Last modified: 25 March 2024

Stacked Observation Detections Table


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.

Note: Source properties in the catalog which have a value for each science energy band (type "double[6]", "long[6]", and "integer[6]" in the table below) have the corresponding letters appended to their names. For example, "flux_aper_b" and "flux_aper_h" represent the background-subtracted, aperture-corrected broad-band and hard-band energy fluxes, respectively.

Note: "Description" entries with a vertical bar running to the left of the text have more information available that will be displayed when the cursor hovers over the column description.

Switch to: Columns listed alphabetically
Context Column Name Type Units Description
Stack Identification detect_stack_id detect stack identifier (designation of observation stack used for source detection) in the format '{acis|hrc}fJhhmmsss{+|-}ddmmss_nnn'
ra_stack detect stack tangent plane reference position, ICRS right ascension
dec_stack detect stack tangent plane reference position, ICRS declination

Instrument Information instrument string instrument used for the observation: 'ACIS' or 'HRC'
grating string transmission grating used for the stacked observation: 'NONE', 'HETG', or 'LETG'

Aspect Information deltax double arcsec SKY coordinate system X translation correction required to co-align the observation stack astrometric frame with the Gaia-CRF3 realization of the ICRF
deltay double arcsec SKY coordinate system Y translation correction required to co-align the observation stack astrometric frame with the Gaia-CRF3 realization of the ICRF
deltarot double deg SKY coordinate system roll angle correction required to co-align the observation stack astrometric frame within with the Gaia-CRF3 realization of the ICRF
dscale double deg SKY coordinate system scale factor correction required to co-align the observation stack astrometric frame with the Gaia-CRF3 realization of the ICRF stack
man_astrom_flag Boolean Observation stack astrometric transform was manually modified by human review

Processing Information ascdsver string software version used to create the Level 3 detect stack event data file
caldbver string calibration database version used to calibrate the Level 3 detect stack event data file
crdate string creation date/time of the Level 3 detect stack event data file, UTC (yyyy-mm-ddThh:mm:ss)

Source Identification region_id integer detection region identifier (component number)

Source Position and Position Errors ra double deg
detection position, ICRS right ascension

From the Position and Position Errors column descriptions page:

The position of each stacked observation detection is defined by the ICRS right ascension and declination of the center of the source region in which the detection is located, which is in-turn determined from the wavdetect and/or mkvtbkg detections, as adjusted by the maximum likelihood estimator (MLE) fits to the observed X-ray event distributions.

dec double deg
detection position, ICRS declination

From the Position and Position Errors column descriptions page:

The position of each stacked observation detection is defined by the ICRS right ascension and declination of the center of the source region in which the detection is located, which is in-turn determined from the wavdetect and/or mkvtbkg detections, as adjusted by the maximum likelihood estimator (MLE) fits to the observed X-ray event distributions.

err_ellipse_r0 double arcsec
major radius of the 95% confidence level position error ellipse

From the Position and Position Errors column descriptions page:

The position of each stacked observation detection is defined by the ICRS right ascension and declination of the center of the source region in which the detection is located, which is in-turn determined from the wavdetect and/or mkvtbkg detections, as adjusted by the maximum likelihood estimator (MLE) fits to the observed X-ray event distributions.

err_ellipse_r1 double arcsec
minor radius of the 95% confidence level position error ellipse

From the Position and Position Errors column descriptions page:

The position of each stacked observation detection is defined by the ICRS right ascension and declination of the center of the source region in which the detection is located, which is in-turn determined from the wavdetect and/or mkvtbkg detections, as adjusted by the maximum likelihood estimator (MLE) fits to the observed X-ray event distributions.

err_ellipse_ang double deg
position angle (referenced from local true north) of the major axis 95% confidence level error ellipse

From the Position and Position Errors column descriptions page:

The position of each stacked observation detection is defined by the ICRS right ascension and declination of the center of the source region in which the detection is located, which is in-turn determined from the wavdetect and/or mkvtbkg detections, as adjusted by the maximum likelihood estimator (MLE) fits to the observed X-ray event distributions.

theta_mean double arcmin
mean source region aperture off-axis angle from all stacked observations

From the Position and Position Errors column descriptions page:

The mean source region aperture off-axis angle, θmean, computed by averaging the off-axis angles θ from all observations in a stack.


