlaid on an extended detection
The confusion code for an extended (convex hull) detection is always NULL.
Pileup_Flag
The flag for a compact detection if the ACIS pile-up fraction exceeds ~ 10%
in any contributing ACIS per-observation detections and energy bands. The
pileup warning flag is NULL for extended (convex hull) detections.
Var_Flag
The flag indicating flux variability within any single observation or between
any pair of observations contributing to the stacked detection, in any energy
band.
Edge_Code
The code indicating whether the detection position, or source or background
region dithered off a detector boundary (chip pixel mask) during one or more
of the stacked observations. The code bits are set as follows:
1: Background region dithers off detector boundary
2: Source region dithers off detector boundary
4: Detection position dithers off detector boundary
Note that an extended (convex hull) detection (or associated background
region) that extends across more than one chip by definition must dither off
the chip boundary.
Multi_Chip_Code
The code indicating whether the source position, or source or background
region dithered between two or more chips during one or more of the stacked
observations. The code bits are set as follows:
1: Background region dithers across two chips
2: Background region dithers across more than two chips
4: Source region dithers across two chips
8: Source region dithers across more than two chips
16: Detection position dithers across two chips
32: Detection position dithers across more than two chips
Note that an extended (convex hull) detection (or associated background
region) that extends across more than one chip by definition must dither
across the chips.
Streak_Src_Flag
The flag indicating that the compact detection suffers from readout streak
effects, i.e. if all of the contributing observations are ACIS observations
and ALL per-observation source regions overlap a defined region enclosing an
identified readout streak. The flag is TRUE for extended sources if any
contributing observations are ACIS observations and ANY per-observations
detection source region region overlaps a defined region enclosing an
identified readout streak.
Sat_Src_Flag
The flag indicating whether the compact detection suffers from saturation,
i.e. all contributing observations are ACIS observations and all
per-observation detections are significantly piled-up. The detection
properties are unreliable for all ACIS energy bands. This is NULL for
extended sources.
Man_Add_Flag
The flag indicating that the source was manually added in the catalog via
human review. Detections that are manually added must satisfy detection
likelihood and other validity checks in order to appear in the final catalog.
See also the Manual Source/Detection Inclusion Flag as described here:
https://cxc.cfa.harvard.edu/csc/columns/flags.html and in the man_inc_flag
field description.
Man_Inc_Flag
The flag indicating that the detection was manually included in the catalog
via human review. Detections that are manually included are not required to
satisfy detection likelihood or other validity checks. Manually included
detections may or may not be manually added; if they are manually added then
the man_add_flag will also be set to TRUE.
Man_Reg_Flag
The flag indicating that the detections region parameters (i.e., the source
region ellipse semi-axes and/or rotation angle, and/or position that define
the detection region evaluated by the maximum likelihood estimator [MLE])
were manually modified by human review. The manual detection region
parameters flag for an extended source is set to TRUE if the shape or
position of the defining polygon was manually modified by human review.
Man_Pos_Flag
The flag indicating that the final detection position was manually modified
from the fitted position (determined by the maximum likelihood estimator
[MLE]) by human review. The manual detection position flag for an extended
(convex hull) detection is set to TRUE if the final detection position was
manually modified from the flux-weighted centroid position by human review.
Var_Inter_Hard_Flag
The flag indicating variable hardness ratio for a compact detection, provided
that one or more of the hardness ratios computed for any of the contributing
observation detections is statistically inconsistent with the corresponding
hardness ratios computed for any other contributing observations detections.
RA_Ap
The ICRS Right Ascension corresponding to the center of the source region and
background region apertures. The spatial regions defining a source and its
corresponding background are determined by scaling and merging the individual
source detection regions that result from all of the spatial scales and
source detection energy bands in which the source is detected during the
source detection process (wavdetect). The result is a single elliptical
source region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
Dec_Ap
The ICRS Declination corresponding to the center of the source region and
background region apertures. The spatial regions defining a source and its
corresponding background are determined by scaling and merging the individual
source detection regions that result from all of the spatial scales and
source detection energy bands in which the source is detected during the
source detection process (wavdetect). The result is a single elliptical
source region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
Major_Axis_Ap
The semi-major axis defining the elliptical source region aperture. The
spatial regions defining a source and its corresponding background are
determined by scaling and merging the individual source detection regions
that result from all of the spatial scales and source detection energy bands
in which the source is detected during the source detection process
(wavdetect). The result is a single elliptical source region which excludes
any overlapping source regions, and a single, co-located, scaled, elliptical
annular background region.
Minor_Axis_Ap
The semi-minor axis defining the elliptical source region aperture. The
spatial regions defining a source and its corresponding background are
determined by scaling and merging the individual source detection regions
that result from all of the spatial scales and source detection energy bands
in which the source is detected during the source detection process
(wavdetect). The result is a single elliptical source region which excludes
any overlapping source regions, and a single, co-located, scaled, elliptical
annular background region.
Position_Angle_Ap
The position angle of the semi-major axes (with respect to true local North)
defining the elliptical source region aperture. The spatial regions defining
a source and its corresponding background are determined by scaling and
merging the individual source detection regions that result from all of the
spatial scales and source detection energy bands in which the source is
detected during the source detection process (wavdetect). The result is a
single elliptical source region which excludes any overlapping source
regions, and a single, co-located, scaled, elliptical annular background
region.
Major_Axis1_Apbkg
The semi-major axis defining the inner ellipse of the annular background
region aperture. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
Minor_Axis1_Apbkg
The semi-minor axis defining the inner ellipse of the annular background
region aperture. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
Major_Axis2_Apbkg
The semi-major axis defining the outer ellipse of the annular background
region aperture. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
Minor_Axis2_Apbkg
The semi-minor axis defining the outer ellipse of the annular background
region aperture. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
Position_Angle_Apbkg
The position angle of the semi-major axes (with respect to true local North)
of the elliptical background region aperture. The spatial regions defining a
source and its corresponding background are determined by scaling and merging
the individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
B_Major_Axis
The 1-sigma radius along the major axis of the ellipse defining the
deconvolved detection extent for the ACIS broad (0.5-7.0 keV) energy band.
For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
H_Major_Axis
The 1-sigma radius along the major axis of the ellipse defining the
deconvolved detection extent for the ACIS hard (2.0-7.0 keV) energy band. For
stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
M_Major_Axis
The 1-sigma radius along the major axis of the ellipse defining the
deconvolved detection extent for the ACIS medium (1.2-2.0 keV) energy band.
For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
S_Major_Axis
The 1-sigma radius along the major axis of the ellipse defining the
deconvolved detection extent for the ACIS soft (0.5-1.2 keV) energy band. For
stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
U_Major_Axis
The 1-sigma radius along the major axis of the ellipse defining the
deconvolved detection extent for the ACIS ultrasoft (0.2-0.5 keV) energy
band. For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
W_Major_Axis
The 1-sigma radius along the major axis of the ellipse defining the
deconvolved detection extent for the HRC wide (~0.1-10.0 keV) energy band.
For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
B_Major_Axis_Lo
The 68% lower confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS broad (0.5-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
H_Major_Axis_Lo
The 68% lower confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS hard (2.0-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
M_Major_Axis_Lo
The 68% lower confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS medium (1.2-2.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
S_Major_Axis_Lo
The 68% lower confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS soft (0.5-1.2
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
U_Major_Axis_Lo
The 68% lower confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS ultrasoft
(0.2-0.5 keV) energy band. For stacked observation detections, the
deconvolved source extent is a parameterization of the best estimate of the
flux distribution defining the PSF-deconvolved source, which is determined in
each science energy band from a variance-weighted mean of the deconvolved
extent of each source measured in all contributing observations. The
parameterization represents the associated uncertainty.
W_Major_Axis_Lo
The 68% lower confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the HRC wide (~0.1-10.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
B_Major_Axis_Hi
The 68% upper confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS broad (0.5-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
H_Major_Axis_Hi
The 68% upper confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS hard (2.0-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
M_Major_Axis_Hi
The 68% upper confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS medium (1.2-2.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
S_Major_Axis_Hi
The 68% upper confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS soft (0.5-1.2
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
U_Major_Axis_Hi
The 68% upper confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the ACIS ultrasoft
(0.2-0.5 keV) energy band. For stacked observation detections, the
deconvolved source extent is a parameterization of the best estimate of the
flux distribution defining the PSF-deconvolved source, which is determined in
each science energy band from a variance-weighted mean of the deconvolved
extent of each source measured in all contributing observations. The
parameterization represents the associated uncertainty.
W_Major_Axis_Hi
The 68% upper confidence limit for the radius along the major axis of the
ellipse defining the deconvolved detection extent in the HRC wide (~0.1-10.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
B_Minor_Axis
The 1-sigma radius along the minor axis of the ellipse defining the
deconvolved detection extent for the ACIS broad (0.5-7.0 keV) energy band.
For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
H_Minor_Axis
The 1-sigma radius along the minor axis of the ellipse defining the
deconvolved detection extent for the ACIS hard (2.0-7.0 keV) energy band. For
stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
M_Minor_Axis
The 1-sigma radius along the minor axis of the ellipse defining the
deconvolved detection extent for the ACIS medium (1.2-2.0 keV) energy band.
For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
S_Minor_Axis
The 1-sigma radius along the minor axis of the ellipse defining the
deconvolved detection extent for the ACIS soft (0.5-1.2 keV) energy band. For
stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
U_Minor_Axis
The 1-sigma radius along the minor axis of the ellipse defining the
deconvolved detection extent for the ACIS ultrasoft (0.2-0.5 keV) energy
band. For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
W_Minor_Axis
The 1-sigma radius along the minor axis of the ellipse defining the
deconvolved detection extent for the HRC wide (~0.1-10.0 keV) energy band.
For stacked observation detections, the deconvolved source extent is a
parameterization of the best estimate of the flux distribution defining the
PSF-deconvolved source, which is determined in each science energy band from
a variance-weighted mean of the deconvolved extent of each source measured in
all contributing observations. The parameterization represents the best
estimate values.
B_Minor_Axis_Lo
The 68% lower confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS broad (0.5-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
H_Minor_Axis_Lo
The 68% lower confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS hard (2.0-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
M_Minor_Axis_Lo
The 68% lower confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS medium (1.2-2.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
S_Minor_Axis_Lo
The 68% lower confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS soft (0.5-1.2
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
U_Minor_Axis_Lo
The 68% lower confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS ultrasoft
(0.2-0.5 keV) energy band. For stacked observation detections, the
deconvolved source extent is a parameterization of the best estimate of the
flux distribution defining the PSF-deconvolved source, which is determined in
each science energy band from a variance-weighted mean of the deconvolved
extent of each source measured in all contributing observations. The
parameterization represents the associated uncertainty.
W_Minor_Axis_Lo
The 68% lower confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the HRC wide (~0.1-10.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
B_Minor_Axis_Hi
The 68% upper confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS broad (0.5-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
H_Minor_Axis_Hi
The 68% upper confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS hard (2.0-7.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
M_Minor_Axis_Hi
The 68% upper confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS medium (1.2-2.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
S_Minor_Axis_Hi
The 68% upper confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS soft (0.5-1.2
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
U_Minor_Axis_Hi
The 68% upper confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the ACIS ultrasoft
(0.2-0.5 keV) energy band. For stacked observation detections, the
deconvolved source extent is a parameterization of the best estimate of the
flux distribution defining the PSF-deconvolved source, which is determined in
each science energy band from a variance-weighted mean of the deconvolved
extent of each source measured in all contributing observations. The
parameterization represents the associated uncertainty.
W_Minor_Axis_Hi
The 68% upper confidence limit for the radius along the minor axis of the
ellipse defining the deconvolved detection extent in the HRC wide (~0.1-10.0
keV) energy band. For stacked observation detections, the deconvolved source
extent is a parameterization of the best estimate of the flux distribution
defining the PSF-deconvolved source, which is determined in each science
energy band from a variance-weighted mean of the deconvolved extent of each
source measured in all contributing observations. The parameterization
represents the associated uncertainty.
B_Position_Angle
The position angle of the major axes (with respect to true local North)
defining the deconvolved detection extent in the ACIS broad (0.5-7.0 keV)
energy band. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
H_Position_Angle
The position angle of the major axes (with respect to true local North)
defining the deconvolved detection extent in the ACIS hard (2.0-7.0 keV)
energy band. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
M_Position_Angle
The position angle of the major axes (with respect to true local North)
defining the deconvolved detection extent in the ACIS medium (1.2-2.0 keV)
energy band. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
S_Position_Angle
The position angle of the major axes (with respect to true local North)
defining the deconvolved detection extent in the ACIS soft (0.5-1.2 keV)
energy band. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
U_Position_Angle
The position angle of the major axes (with respect to true local North)
defining the deconvolved detection extent in the ACIS ultrasoft (0.2-0.5 keV)
energy band. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
W_Position_Angle
The position angle of the major axes (with respect to true local North)
defining the deconvolved detection extent in the HRC wide (~0.1-10.0 keV)
energy band. The spatial regions defining a source and its corresponding
background are determined by scaling and merging the individual source
detection regions that result from all of the spatial scales and source
detection energy bands in which the source is detected during the source
detection process (wavdetect). The result is a single elliptical source
region which excludes any overlapping source regions, and a single,
co-located, scaled, elliptical annular background region.
B_Position_Angle_Lo
The 68% lower confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS broad (0.5-7.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
H_Position_Angle_Lo
The 68% lower confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS hard (2.0-7.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
M_Position_Angle_Lo
The 68% lower confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS medium (1.2-2.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
S_Position_Angle_Lo
The 68% lower confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS soft (0.5-1.2 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
U_Position_Angle_Lo
The 68% lower confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS ultrasoft (0.2-0.5 keV) energy band. The spatial regions defining a
source and its corresponding background are determined by scaling and merging
the individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
W_Position_Angle_Lo
The 68% lower confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
HRC wide (~0.1-10.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
B_Position_Angle_Hi
The 68% upper confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS broad (0.5-7.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
H_Position_Angle_Hi
The 68% upper confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS hard (2.0-7.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
M_Position_Angle_Hi
The 68% upper confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS medium (1.2-2.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
S_Position_Angle_Hi
The 68% upper confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS soft (0.5-1.2 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
U_Position_Angle_Hi
The 68% upper confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
ACIS ultrasoft (0.2-0.5 keV) energy band. The spatial regions defining a
source and its corresponding background are determined by scaling and merging
the individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
W_Position_Angle_Hi
The 68% upper confidence limit for the position angle of the major axes (with
respect to true local North) defining the deconvolved detection extent in the
HRC wide (~0.1-10.0 keV) energy band. The spatial regions defining a source
and its corresponding background are determined by scaling and merging the
individual source detection regions that result from all of the spatial
scales and source detection energy bands in which the source is detected
during the source detection process (wavdetect). The result is a single
elliptical source region which excludes any overlapping source regions, and a
single, co-located, scaled, elliptical annular background region.
B_Src_Area
The area in square arcseconds of the deconvolved detection extent ellipse, or
area of the detection polygon for extended detection, in the ACIS broad
(0.5-7.0 keV) energy band.
H_Src_Area
The area in square arcseconds of the deconvolved detection extent ellipse, or
area of the detection polygon for extended detection, in the ACIS hard
(2.0-7.0 keV) energy band.
M_Src_Area
The area in square arcseconds of the deconvolved detection extent ellipse, or
area of the detection polygon for extended detection, in the ACIS medium
(1.2-2.0 keV) energy band.
S_Src_Area
The area in square arcseconds of the deconvolved detection extent ellipse, or
area of the detection polygon for extended detection, in the ACIS soft
(0.5-1.2 keV) energy band.
U_Src_Area
The area in square arcseconds of the deconvolved detection extent ellipse, or
area of the detection polygon for extended detection, in the ACIS ultrasoft
(0.2-0.5 keV) energy band.
W_Src_Area
The area in square arcseconds of the deconvolved detection extent ellipse, or
area of the detection polygon for extended detection, in the HRC wide
(~0.1-10.0 keV) energy band.
Phot_Nsrcs
The number of detections fit simultaneously to compute the aperture
photometry quantities.
B_Counts_Ap
The aperture-corrected source net counts inferred from the source region
aperture in the ACIS broad (0.5-7.0 keV) energy band. These counts represent
the combined net number of background-subtracted source counts in the
modified source region, corrected by the appropriate PSF aperture fractions,
for all valid source observations in the stack.
H_Counts_Ap
The aperture-corrected source net counts inferred from the source region
aperture in the ACIS hard (2.0-7.0 keV) energy band. These counts represent
the combined net number of background-subtracted source counts in the
modified source region, corrected by the appropriate PSF aperture fractions,
for all valid source observations in the stack.
M_Counts_Ap
The aperture-corrected source net counts inferred from the source region
aperture in the ACIS medium (1.2-2.0 keV) energy band. These counts represent
the combined net number of background-subtracted source counts in the
modified source region, corrected by the appropriate PSF aperture fractions,
for all valid source observations in the stack.