Source Significance flux_significance double[6]
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 each science energy band

From the Source Significance column descriptions page:

Likelihood, detect significance, and flux significance are reported per band for all sources detected in the valid stack. The likelihood reported is the maximum of the likelihood determined from the MLE fit to all valid stack data, and the likelihoods from each individual observation, per band.

Flux significance is a simple estimate of the ratio of the flux measurement to its average error. The mode of the marginalized probability distribution for photflux_aper is used as the flux measurement and the average error, \(\sigma_{e}\), is defined to be:

\[ \sigma_{e} = \frac{\mathit{photflux\_aper\_hilim} - \mathit{photflux\_aper\_lolim}}{2} \]

which are both used to estimate flux significance.

detect_significance double[6]
significance of the stacked-observation detection computed by the stacked-observation detection algorithm for each science energy band

From the Source Significance column descriptions page:

Likelihood, detect significance, and flux significance are reported per band for all sources detected in the valid stack. The likelihood reported is the maximum of the likelihood determined from the MLE fit to all valid stack data, and the likelihoods from each individual observation, per band.

The fundamental metric used to decide whether a source is included in CSC 2.1 is the likelihood,

\[ \mathcal{L}=-\ln{P} \ \mathrm{,} \]

where \(P\) is the probability that an MLE fit to a point or extended source model, in a region with no source, would yield a change in fit statistic as large or larger than that observed, when compared to a fit to background only.

The likelihood is closely related to the probability, \(P_{\mathrm{Pois}}\), that a Poisson distribution with a mean background in the source aperture would produce at least the number of counts observed in the aperture. This quantity, called detect_significance, is also reported in CSC 2.1. Smoothed background maps are used to estimate mean background, and detect_significance is expressed in terms of the number of \(\sigma\), \(z\), in a zero-mean, unit standard deviation Gaussian distribution that would yield an upper integral probability \(P_{\mathrm{Gaus}}\), from \(z\) to \(\infty\), equivalent to \(P_{\mathrm{Pois}}\). That is,

\[ P_{\mathrm{Pois}} = P_{\mathrm{Gaus}} \]

where

\[ P_{\mathrm{Gaus}} = \int_{z}^{\infty} \frac{e^{-x^{2}/2}}{\sqrt{2\pi}} dx \]
likelihood double[6]
log-likelihood of the stacked-observation detection computed by the Maximum Likelihood Estimator fit to the photon counts distribution for each science energy band

From the Source Significance column descriptions page:

Likelihood, detect significance, and flux significance are reported per band for all sources detected in the valid stack. The likelihood reported is the maximum of the likelihood determined from the MLE fit to all valid stack data, and the likelihoods from each individual observation, per band.

The fundamental metric used to decide whether a source is included in CSC 2.1 is the likelihood,

\[ \mathcal{L}=-\ln{P} \ \mathrm{,} \]

where \(P\) is the probability that an MLE fit to a point or extended source model, in a region with no source, would yield a change in fit statistic as large or larger than that observed, when compared to a fit to background only.

The likelihood is closely related to the probability, \(P_{\mathrm{Pois}}\), that a Poisson distribution with a mean background in the source aperture would produce at least the number of counts observed in the aperture. This quantity, called detect_significance, is also reported in CSC 2.1. Smoothed background maps are used to estimate mean background, and detect_significance is expressed in terms of the number of \(\sigma\), \(z\), in a zero-mean, unit standard deviation Gaussian distribution that would yield an upper integral probability \(P_{\mathrm{Gaus}}\), from \(z\) to \(\infty\), equivalent to \(P_{\mathrm{Pois}}\). That is,

\[ P_{\mathrm{Pois}} = P_{\mathrm{Gaus}} \]

where

\[ P_{\mathrm{Gaus}} = \int_{z}^{\infty} \frac{e^{-x^{2}/2}}{\sqrt{2\pi}} dx \]
likelihood_class string highest detection likelihood classification across all energy bands

Source Codes and Flags conf_code integer
compact detection may be confused (bit encoded: 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)

From the Source Flags column descriptions page:

The confusion code for a compact detection is a 16-bit coded integer that has all bits 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 detection. Otherwise, the bits are set as follows:

Bit Value Code
1 1 Background region overlaps another background region
2 2 Background region overlaps another source region
3 4 Source region overlaps another background region
4 8 Source region overlaps another source region
5 16
6 32
7 64
8 128
9 256 Compact detection is overlaid on an extended detection
10 512
11 1024
12 2048
13 4096
14 8192
15 16384
16 32768