S_Counts_Ap
The aperture-corrected source net counts inferred from the source region
aperture in the ACIS soft (0.5-1.2 keV) energy band. These counts represent
the combined net number of background-subtracted source counts in the
modified source region, corrected by the appropriate PSF aperture fractions,
for all valid source observations in the stack.
U_Counts_Ap
The aperture-corrected source net counts inferred from the source region
aperture in the ACIS ultrasoft (0.2-0.5 keV) energy band. These counts
represent the combined net number of background-subtracted source counts in
the modified source region, corrected by the appropriate PSF aperture
fractions, for all valid source observations in the stack.
W_Counts_Ap
The aperture-corrected source net counts inferred from the source region
aperture in the HRC wide (~0.1-10.0 keV) energy band. These counts represent
the combined net number of background-subtracted source counts in the
modified source region, corrected by the appropriate PSF aperture fractions,
for all valid source observations in the stack.
B_Counts_Ap_Lo
The 68% lower confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS broad (0.5-7.0) energy
band. These counts represent the uncertainty in the combined net number of
background-subtracted source counts in the modified source region, corrected
by the appropriate PSF aperture fractions, for all valid source observations
in the stack.
H_Counts_Ap_Lo
The 68% lower confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS hard (2.0-7.0 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
M_Counts_Ap_Lo
The 68% lower confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS medium (1.2-2.0 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
S_Counts_Ap_Lo
The 68% lower confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS soft (0.5-1.2 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
U_Counts_Ap_Lo
The 68% lower confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS ultrasoft (0.2-0.5 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
W_Counts_Ap_Lo
The 68% lower confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the HRC wide (~0.1-10.0 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
B_Counts_Ap_Hi
The 68% upper confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS broad (0.5-7.0) energy
band. These counts represent the uncertainty in the combined net number of
background-subtracted source counts in the modified source region, corrected
by the appropriate PSF aperture fractions, for all valid source observations
in the stack.
H_Counts_Ap_Hi
The 68% upper confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS hard (2.0-7.0 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
M_Counts_Ap_Hi
The 68% upper confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS medium (1.2-2.0 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
S_Counts_Ap_Hi
The 68% upper confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS soft (0.5-1.2 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
U_Counts_Ap_Hi
The 68% upper confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the ACIS ultrasoft (0.2-0.5 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
W_Counts_Ap_Hi
The 68% upper confidence limit for the aperture-corrected source net counts
inferred from the source region aperture in the HRC wide (~0.1-10.0 keV)
energy band. These counts represent the uncertainty in the combined net
number of background-subtracted source counts in the modified source region,
corrected by the appropriate PSF aperture fractions, for all valid source
observations in the stack.
B_Counts_Ap90
The aperture-corrected net source counts inferred from the PSF 90% ECF
aperture in the ACIS broad (0.5-7.0 keV) energy band. These counts are based
on the average background-subtracted source count rates in the modified
elliptical aperture, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
H_Counts_Ap90
The aperture-corrected net source counts inferred from the PSF 90% ECF
aperture in the ACIS hard (2.0-7.0 keV) energy band. These counts are based
on the average background-subtracted source count rates in the modified
elliptical aperture, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
M_Counts_Ap90
The aperture-corrected net source counts inferred from the PSF 90% ECF
aperture in the ACIS medium (1.2-2.0 keV) energy band. These counts are based
on the average background-subtracted source count rates in the modified
elliptical aperture, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
S_Counts_Ap90
The aperture-corrected net source counts inferred from the PSF 90% ECF
aperture in the ACIS soft (0.5-1.2 keV) energy band. These counts are based
on the average background-subtracted source count rates in the modified
elliptical aperture, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
U_Counts_Ap90
The aperture-corrected net source counts inferred from the PSF 90% ECF
aperture in the ACIS ultrasoft (0.2-0.5 keV) energy band. These counts are
based on the average background-subtracted source count rates in the modified
elliptical aperture, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
W_Counts_Ap90
The aperture-corrected net source counts inferred from the PSF 90% ECF
aperture in the HRC wide (~0.1-10.0 keV) energy band. These counts are based
on the average background-subtracted source count rates in the modified
elliptical aperture, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
B_Counts_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS broad (0.5-7.0) energy
band.
H_Counts_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS hard (2.0-7.0 keV) energy
band.
M_Counts_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS medium (1.2-2.0 keV)
energy band.
S_Counts_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS soft (0.5-1.2 keV) energy
band.
U_Counts_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS ultrasoft (0.2-0.5 keV)
energy band.
W_Counts_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the HRC wide (~0.1-10.0 keV) energy
band. #the stack.
B_Counts_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS broad (0.5-7.0) energy
band.
H_Counts_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS hard (2.0-7.0 keV) energy
band.
M_Counts_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS medium (1.2-2.0 keV)
energy band.
S_Counts_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS soft (0.5-1.2 keV) energy
band.
U_Counts_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the ACIS ultrasoft (0.2-0.5 keV)
energy band.
W_Counts_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source counts
inferred from the PSF 90% ECF aperture in the HRC wide (~0.1-10.0 keV) energy
band.
B_Count_Rate_Ap
The aperture-corrected detection net count rate inferred from the source
region aperture in the ACIS broad (0.5-7.0 keV) energy band. These are
defined as the average background-subtracted source count rates in the
modified source region, corrected by the appropriate PSF aperture fractions
and livetime, for all valid source observations in the stack.
H_Count_Rate_Ap
The aperture-corrected detection net count rate inferred from the source
region aperture in the ACIS hard (2.0-7.0 keV)energy band. These are defined
as the average background-subtracted source count rates in the modified
source region, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
M_Count_Rate_Ap
The aperture-corrected detection net count rate inferred from the source
region aperture in the ACIS medium (1.2-2.0 keV) energy band. These are
defined as the average background-subtracted source count rates in the
modified source region, corrected by the appropriate PSF aperture fractions
and livetime, for all valid source observations in the stack.
S_Count_Rate_Ap
The aperture-corrected detection net count rate inferred from the source
region aperture in the ACIS soft (0.5-1.2 keV) energy band. These are defined
as the average background-subtracted source count rates in the modified
source region, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
U_Count_Rate_Ap
The aperture-corrected detection net count rate inferred from the source
region aperture in the ACIS ultrasoft (0.2-0.5 keV) energy band. These are
defined as the average background-subtracted source count rates in the
modified source region, corrected by the appropriate PSF aperture fractions
and livetime, for all valid source observations in the stack.
W_Count_Rate_Ap
The aperture-corrected detection net count rate inferred from the source
region aperture in the HRC wide (~0.1-10.0 keV) energy band. These are
defined as the average background-subtracted source count rates in the
modified source region, corrected by the appropriate PSF aperture fractions
and livetime, for all valid source observations in the stack.
B_Count_Rate_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS broad (0.5-7.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
H_Count_Rate_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS hard (2.0-7.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
M_Count_Rate_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS medium (1.2-2.0
keV) energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
S_Count_Rate_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS soft (0.5-1.2
keV)energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
U_Count_Rate_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS ultrasoft (0.2-0.5
keV) energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
W_Count_Rate_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the HRC wide (~0.1-10.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
B_Count_Rate_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS broad (0.5-7.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
H_Count_Rate_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS hard (2.0-7.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
M_Count_Rate_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS medium (1.2-2.0
keV) energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
S_Count_Rate_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS soft (0.5-1.2 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
U_Count_Rate_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the ACIS ultrasoft (0.2-0.5
keV) energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
W_Count_Rate_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net count
rate inferred from the source region aperture in the HRC wide (~0.1-10.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
B_Count_Rate_Ap90
The aperture-corrected net source count rate inferred from the PSF 90% ECF
aperture in the ACIS broad (0.5-7.0) energy band. These are defined as the
average background-subtracted source count rates in the modified source
region, corrected by the appropriate PSF aperture fractions and livetime, for
all valid source observations in the stack.
H_Count_Rate_Ap90
The aperture-corrected net source count rate inferred from the PSF 90% ECF
aperture in the ACIS hard (2.0-7.0 keV) energy band. These are defined as the
average background-subtracted source count rates in the modified source
region, corrected by the appropriate PSF aperture fractions and livetime, for
all valid source observations in the stack.
M_Count_Rate_Ap90
The aperture-corrected net source count rate inferred from the PSF 90% ECF
aperture in the ACIS medium (1.2-2.0 keV) energy band. These are defined as
the average background-subtracted source count rates in the modified source
region, corrected by the appropriate PSF aperture fractions and livetime, for
all valid source observations in the stack.
S_Count_Rate_Ap90
The aperture-corrected net source count rate inferred from the PSF 90% ECF
aperture in the ACIS soft (0.5-1.2 keV) energy band. These are defined as the
average background-subtracted source count rates in the modified source
region, corrected by the appropriate PSF aperture fractions and livetime, for
all valid source observations in the stack.