The confusion code for an extend (convex hull) detection is always NULL.

dither_warning_flag Boolean
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

From the Source Flags column descriptions page:

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.

edge_code coded byte
detection position, or source or background region dithered off a detector boundary (chip pixel mask) during one or more of the stacked observations (bit encoded: 1: background region dithers off detector boundary; 2:source region dithers off detector boundary; 4: detection position dithers off detector boundary)

From the Source Flags column descriptions page:

The edge code for a compact or extended (convex hull) detection is a 16-bit coded integer that has all bits set to zero if the detection's position, source region, and background region do not dither off a chip boundary (the edge of the unmasked area of the active region of the ACIS CCD or HRC microchannel plate segment, as appropriate) during the observation. Otherwise, the bits are set as follows:

Bit Value Code
1 1 Background region dithers off detector boundary
2 2 Source region dithers off detector boundary
3 4 Detection position dithers off detector boundary
4 8
5 16
6 32
7 64
8 128
9 256
10 512
11 1024
12 2048
13 4096
14 8192
15 16384
16 32768

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.

extent_code integer
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 (bit encoded: 1, 2, 4, 8, 16, 32: deconvolved compact detection extent is not consistent with a point source in the ACIS ultrasoft, soft, medium, hard, broad, or HRC wide (~0.1-10.0 keV) energy band, respectively; 256: extended detection)

From the Source Flags column descriptions page:

The extent code for a compact detection is a 16-bit coded integer that has all bits set to zero if a wavelet transform analysis of counts in the detection's source region ellipse is consistent with a point source at the 90% confidence level in all science energy bands . Otherwise, the bits are set as follows:

Bit Value Code
1 1 Deconvolved compact detection extent is not consistent with point source at the 90% confidence level in the ACIS ultrasoft energy band
2 2 Deconvolved compact detection extent is not consistent with point source at the 90% confidence level in the ACIS soft energy band
3 4 Deconvolved compact detection extent is not consistent with point source at the 90% confidence level in the ACIS medium energy band
4 8 Deconvolved compact detection extent is not consistent with point source at the 90% confidence level in the ACIS hard energy band
5 16 Deconvolved compact detection extent is not consistent with point source at the 90% confidence level in the ACIS broad energy band
6 32 Deconvolved compact detection extend is not consistent with point source at the 90% confidence level in the HRC wide energy band
7 64
8 128
9 256 Extended detection
10 512
11 1024
12 2048
13 4096
14 8192
15 16384
16 32768

The extent code for an extended (convex hull) detection is always set to 256 (Extended detection).

multi_chip_code coded byte
source position, or source or background region dithered multiple detector chips during one or more of the stacked observations (bit encoded: 1: background region dithers across 2 chips; 2: background region dithers across >2 chips; 4: source region dithers across 2 chips; 8: source region dithers across >2 chips; 16: detection position dithers across 2 chips; 32: detection position dithers across >2 chips)

From the Source Flags column descriptions page:

The multi-chip code for a compact or extended (convex hull) detection is a 16-bit coded integer that has all bits set to zero if the detection's position, source region, and background region do not dither between two or more chips (ACIS CCDs or HRC microchannel plate segment, as appropriate) during the observation. Otherwise, the bits are set as follows:

Bit Value Code
1 1 Background region dithers across two chips
2 2 Background region dithers across more than two chips
3 4 Source region dithers across two chips
4 8 Source region dithers across more than two chips
5 16 Detection position dithers across two chips
6 32 Detection position dithers across more than two chips
7 64
8 128
9 256
10 512
11 1024
12 2048
13 4096
14 8192
15 16384
16 32768

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.

pileup_flag Boolean
ACIS pile-up fraction exceeds ~10% in any stacked observations; detection properties may be affected

From the Source Flags column descriptions page:

The pileup warning flag for a compact detection is a Boolean that has a value of TRUE if the pileup fraction exceed ~10% for any contributing ACIS per-observation detections and energy bands. Otherwise, the value is FALSE.