U_Count_Rate_Ap90
The aperture-corrected net source count rate inferred from the PSF 90% ECF
aperture in the ACIS ultrasoft (0.2-0.5 keV) energy band. These are defined
as the average background-subtracted source count rates in the modified
source region, corrected by the appropriate PSF aperture fractions and
livetime, for all valid source observations in the stack.
W_Count_Rate_Ap90
The aperture-corrected net source count rate inferred from the PSF 90% ECF
aperture in the HRC wide (~0.1-10.0 keV) energy band. These are defined as
the average background-subtracted source count rates in the modified source
region, corrected by the appropriate PSF aperture fractions and livetime, for
all valid source observations in the stack.
B_Count_Rate_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS broad (0.5-7.0)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
H_Count_Rate_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS hard (2.0-7.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
M_Count_Rate_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS medium (1.2-2.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
S_Count_Rate_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS soft (0.5-1.2 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
U_Count_Rate_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS ultrasoft (0.2-0.5
keV) energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
W_Count_Rate_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the HRC wide (~0.1-10.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
B_Count_Rate_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS broad (0.5-7.0)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
H_Count_Rate_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS hard (2.0-7.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
M_Count_Rate_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS medium (1.2-2.0 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
S_Count_Rate_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS soft (0.5-1.2 keV)
energy band. These are defined as the average background-subtracted source
count rates in the modified source region, corrected by the appropriate PSF
aperture fractions and livetime, for all valid source observations in the
stack.
U_Count_Rate_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the ACIS ultrasoft (0.2-0.5
keV) energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
W_Count_Rate_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected net source count
rate inferred from the PSF 90% ECF aperture in the HRC wide (~0.1-10.0
keV)energy band. These are defined as the average background-subtracted
source count rates in the modified source region, corrected by the
appropriate PSF aperture fractions and livetime, for all valid source
observations in the stack.
B_Photflux_Ap
The aperture-corrected detection net photon flux inferred from the source
region aperture, calculated by counting X-ray events, in the ACIS broad
(0.5-7.0 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
H_Photflux_Ap
The aperture-corrected detection net photon flux inferred from the source
region aperture, calculated by counting X-ray events, in the ACIS hard
(2.0-7.0 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
M_Photflux_Ap
The aperture-corrected detection net photon flux inferred from the source
region aperture, calculated by counting X-ray events, in the ACIS medium
(1.2-2.0 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
S_Photflux_Ap
The aperture-corrected detection net photon flux inferred from the source
region aperture, calculated by counting X-ray events, in the ACIS soft
(0.5-1.2 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
U_Photflux_Ap
The aperture-corrected detection net photon flux inferred from the source
region aperture, calculated by counting X-ray events, in the ACIS ultrasoft
(0.2-0.5 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
W_Photflux_Ap
The aperture-corrected detection net photon flux inferred from the source
region aperture, calculated by counting X-ray events, in the HRC wide
(~0.1-10.0 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
B_Photflux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS broad (0.5-7.0) energy band.
H_Photflux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS hard (2.0-7.0 keV) energy band.
M_Photflux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS medium (1.2-2.0 keV) energy band.
S_Photflux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS soft (0.5-1.2 keV) energy band.
U_Photflux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS ultrasoft (0.2-0.5 keV)energy band.
W_Photflux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the HRC wide (~0.1-10.0 keV) energy band.
B_Photflux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS broad (0.5-7.0) energy band.
H_Photflux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS hard (2.0-7.0 keV) energy band.
M_Photflux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS medium (1.2-2.0 keV) energy band.
S_Photflux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS soft (0.5-1.2 keV)energy band.
U_Photflux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the ACIS ultrasoft (0.2-0.5 keV) energy band.
W_Photflux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the source region aperture, calculated by counting
X-ray events, in the HRC wide (~0.1-10.0 keV) energy band.
B_Photflux_Ap90
The aperture-corrected detection net photon flux inferred from the PSF 90%
ECF aperture, calculated by counting X-ray events, in the ACIS broad (0.5-7.0
keV) energy band. These fluxes represent the average background-subtracted
fluxes in the modified source region, corrected by the appropriate PSF
aperture fractions, livetime, and exposure for all valid observations in the
stack.
H_Photflux_Ap90
The aperture-corrected detection net photon flux inferred from the PSF 90%
ECF aperture, calculated by counting X-ray events, in the ACIS hard (2.0-7.0
keV) energy band. These fluxes represent the average background-subtracted
fluxes in the modified source region, corrected by the appropriate PSF
aperture fractions, livetime, and exposure for all valid observations in the
stack.
M_Photflux_Ap90
The aperture-corrected detection net photon flux inferred from the PSF 90%
ECF aperture, calculated by counting X-ray events, in the ACIS medium
(1.2-2.0 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
S_Photflux_Ap90
The aperture-corrected detection net photon flux inferred from the PSF 90%
ECF aperture, calculated by counting X-ray events, in the ACIS soft (0.5-1.2
keV) energy band. These fluxes represent the average background-subtracted
fluxes in the modified source region, corrected by the appropriate PSF
aperture fractions, livetime, and exposure for all valid observations in the
stack.
U_Photflux_Ap90
The aperture-corrected detection net photon flux inferred from the PSF 90%
ECF aperture, calculated by counting X-ray events, in the ACIS ultrasoft
(0.2-0.5 keV) energy band. These fluxes represent the average
background-subtracted fluxes in the modified source region, corrected by the
appropriate PSF aperture fractions, livetime, and exposure for all valid
observations in the stack.
W_Photflux_Ap90
The aperture-corrected detection net photon flux inferred from the PSF 90%
ECF aperture, calculated by counting X-ray events, in the HRC wide (~0.1-10.0
keV)) energy band. These fluxes represent the average background-subtracted
fluxes in the modified source region, corrected by the appropriate PSF
aperture fractions, livetime, and exposure for all valid observations in the
stack.
B_Photflux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS broad (0.5-7.0) energy band.
H_Photflux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS hard (2.0-7.0 keV) energy band.
M_Photflux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, ACIS medium (1.2-2.0 keV) energy band.
S_Photflux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS soft (0.5-1.2 keV) energy band.
U_Photflux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS ultrasoft (0.2-0.5 keV) energy band.
W_Photflux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the HRC wide (~0.1-10.0 keV) energy band.
B_Photflux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS broad (0.5-7.0 keV) energy band.
H_Photflux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS hard (2.0-7.0 keV) energy band.
M_Photflux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS medium (1.2-2.0 keV) energy band.
S_Photflux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the ACIS soft (0.5-1.2 keV) energy band.
U_Photflux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, ACIS ultrasoft (0.2-0.5 keV) energy band.
W_Photflux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
photon flux inferred from the PSF 90% ECF aperture, calculated by counting
X-ray events, in the HRC wide (~0.1-10.0 keV) energy band.
B_Flux_Ap
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the source region aperture, calculated by counting X-ray
events, in the ACIS broad (0.5-7.0 keV) energy band. These fluxes represent
the average background-subtracted fluxes in the modified source region,
corrected by the appropriate PSF aperture fractions, livetime, and exposure
for all valid observations in the stack. The conversion from photon flux in
photons s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon
energies for each incident source photon and scaling by the local value of
the ARF at the location of the incident photon.
H_Flux_Ap
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the source region aperture, calculated by counting X-ray
events, in the ACIS hard (2.0-7.0 keV) energy band. These fluxes represent
the average background-subtracted fluxes in the modified source region,
corrected by the appropriate PSF aperture fractions, livetime, and exposure
for all valid observations in the stack. The conversion from photon flux in
photons s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon
energies for each incident source photon and scaling by the local value of
the ARF at the location of the incident photon.
M_Flux_Ap
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the source region aperture, calculated by counting X-ray
events, in the ACIS medium (1.2-2.0 keV) energy band. These fluxes represent
the average background-subtracted fluxes in the modified source region,
corrected by the appropriate PSF aperture fractions, livetime, and exposure
for all valid observations in the stack. The conversion from photon flux in
photons s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon
energies for each incident source photon and scaling by the local value of
the ARF at the location of the incident photon.
S_Flux_Ap
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the source region aperture, calculated by counting X-ray
events, in the ACIS soft (0.5-1.2 keV) energy band. These fluxes represent
the average background-subtracted fluxes in the modified source region,
corrected by the appropriate PSF aperture fractions, livetime, and exposure
for all valid observations in the stack. The conversion from photon flux in
photons s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon
energies for each incident source photon and scaling by the local value of
the ARF at the location of the incident photon.
U_Flux_Ap
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the source region aperture, calculated by counting X-ray
events, in the ACIS ultrasoft (0.2-0.5 keV) energy band. These fluxes
represent the average background-subtracted fluxes in the modified source
region, corrected by the appropriate PSF aperture fractions, livetime, and
exposure for all valid observations in the stack. The conversion from photon
flux in photons s-1 cm-2 to ergs s-1 cm-2 is performed by summing the
photon energies for each incident source photon and scaling by the local
value of the ARF at the location of the incident photon.
W_Flux_Ap
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the source region aperture, calculated by counting X-ray
events, in the HRC wide (~0.1-10.0 keV) energy band. These fluxes represent
the average background-subtracted fluxes in the modified source region,
corrected by the appropriate PSF aperture fractions, livetime, and exposure
for all valid observations in the stack. The conversion from photon flux in
photons s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon
energies for each incident source photon and scaling by the local value of
the ARF at the location of the incident photon.
B_Flux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS broad (0.5-7.0 keV)
energy band.
H_Flux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS hard (2.0-7.0 keV)
energy band.
M_Flux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS medium (1.2-2.0 keV)
energy band.
S_Flux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS soft (0.5-1.2 keV)
energy band.
U_Flux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS ultrasoft (0.2-0.5 keV)
energy band.
W_Flux_Ap_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the HRC wide (~0.1-10.0 keV)
energy band.
B_Flux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS broad (0.5-7.0 keV)
energy band.
H_Flux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS hard (2.0-7.0 keV)
energy band.
M_Flux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS medium (1.2-2.0 keV)
energy band.
S_Flux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS soft (0.5-1.2 keV)
energy band.
U_Flux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the ACIS ultrasoft (0.2-0.5 keV)
energy band.
W_Flux_Ap_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the source region aperture
and calculated by counting X-ray events, in the HRC wide (~0.1-10.0 keV)
energy band.
B_Flux_Ap90
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the PSF 90% ECF aperture, calculated by counting X-ray events,
in the ACIS broad (0.5-7.0 keV) energy band. These fluxes represent the
average background-subtracted fluxes in the modified source region, corrected
by the appropriate PSF aperture fractions, livetime, and exposure for all
valid observations in the stack. The conversion from photon flux in photons
s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon energies
for each incident source photon and scaling by the local value of the ARF at
the location of the incident photon.
H_Flux_Ap90
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the PSF 90% ECF aperture, calculated by counting X-ray events,
in the ACIS hard (2.0-7.0 keV) energy band. These fluxes represent the
average background-subtracted fluxes in the modified source region, corrected
by the appropriate PSF aperture fractions, livetime, and exposure for all
valid observations in the stack. The conversion from photon flux in photons
s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon energies
for each incident source photon and scaling by the local value of the ARF at
the location of the incident photon.
M_Flux_Ap90
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the PSF 90% ECF aperture, calculated by counting X-ray events,
in the ACIS medium (1.2-2.0 keV) energy band. These fluxes represent the
average background-subtracted fluxes in the modified source region, corrected
by the appropriate PSF aperture fractions, livetime, and exposure for all
valid observations in the stack. The conversion from photon flux in photons
s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon energies
for each incident source photon and scaling by the local value of the ARF at
the location of the incident photon.
S_Flux_Ap90
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the PSF 90% ECF aperture, calculated by counting X-ray events,
in the ACIS soft (0.5-1.2 keV) energy band. These fluxes represent the
average background-subtracted fluxes in the modified source region, corrected
by the appropriate PSF aperture fractions, livetime, and exposure for all
valid observations in the stack. The conversion from photon flux in photons
s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon energies
for each incident source photon and scaling by the local value of the ARF at
the location of the incident photon.
U_Flux_Ap90
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the PSF 90% ECF aperture, calculated by counting X-ray events,
in the ACIS ultrasoft (0.2-0.5 keV) energy band. These fluxes represent the
average background-subtracted fluxes in the modified source region, corrected
by the appropriate PSF aperture fractions, livetime, and exposure for all
valid observations in the stack. The conversion from photon flux in photons
s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon energies
for each incident source photon and scaling by the local value of the ARF at
the location of the incident photon.
W_Flux_Ap90
The aperture-corrected detection net energy flux, in erg s-1 cm-2,
inferred from the PSF 90% ECF aperture, calculated by counting X-ray events,
in the HRC wide (~0.1-10.0 keV) energy band. These fluxes represent the
average background-subtracted fluxes in the modified source region, corrected
by the appropriate PSF aperture fractions, livetime, and exposure for all
valid observations in the stack. The conversion from photon flux in photons
s-1 cm-2 to ergs s-1 cm-2 is performed by summing the photon energies
for each incident source photon and scaling by the local value of the ARF at
the location of the incident photon.
B_Flux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS broad (0.5-7.0 keV) energy
band.
H_Flux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS hard (2.0-7.0 keV) energy
band.
M_Flux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS medium (1.2-2.0 keV) energy
band.
S_Flux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS soft (0.5-1.2 keV) energy
band.
U_Flux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS ultrasoft (0.2-0.5 keV)
energy band.
W_Flux_Ap90_Lo
The 68% lower confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the HRC wide (~0.1-10.0 keV) energy
band.
B_Flux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS broad (0.5-7.0 keV) energy
band.
H_Flux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS hard (2.0-7.0 keV) energy
band.
M_Flux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS medium (1.2-2.0 keV) energy
band.
S_Flux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS soft (0.5-1.2 keV) energy
band.
U_Flux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the ACIS ultrasoft (0.2-0.5 keV)
energy band.
W_Flux_Ap90_Hi
The 68% upper confidence limit for the aperture-corrected detection net
energy flux, in erg s-1 cm-2, inferred from the PSF 90% ECF aperture,
calculated by counting X-ray events, in the HRC wide (~0.1-10.0 keV) energy
band.
Hardness_Ratio_HM
The ACIS hard (2.0-7.0 keV) to medium (1.2-2.0 keV) energy band photon flux
hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio. The
aperture fluxes are reported from marginalized probability distributions,
which in turn are used to calculate marginalized probability distributions
for the hardness ratios. As the reported values for each of these quantities
represent the modes of their given distributions, the column hardness ratio
values might differ slightly from that calculated directly from the aperture
fluxes reported in the catalog.
Hardness_Ratio_HM_Lo
The 68% lower confidence limit for the ACIS hard (2.0-7.0 keV) to medium
(1.2-2.0 keV) energy band photon flux hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio.
Hardness_Ratio_HM_Hi
The 68% upper confidence limit for the ACIS hard (2.0-7.0 keV) to medium
(1.2-2.0 keV) energy band photon flux hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio.
Var_Inter_Hard_Hm_Prob
The inter-observation ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy
band photon flux hardness ratio variability probability. This records the
probability that the source region hardness ratios varied between the
contributing observations, based on the hypothesis rejection test described
in the hardness ratios and variability
memo.
The definition of the hardness ratio PDFs can be found in the
memo,
and also in the hardness ratios columns page:
https://cxc.cfa.harvard.edu/csc2.1/columns/spectral_properties.html#hrd_ratios.
High values of var_inter_hard_prob indicate that the source is spectrally
variable in the corresponding combination of bands.
Var_Inter_Hard_Hm_Sigma
The inter-observation ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy
band photon flux hardness ratio variability standard deviation. This quantity
is the absolute value of the difference between the error weighted mean of
the source region photon flux density PDF when a single hardness ratio is
assumed, and the mean of the source region hardness ratio PDF for the
individual observation that maximizes the absolute value of the difference.
Of all the contributing observations, the observation that yields the highest
value for this equation, is used in computing this value. Intuitively, this
quantity can be interpreted as the variance of the individual observation
hardness ratios. This is described in the CSC documentation here:
https://cxc.cfa.harvard.edu/csc2.1/columns/variability.html.
Hardness_Ratio_HS
The ACIS hard (2.0-7.0 keV) to soft (0.5-1.2 keV) energy band photon flux
hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio. The
aperture fluxes are reported from marginalized probability distributions,
which in turn are used to calculate marginalized probability distributions
for the hardness ratios. As the reported values for each of these quantities
represent the modes of their given distributions, the column hardness ratio
values might differ slightly from that calculated directly from the aperture
fluxes reported in the catalog.
Hardness_Ratio_HS_Lo
The 68% lower confidence limit for the ACIS hard (2.0-7.0 keV) to soft
(0.5-1.2 keV) energy band photon flux hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio.
Hardness_Ratio_HS_Hi
The 68% upper confidence limit for the ACIS hard (2.0-7.0 keV) to soft
(0.5-1.2 keV) energy band photon flux hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio.
Var_Inter_Hard_Hs_Prob
The inter-observation ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy
band photon flux hardness ratio variability probability. This records the
probability that the source region hardness ratios varied between the
contributing observations, based on the hypothesis rejection test described
in the hardness ratios and variability
memo.