The pileup warning flag for an extended (convex hull) detection is always NULL.

sat_src_flag Boolean
detection is saturated in all stacked observations (strong ACIS pileup); detection properties are unreliable

From the Source Flags column descriptions page:

The saturated detection flag is for a compact detection is a Boolean that has a value of TRUE if all contributing observations are ACIS observations and all per-observation detections are significantly piled-up, i.e., sat_src_flag is TRUE for all of the contributing per-observation detections. Detection properties (including the pileup warning flag) are unreliable for all ACIS energy bands. Otherwise, the value is FALSE.

sat_src_flag for an extended (convex hull) source is always NULL.

streak_src_flag Boolean
detection located on an ACIS readout streak in all stacked observations; detection properties may be affected

From the Source Flags column descriptions page:

The streak detection flag for a compact detection is a Boolean that has a value of TRUE if all contributing observations are ACIS observations and all per-observation source regions overlap a defined region enclosing an identified readout streak, i.e., streak_src_flag is TRUE for all of the contributing per-observation detections. Otherwise, the value is FALSE.

The streak source flag for an extended (convex hull) detection is TRUE if any contributing observations are ACIS observations and any per-observation detection source region overlaps a defined region enclosing an identified readout streak . Otherwise, the value is FALSE.

var_flag Boolean
detection displays flux variability within one or more of the stacked observations, or between stacked observations in one or more energy bands

From the Source Flags column descriptions page:

The variability flag is a Boolean that has a value of TRUE if variability is detected (the corresponding var_index value is ≥6) within any single observation or between any pair of observations contributing to the stacked detection, in any science energy band. Otherwise, the value is FALSE.

var_inter_hard_flag Boolean
detection hardness ratios are statistically inconsistent between two or more of the stacked observations

From the Source Flags column descriptions page:

The inter-observation variable hardness ratio flag for a compact detection is a Boolean that has a value of TRUE if 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 observation detections. Otherwise, the values is FALSE.

From the Source Variability column descriptions page:

A Boolean set to FALSE if var_inter_hard_prob is below 0.3 for all three hardness ratios, and set to TRUE otherwise.

man_add_flag Boolean
detection was manually added to the catalog via human review

From the Source Flags column descriptions page:

The manual detection addition flag for a compact or extended (convex hull) detection is a Boolean that has a value of TRUE if the stacked observation detection was manually added to the catalog by human review. Otherwise, the value is FALSE.

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 below.

man_inc_flag Boolean
detection manually included to the catalog (detection was rejected by automated criteria)

From the Source Flags column descriptions page:

The manual detection inclusion flag for a compact or extended (convex hull) detection is a Boolean that has a value of TRUE if the stacked observation detection was manually included in this catalog by human review. Otherwise, the value is FALSE.

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. See also the Manual Source/Detection Addition Flag above.

man_pos_flag Boolean
best fit detection position was manually modified via human review

From the Source Flags column descriptions page:

The manual detection position flag for a compact detection is a Boolean that has a value of TRUE if the final detection position was manually modified from the fitted position (determined by the maximum likelihood estimator [MLE]) were manually modified by human review. Otherwise, the value is FALSE.

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. Otherwise, the value is FALSE.

man_reg_flag Boolean
source region parameters (dimensions, initial guess position input to the Maximum Likelihood Estimator fit) were manually modified via human review

From the Source Flags column descriptions page:

The manual detection region parameters flag for a compact source is a Boolean that has a value of TRUE if any of the detection's 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. Otherwise, the value is FALSE.

The manual detection region parameters flag for an extended (convex hull) source is set to TRUE if the shape or position of the defining polygon was manually modified by human review. Otherwise, the value is FALSE.


Source Extent major_axis double[6] arcsec
1σ radius along the major axis of the ellipse defining the deconvolved source extent for each science energy band

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

major_axis_lolim double[6] arcsec
1σ radius along the major axis of the ellipse defining the deconvolved detection extent (68% lower confidence limit) for each science energy band

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

major_axis_hilim double[6] arcsec
1σ radius along the major axis of the ellipse defining the deconvolved detection extent (68% upper confidence limit) for each science energy band

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

minor_axis double[6] arcsec
1σ radius along the minor axis of the ellipse defining the deconvolved source extent for each science energy band

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

minor_axis_lolim double[6] arcsec
1σ radius along the minor axis of the ellipse defining the deconvolved detection extent (68% lower confidence limit) for each science energy band

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

minor_axis_hilim double[6] arcsec
1σ radius along the minor axis of the ellipse defining the deconvolved detection extent (68% upper confidence limit) for each science energy band

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

pos_angle double[6] deg
position angle (referenced from local true north) of the major axis of the ellipse defining the deconvolved source extent for each science energy band