The definition of the hardness ratio PDFs can be found in the
memo,
and also in the hardness ratios columns page:
https://cxc.cfa.harvard.edu/csc2.1/columns/spectral_properties.html#hrd_ratios.
High values of var_inter_hard_prob indicate that the source is spectrally
variable in the corresponding combination of bands.
Var_Inter_Hard_Hs_Sigma
The inter-observation ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy
band photon flux hardness ratio variability standard deviation. This quantity
is the absolute value of the difference between the error weighted mean of
the source region photon flux density PDF when a single hardness ratio is
assumed, and the mean of the source region hardness ratio PDF for the
individual observation that maximizes the absolute value of the difference.
Of all the contributing observations, the observation that yields the highest
value for this equation, is used in computing this value. Intuitively, this
quantity can be interpreted as the variance of the individual observation
hardness ratios. This is described in the CSC documentation here:
https://cxc.cfa.harvard.edu/csc2.1/columns/variability.html.
Hardness_Ratio_MS
The ACIS medium (1.2-2.0 keV) to soft (0.5-1.2 keV) energy band photon flux
hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio. The
aperture fluxes are reported from marginalized probability distributions,
which in turn are used to calculate marginalized probability distributions
for the hardness ratios. As the reported values for each of these quantities
represent the modes of their given distributions, the column hardness ratio
values might differ slightly from that calculated directly from the aperture
fluxes reported in the catalog.
Hardness_Ratio_MS_Lo
The 68% lower confidence limit for the medium (1.2-2.0 keV) to soft (0.5-1.2
keV) energy band photon flux hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio.
Hardness_Ratio_MS_Hi
The 68% upper confidence limit for the medium (1.2-2.0 keV) to soft (0.5-1.2
keV) energy band photon flux hardness ratio, as described in
https://cxc.cfa.harvard.edu/csc/dictionary/entries.html#hardness_ratio.
Var_Inter_Hard_Ms_Prob
The inter-observation ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy
band photon flux hardness ratio variability probability. This records the
probability that the source region hardness ratios varied between the
contributing observations, based on the hypothesis rejection test described
in the hardness ratios and variability
memo.
The definition of the hardness ratio PDFs can be found in the
memo,
and also in the hardness ratios columns page:
https://cxc.cfa.harvard.edu/csc2.1/columns/spectral_properties.html#hrd_ratios.
High values of var_inter_hard_prob indicate that the source is spectrally
variable in the corresponding combination of bands.
Var_Inter_Hard_Ms_Sigma
The inter-observation ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy
band photon flux hardness ratio variability standard deviation. This quantity
is the absolute value of the difference between the error weighted mean of
the source region photon flux density PDF when a single hardness ratio is
assumed, and the mean of the source region hardness ratio PDF for the
individual observation that maximizes the absolute value of the difference.
Of all the contributing observations, the observation that yields the highest
value for this equation, is used in computing this value. Intuitively, this
quantity can be interpreted as the variance of the individual observation
hardness ratios. This is described in the CSC documentation here:
https://cxc.cfa.harvard.edu/csc2.1/columns/variability.html.
B_Ks_Intra_Prob
The intra-observation Kolmogorov-Smirnov test variability probability
(highest value across all observations) in the ACIS broad (0.5-7.0 keV)
energy band. This measures the probability that the arrival times of the
events within the source region are inconsistent with a constant source count
rate throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample K-S test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
H_Ks_Intra_Prob
The intra-observation Kolmogorov-Smirnov test variability probability
(highest value across all observations )in the ACIS hard (2.0-7.0 keV) energy
band. This measures the probability that the arrival times of the events
within the source region are inconsistent with a constant source count rate
throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample K-S test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
M_Ks_Intra_Prob
The intra-observation Kolmogorov-Smirnov test variability probability
(highest value across all observations) in the ACIS medium (1.2-2.0 keV)
energy band. This measures the probability that the arrival times of the
events within the source region are inconsistent with a constant source count
rate throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample K-S test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
S_Ks_Intra_Prob
The intra-observation Kolmogorov-Smirnov test variability probability
(highest value across all observations) in the ACIS soft (0.5-1.2 keV) energy
band. This measures the probability that the arrival times of the events
within the source region are inconsistent with a constant source count rate
throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample K-S test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
U_Ks_Intra_Prob
The intra-observation Kolmogorov-Smirnov test variability probability
(highest value across all observations) in the ACIS broad (0.2-0.5 keV)
energy band. This measures the probability that the arrival times of the
events within the source region are inconsistent with a constant source count
rate throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample K-S test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
W_Ks_Intra_Prob
The intra-observation Kolmogorov-Smirnov test variability probability
(highest value across all observations) in the HRC wide (~0.1-10.0 keV)
energy band. This measures the probability that the arrival times of the
events within the source region are inconsistent with a constant source count
rate throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample K-S test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
B_Kp_Intra_Prob
The intra-observation Kuiper's test variability probability (highest value
across all stacked observations) in the ACIS broad (0.5-7.0 keV) energy band.
This measures the probability that the arrival times of the events within the
source region are inconsistent with a constant source count rate throughout
the observation. High values of this quantity imply that the source is not
consistent with a constant rate, and that the source is likely variable. The
probability is computed by means of a hypothesis rejection test from a
one-sample Kuiper's test applied to the unbinned event data, with corrections
applied for good time intervals and for the source region dithering across
regions of variable exposure (e.g., chip edges) during the observation.
Probability values are calculated for each science energy band. Note that
this variability diagnostic does not treat the source and background
separately.
H_Kp_Intra_Prob
The intra-observation Kuiper's test variability probability (highest value
across all stacked observations) in the ACIS hard (2.0-7.0 keV) energy band.
This measures the probability that the arrival times of the events within the
source region are inconsistent with a constant source count rate throughout
the observation. High values of this quantity imply that the source is not
consistent with a constant rate, and that the source is likely variable. The
probability is computed by means of a hypothesis rejection test from a
one-sample Kuiper's test applied to the unbinned event data, with corrections
applied for good time intervals and for the source region dithering across
regions of variable exposure (e.g., chip edges) during the observation.
Probability values are calculated for each science energy band. Note that
this variability diagnostic does not treat the source and background
separately.
M_Kp_Intra_Prob
The intra-observation Kuiper's test variability probability (highest value
across all stacked observations) in the ACIS medium (1.2-2.0 keV) energy
band. This measures the probability that the arrival times of the events
within the source region are inconsistent with a constant source count rate
throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample Kuiper's test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
S_Kp_Intra_Prob
The intra-observation Kuiper's test variability probability (highest value
across all stacked observations) in the ACIS soft (0.5-1.2 keV) energy band.
This measures the probability that the arrival times of the events within the
source region are inconsistent with a constant source count rate throughout
the observation. High values of this quantity imply that the source is not
consistent with a constant rate, and that the source is likely variable. The
probability is computed by means of a hypothesis rejection test from a
one-sample Kuiper's test applied to the unbinned event data, with corrections
applied for good time intervals and for the source region dithering across
regions of variable exposure (e.g., chip edges) during the observation.
Probability values are calculated for each science energy band. Note that
this variability diagnostic does not treat the source and background
separately.
U_Kp_Intra_Prob
The intra-observation Kuiper's test variability probability (highest value
across all stacked observations) in the ACIS ultrasoft (0.2-0.5 keV) energy
band. This measures the probability that the arrival times of the events
within the source region are inconsistent with a constant source count rate
throughout the observation. High values of this quantity imply that the
source is not consistent with a constant rate, and that the source is likely
variable. The probability is computed by means of a hypothesis rejection test
from a one-sample Kuiper's test applied to the unbinned event data, with
corrections applied for good time intervals and for the source region
dithering across regions of variable exposure (e.g., chip edges) during the
observation. Probability values are calculated for each science energy band.
Note that this variability diagnostic does not treat the source and
background separately.
W_Kp_Intra_Prob
The intra-observation Kuiper's test variability probability (highest value
across all stacked observations) in the HRC wide (~0.1-10.0 keV) energy band.
This measures the probability that the arrival times of the events within the
source region are inconsistent with a constant source count rate throughout
the observation. High values of this quantity imply that the source is not
consistent with a constant rate, and that the source is likely variable. The
probability is computed by means of a hypothesis rejection test from a
one-sample Kuiper's test applied to the unbinned event data, with corrections
applied for good time intervals and for the source region dithering across
regions of variable exposure (e.g., chip edges) during the observation.
Probability values are calculated for each science energy band. Note that
this variability diagnostic does not treat the source and background
separately.