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

pos_angle_lolim double[6] deg
position angle (referenced from local true north) of the major axis of the ellipse defining the deconvolved detection extent (68% lower confidence limit)

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

pos_angle_hilim double[6] deg
position angle (referenced from local true north) of the major axis of the ellipse defining the deconvolved detection extent (68% upper confidence limit)

From the 'Deconvolved Source Extent' section of the Source Extent and Errors column descriptions page:

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 and associated errors for the \(1\sigma\) radius along the major axis, the \(1\sigma\) radius along the minor axis, and the position angle of the major axis of a rotated elliptical Gaussian source that has been fitted to the observed source spatial event distribution deconvolved with the ray-trace local PSF at the location of that source event distribution.

Deconvolving the raw source image with the PSF produces the intrinsic shape of the source. In order to determine whether a source is extended, we first need to realize that the intrinsic size of a point source is, by definition, zero. By performing the fitting described above, srcextent estimates the raw sizes and errors of both the source and the PSF. In what follows, we derive the size and error for the intrinsic size of the source, and then we establish a criterion to flag a source as extended.

In principle, one can determine the parameters of the intrinsic source ellipse, \(\{a_{1},a_{2},\phi\}\), by solving a non-linear system of equations involving the PSF parameters, \(\{a_{1},a_{2},\psi\}\), and the measured source parameters, \(\{\sigma_{1},\sigma_{2},\delta\}\). However, because these equations are based on a crude approximation and because the input parameters are often uncertain, such an elaborate calculation seems unjustified.

A much simpler and more robust approach makes use of the identity:

\[ \sigma_{1}^{2} + \sigma_{2}^{2} = a_{1}^{2} + a_{2}^{2} + b_{1}^{2} + b_{2}^{2} \ , \]

which applies to the convolution of two elliptical Gaussians having arbitrary relative sizes and position angles. Using this identity, one can define a root-sum-square intrinsic source size:

\[ a_{\mathrm{rss}} \equiv \sqrt{a_{1}^2 + a_{2}^{2}} = \sqrt{ \max\{0,(\sigma_{1}^{2} + \sigma_{2}^{2}) - (b_{1}^{2} + b_{2}^{2}) \}} \ , \]

that depends only on the sizes of the relevant ellipses and is independent of their orientations. This expression is analogous to the well-known result for convolution of 1D Gaussians and for convolution of circular Gaussians in 2D.

Using the equation above, one can derive an analytic expression for the uncertainty in \(a_{\mathrm{rss}}\) in terms of the measurement errors associated with \(\sigma_{i}\) and \(b_{i}\). Because \(\sigma_{i}\) and \(b_{i}\) are non-negative, evaluating the right-hand side of the equation using the corresponding mean values should give a reasonable estimate of the mean value of \(a_{\mathrm{rss}}\). A Taylor series expansion of the right-hand side evaluated at the mean parameter values, therefore, yields the uncertainty:

\[ \Delta a_{\mathrm{rss}} = \frac{1}{a} \sqrt{ \sigma_{1}^{2} \left(\Delta \sigma_{1} \right)^{2} + \sigma_{2}^{2} \left(\Delta \sigma_{2} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} + b_{1}^{2} \left(\Delta b_{1} \right)^{2} } \]

where \(\left(\Delta X \right)^{2}\) represents the variance in \(X\) and where

\[ a \equiv \left\{ \begin{array}{ll} a_{\mathrm{rss}} \ , & a_{\mathrm{rss}} > 0 \ , \\ \sqrt{b_{1}^{2} + b_{2}^{2}} \ , & a_{\mathrm{rss}} = 0 \ . \end{array} \right. \]

A source is extended if its root-sum-square intrinsic size is larger than the root-sum-square error of this size. Namely, if its derived intrinsic size, that depends on the raw source and PSF sizes and errors, is larger than the fluctuations due to the uncertainty in the determination (different from zero). If \(a_{\mathrm{rss}} > f \Delta a_{\mathrm{rss}}\), then the source is extended at the \(f\sigma\) level. In CSC2, we use \(f = 5\), which implies that sources are flagged as extended if the intrinsic size is determined with a significance of \(5\sigma\).

src_area double[6] sq. arcseconds area of the deconvolved detection extent ellipse, or area of the detection polygon for extended detections for each science energy band