B_Var_Intra_Prob
The intra-observation Gregory-Loredo variability probability (highest value
across all stacked observations) in the ACIS broad (0.5-7.0 keV) energy band.
This measures the probability that the source region count rate lightcurve is
the result of multiple, uniformly sampled time bins, each with different
rates, as opposed to the result of a single, uniform rate time bin, and is
based upon the odd ratios (for describing the lightcurve with two or more
bins of potentially different rates) calculated from a Gregory-Loredo
analysis of the arrival times of the events within the source region.
Corrections to the event rate are applied accounting for good time intervals
and for the source region dithering across regions of variable exposure
(e.g., chip edges) during the observation.
H_Var_Intra_Prob
The intra-observation Gregory-Loredo variability probability (highest value
across all stacked observations) in the ACIS hard (2.0-7.0 keV) energy band.
This measures the probability that the source region count rate lightcurve is
the result of multiple, uniformly sampled time bins, each with different
rates, as opposed to the result of a single, uniform rate time bin, and is
based upon the odd ratios (for describing the lightcurve with two or more
bins of potentially different rates) calculated from a Gregory-Loredo
analysis of the arrival times of the events within the source region.
Corrections to the event rate are applied accounting for good time intervals
and for the source region dithering across regions of variable exposure
(e.g., chip edges) during the observation.
M_Var_Intra_Prob
The intra-observation Gregory-Loredo variability probability (highest value
across all stacked observations) in the ACIS medium (1.2-2.0 keV) energy
band. This measures the probability that the source region count rate
lightcurve is the result of multiple, uniformly sampled time bins, each with
different rates, as opposed to the result of a single, uniform rate time bin,
and is based upon the odd ratios (for describing the lightcurve with two or
more bins of potentially different rates) calculated from a Gregory-Loredo
analysis of the arrival times of the events within the source region.
Corrections to the event rate are applied accounting for good time intervals
and for the source region dithering across regions of variable exposure
(e.g., chip edges) during the observation.
S_Var_Intra_Prob
The intra-observation Gregory-Loredo variability probability (highest value
across all stacked observations) in the ACIS soft (0.5-1.2 keV) energy band.
This measures the probability that the source region count rate lightcurve is
the result of multiple, uniformly sampled time bins, each with different
rates, as opposed to the result of a single, uniform rate time bin, and is
based upon the odd ratios (for describing the lightcurve with two or more
bins of potentially different rates) calculated from a Gregory-Loredo
analysis of the arrival times of the events within the source region.
Corrections to the event rate are applied accounting for good time intervals
and for the source region dithering across regions of variable exposure
(e.g., chip edges) during the observation.
U_Var_Intra_Prob
The intra-observation Gregory-Loredo variability probability (highest value
across all stacked observations) in the ACIS ultrasoft (0.2-0.5 keV) energy
band. This measures the probability that the source region count rate
lightcurve is the result of multiple, uniformly sampled time bins, each with
different rates, as opposed to the result of a single, uniform rate time bin,
and is based upon the odd ratios (for describing the lightcurve with two or
more bins of potentially different rates) calculated from a Gregory-Loredo
analysis of the arrival times of the events within the source region.
Corrections to the event rate are applied accounting for good time intervals
and for the source region dithering across regions of variable exposure
(e.g., chip edges) during the observation.
W_Var_Intra_Prob
The intra-observation Gregory-Loredo variability probability (highest value
across all stacked observations) in the HRC wide (~0.1-10.0 keV) energy band.
This measures the probability that the source region count rate lightcurve is
the result of multiple, uniformly sampled time bins, each with different
rates, as opposed to the result of a single, uniform rate time bin, and is
based upon the odd ratios (for describing the lightcurve with two or more
bins of potentially different rates) calculated from a Gregory-Loredo
analysis of the arrival times of the events within the source region.
Corrections to the event rate are applied accounting for good time intervals
and for the source region dithering across regions of variable exposure
(e.g., chip edges) during the observation.
B_Var_Intra_Index
The intra-observation Gregory-Loredo variability index in the range [0, 10],
which indicates whether the source region photon flux in the ACIS broad
(0.5-7.0 keV) energy band is constant within an observation (highest value
across all stacked observations). This index combines (a) the Gregory-Loredo
variability probability with (b) the fractions of the multi-resolution light
curve output by the Gregory-Loredo analysis that are within 3 and 5 sigma of
the average count rate, to evaluate whether the source region flux is uniform
throughout the observation. See the Gregory-Loredo Probability How and Why
topic
for a definition of this index value.
H_Var_Intra_Index
The intra-observation Gregory-Loredo variability index in the range [0, 10],
which indicates whether the source region photon flux in the ACIS hard
(2.0-7.0 keV) energy band is constant within an observation (highest value
across all stacked observations). This index combines (a) the Gregory-Loredo
variability probability with (b) the fractions of the multi-resolution light
curve output by the Gregory-Loredo analysis that are within 3 and 5 sigma of
the average count rate, to evaluate whether the source region flux is uniform
throughout the observation. See the Gregory-Loredo Probability How and Why
topic
for a definition of this index value.
M_Var_Intra_Index
The intra-observation Gregory-Loredo variability index in the range [0, 10],
which indicates whether the source region photon flux in the ACIS medium
(1.2-2.0 keV) energy band is constant within an observation (highest value
across all stacked observations). This index combines (a) the Gregory-Loredo
variability probability with (b) the fractions of the multi-resolution light
curve output by the Gregory-Loredo analysis that are within 3 and 5 sigma of
the average count rate, to evaluate whether the source region flux is uniform
throughout the observation. See the Gregory-Loredo Probability How and Why
topic
for a definition of this index value.
S_Var_Intra_Index
The intra-observation Gregory-Loredo variability index in the range [0, 10],
which indicates whether the source region photon flux in the ACIS soft
(0.5-1.2 keV) energy band is constant within an observation (highest value
across all stacked observations). This index combines (a) the Gregory-Loredo
variability probability with (b) the fractions of the multi-resolution light
curve output by the Gregory-Loredo analysis that are within 3 and 5 sigma of
the average count rate, to evaluate whether the source region flux is uniform
throughout the observation. See the Gregory-Loredo Probability How and Why
topic
for a definition of this index value.
U_Var_Intra_Index
The intra-observation Gregory-Loredo variability index in the range [0, 10],
which indicates whether the source region photon flux in the ACIS ultrasoft
(0.2-0.5 keV) energy band is constant within an observation (highest value
across all stacked observations). This index combines (a) the Gregory-Loredo
variability probability with (b) the fractions of the multi-resolution light
curve output by the Gregory-Loredo analysis that are within 3 and 5 sigma of
the average count rate, to evaluate whether the source region flux is uniform
throughout the observation. See the Gregory-Loredo Probability How and Why
topic
for a definition of this index value.
W_Var_Intra_Index
The intra-observation Gregory-Loredo variability index in the range [0, 10],
which indicates whether the source region photon flux in the HRC wide
(~0.1-10.0 keV) energy band is constant within an observation (highest value
across all stacked observations). This index combines (a) the Gregory-Loredo
variability probability with (b) the fractions of the multi-resolution light
curve output by the Gregory-Loredo analysis that are within 3 and 5 sigma of
the average count rate, to evaluate whether the source region flux is uniform
throughout the observation. See the Gregory-Loredo Probability How and Why
topic
for a definition of this index value.
B_Var_Inter_Prob
The inter-stacked observation variability probability, calculated from the
chi2 distribution of the photon fluxes of the individual observations in
the ACIS broad (0.5-7.0 keV) energy band. This records the probability that
the source region photon flux varied between the contributing observations,
based on the hypothesis rejection test described in the hardness ratios and
variability
memo.
Additional information is available here:
https://cxc.cfa.harvard.edu/csc/columns/variability.html#gl_var_prob.
H_Var_Inter_Prob
The inter-stacked observation variability probability, calculated from the
chi2 distribution of the photon fluxes of the individual observations in
the ACIS hard (2.0-7.0 keV) energy band. This records the probability that
the source region photon flux varied between the contributing observations,
based on the hypothesis rejection test described in the hardness ratios and
variability
memo.
Additional information is available here:
https://cxc.cfa.harvard.edu/csc/columns/variability.html#gl_var_prob.
M_Var_Inter_Prob
The inter-stacked observation variability probability, calculated from the
chi2 distribution of the photon fluxes of the individual observations in
the ACIS medium (1.2-2.0 keV) energy band. This records the probability that
the source region photon flux varied between the contributing observations,
based on the hypothesis rejection test described in the hardness ratios and
variability
memo.
Additional information is available here:
https://cxc.cfa.harvard.edu/csc/columns/variability.html#gl_var_prob.
S_Var_Inter_Prob
The inter-stacked observation variability probability, calculated from the
chi2 distribution of the photon fluxes of the individual observations in
the ACIS soft (0.5-1.2 keV) energy band. This records the probability that
the source region photon flux varied between the contributing observations,
based on the hypothesis rejection test described in the hardness ratios and
variability
memo.
Additional information is available here:
https://cxc.cfa.harvard.edu/csc/columns/variability.html#gl_var_prob.
U_Var_Inter_Prob
The inter-stacked observation variability probability, calculated from the
chi2 distribution of the photon fluxes of the individual observations in
the ACIS ultrasoft (0.2-0.5 keV) energy band. This records the probability
that the source region photon flux varied between the contributing
observations, based on the hypothesis rejection test described in the
hardness ratios and variability
memo.
Additional information is available here:
https://cxc.cfa.harvard.edu/csc/columns/variability.html#gl_var_prob.
W_Var_Inter_Prob
The inter-stacked observation variability probability, calculated from the
chi2 distribution of the photon fluxes of the individual observations in
the HRC wide (~0.1-10.0 keV) energy band. This records the probability that
the source region photon flux varied between the contributing observations,
based on the hypothesis rejection test described in the hardness ratios and
variability
memo.
Additional information is available here:
https://cxc.cfa.harvard.edu/csc/columns/variability.html#gl_var_prob.
B_Var_Inter_Index
The inter-stacked-observation variability index in the range [0, 10], which
indicates whether the source region photon flux is constant between
observations in the ACIS broad (0.5-7.0 keV) energy band. It is used to
evaluate whether the source region photon flux is constant between the
observations. The degree of confidence in variability expressed by this index
is similar to that of the intra-observation variability index. The indices
are described here, which
https://cxc.cfa.harvard.edu/csc/columns/variability.html#var_inter_index.
H_Var_Inter_Index
The inter-stacked-observation variability index in the range [0, 10], which
indicates whether the source region photon flux is constant between
observations in the ACIS hard (2.0-7.0 keV) energy band. It is used to
evaluate whether the source region photon flux is constant between the
observations. The degree of confidence in variability expressed by this index
is similar to that of the intra-observation variability index. The indices
are described here, which
https://cxc.cfa.harvard.edu/csc/columns/variability.html#var_inter_index.
M_Var_Inter_Index
The inter-stacked-observation variability index in the range [0, 10], which
indicates whether the source region photon flux is constant between
observations in the ACIS medium (1.2-2.0 keV) energy band. It is used to
evaluate whether the source region photon flux is constant between the
observations. The degree of confidence in variability expressed by this index
is similar to that of the intra-observation variability index. The indices
are described here, which
https://cxc.cfa.harvard.edu/csc/columns/variability.html#var_inter_index.
S_Var_Inter_Index
The inter-stacked-observation variability index in the range [0, 10], which
indicates whether the source region photon flux is constant between
observations in the ACIS soft (0.5-1.2 keV) energy band. It is used to
evaluate whether the source region photon flux is constant between the
observations. The degree of confidence in variability expressed by this index
is similar to that of the intra-observation variability index. The indices
are described here, which
https://cxc.cfa.harvard.edu/csc/columns/variability.html#var_inter_index.
U_Var_Inter_Index
The inter-stacked-observation variability index in the range [0, 10], which
indicates whether the source region photon flux is constant between
observations in the ACIS ultrasoft (0.2-0.5 keV) energy band. It is used to
evaluate whether the source region photon flux is constant between the
observations. The degree of confidence in variability expressed by this index
is similar to that of the intra-observation variability index. The indices
are described here, which
https://cxc.cfa.harvard.edu/csc/columns/variability.html#var_inter_index.
W_Var_Inter_Index
The inter-stacked-observation variability index in the range [0, 10], which
indicates whether the source region photon flux is constant between
observations in the HRC wide (~0.1-10.0 keV) energy band. It is used to
evaluate whether the source region photon flux is constant between the
observations. The degree of confidence in variability expressed by this index
is similar to that of the intra-observation variability index. The indices
are described here, which
https://cxc.cfa.harvard.edu/csc/columns/variability.html#var_inter_index.
B_Var_Inter_Sigma
The inter-stacked-observation flux variability standard deviation in the the
spread of the individual observation photon fluxes about the error weighted
mean in the ACIS broad (0.5-7.0 keV) energy band. This value is the absolute
value of the difference between the error weighted mean of the source region
photon flux density PDF when a single flux is assumed, and the mean of the
source region photon flux density PDF for the individual observation that
maximizes the absolute value of the difference. Of all the contributing
observations, the observation that yields the highest value for this
equation, is used in computing this value, which is recorded in
var_inter_sigma. Intuitively, this quantity can be interpreted as the
variance of the individual observation fluxes.
H_Var_Inter_Sigma
The inter-stacked-observation flux variability standard deviation in the the
spread of the individual observation photon fluxes about the error weighted
mean in the ACIS hard (2.0-7.0 keV) energy band. This value is the absolute
value of the difference between the error weighted mean of the source region
photon flux density PDF when a single flux is assumed, and the mean of the
source region photon flux density PDF for the individual observation that
maximizes the absolute value of the difference. Of all the contributing
observations, the observation that yields the highest value for this
equation, is used in computing this value, which is recorded in
var_inter_sigma. Intuitively, this quantity can be interpreted as the
variance of the individual observation fluxes.
M_Var_Inter_Sigma
The inter-stacked-observation flux variability standard deviation in the the
spread of the individual observation photon fluxes about the error weighted
mean in the ACIS medium (1.2-2.0 keV) energy band. This value is the absolute
value of the difference between the error weighted mean of the source region
photon flux density PDF when a single flux is assumed, and the mean of the
source region photon flux density PDF for the individual observation that
maximizes the absolute value of the difference. Of all the contributing
observations, the observation that yields the highest value for this
equation, is used in computing this value, which is recorded in
var_inter_sigma. Intuitively, this quantity can be interpreted as the
variance of the individual observation fluxes.
S_Var_Inter_Sigma
The inter-stacked-observation flux variability standard deviation in the the
spread of the individual observation photon fluxes about the error weighted
mean in the ACIS soft (0.5-1.2 keV) energy band. This value is the absolute
value of the difference between the error weighted mean of the source region
photon flux density PDF when a single flux is assumed, and the mean of the
source region photon flux density PDF for the individual observation that
maximizes the absolute value of the difference. Of all the contributing
observations, the observation that yields the highest value for this
equation, is used in computing this value, which is recorded in
var_inter_sigma. Intuitively, this quantity can be interpreted as the
variance of the individual observation fluxes.
U_Var_Inter_Sigma
The inter-stacked-observation flux variability standard deviation in the the
spread of the individual observation photon fluxes about the error weighted
mean in the ACIS ultrasoft (0.2-0.5 keV) energy band. This value is the
absolute value of the difference between the error weighted mean of the
source region photon flux density PDF when a single flux is assumed, and the
mean of the source region photon flux density PDF for the individual
observation that maximizes the absolute value of the difference. Of all the
contributing observations, the observation that yields the highest value for
this equation, is used in computing this value, which is recorded in
var_inter_sigma. Intuitively, this quantity can be interpreted as the
variance of the individual observation fluxes.
W_Var_Inter_Sigma
The inter-stacked-observation flux variability standard deviation in the the
spread of the individual observation photon fluxes about the error weighted
mean in the HRC wide (~0.1-10.0 keV) energy band. This value is the absolute
value of the difference between the error weighted mean of the source region
photon flux density PDF when a single flux is assumed, and the mean of the
source region photon flux density PDF for the individual observation that
maximizes the absolute value of the difference. Of all the contributing
observations, the observation that yields the highest value for this
equation, is used in computing this value, which is recorded in
var_inter_sigma. Intuitively, this quantity can be interpreted as the
variance of the individual observation fluxes.
Dither_Warning_Flag
the highest statistically significant peak in the power spectrum of the
detection source region count rate occurs at the dither frequency or at a
beat frequency of the dither frequency in one or more of the stacked
observations. The dither warning flag for a compact detection is a Boolean
that has a value of TRUE if the dither warning flag for any contributing
per-observation detection is TRUE. Otherwise, the value is FALSE. The dither
warning flag for an extended (convex hull) source is always NULL.
Exposure
The effective stacked observation exposure time, in seconds, after applying
the good time intervals and the deadtime correction factor. The vignetting
and dead area corrections are NOT applied.
Contact Person
Questions regarding the CSCSTACK database table can be addressed to the HEASARC Help Desk.Page Author: Browse Software Development Team
Last Modified: Monday, 27-Jul-2026 22:37:44 EDT
- HEASARC Director: Vacant
- NASA Official: Ryan Smallcomb
- Web Curator: J.D. Myers
- Last Modified: 27-Jul-2026