Aperture Photometry src_cnts_aper double[6] counts
aperture-corrected detection net counts inferred from the source region aperture for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source counts represent the combined net number of background-subtracted source counts in the modified source region (src_cnts_aper) and in the modified elliptical aperture (src_cnts_aper90), corrected by the appropriate PSF aperture fractions, for all valid source observations in the stack.

src_cnts_aper_lolim double[6] counts
aperture-corrected detection net counts inferred from the source region aperture (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source counts represent the combined net number of background-subtracted source counts in the modified source region (src_cnts_aper) and in the modified elliptical aperture (src_cnts_aper90), corrected by the appropriate PSF aperture fractions, for all valid source observations in the stack.

src_cnts_aper_hilim double[6] counts
aperture-corrected detection net counts inferred from the source region aperture (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source counts represent the combined net number of background-subtracted source counts in the modified source region (src_cnts_aper) and in the modified elliptical aperture (src_cnts_aper90), corrected by the appropriate PSF aperture fractions, for all valid source observations in the stack.

src_rate_aper double[6] counts s-1
aperture-corrected detection net count rate inferred from the source region aperture for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source count rates and associated two-sided confidence limits are defined as the average background-subtracted source count rates in the modified source region (src_rate_aper) and in the modified elliptical aperture (src_rate_aper90), corrected by the appropriate PSF aperture fractions and livetime, for all valid source observations in the stack.

src_rate_aper_lolim double[6] counts s-1
aperture-corrected detection net count rate inferred from the source region aperture (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source count rates and associated two-sided confidence limits are defined as the average background-subtracted source count rates in the modified source region (src_rate_aper) and in the modified elliptical aperture (src_rate_aper90), corrected by the appropriate PSF aperture fractions and livetime, for all valid source observations in the stack.

src_rate_aper_hilim double[6] counts s-1
aperture-corrected detection net count rate inferred from the source region aperture (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source count rates and associated two-sided confidence limits are defined as the average background-subtracted source count rates in the modified source region (src_rate_aper) and in the modified elliptical aperture (src_rate_aper90), corrected by the appropriate PSF aperture fractions and livetime, for all valid source observations in the stack.

photflux_aper double[6] photons s-1 cm-2
aperture-corrected detection net photon flux inferred from the source region aperture, calculated by counting X-ray events for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

photflux_aper_lolim double[6] photons s-1 cm-2
aperture-corrected detection net photon flux inferred from the source region aperture, calculated by counting X-ray events (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

photflux_aper_hilim double[6] photons s-1 cm-2
aperture-corrected detection net photon flux inferred from the source region aperture, calculated by counting X-ray events (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

flux_aper double[6] ergs s-1 cm-2
aperture-corrected detection net energy flux inferred from the source region aperture, calculated by counting X-ray events for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

flux_aper_lolim double[6] ergs s-1 cm-2
aperture-corrected detection net energy flux inferred from the source region aperture, calculated by counting X-ray events (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

flux_aper_hilim double[6] ergs s-1 cm-2
aperture-corrected detection net energy flux inferred from the source region aperture, calculated by counting X-ray events (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

src_cnts_aper90 double[6] counts
aperture-corrected detection net counts inferred from the PSF 90% ECF aperture for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source counts represent the combined net number of background-subtracted source counts in the modified source region (src_cnts_aper) and in the modified elliptical aperture (src_cnts_aper90), corrected by the appropriate PSF aperture fractions, for all valid source observations in the stack.

src_cnts_aper90_lolim double[6] counts
aperture-corrected detection net counts inferred from the PSF 90% ECF aperture (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source counts represent the combined net number of background-subtracted source counts in the modified source region (src_cnts_aper) and in the modified elliptical aperture (src_cnts_aper90), corrected by the appropriate PSF aperture fractions, for all valid source observations in the stack.

src_cnts_aper90_hilim double[6] counts
aperture-corrected detection net counts inferred from the PSF 90% ECF aperture (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source counts represent the combined net number of background-subtracted source counts in the modified source region (src_cnts_aper) and in the modified elliptical aperture (src_cnts_aper90), corrected by the appropriate PSF aperture fractions, for all valid source observations in the stack.

src_rate_aper90 double[6] counts s-1
aperture-corrected detection net count rate inferred from the PSF 90% ECF aperture for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source count rates and associated two-sided confidence limits are defined as the average background-subtracted source count rates in the modified source region (src_rate_aper) and in the modified elliptical aperture (src_rate_aper90), corrected by the appropriate PSF aperture fractions and livetime, for all valid source observations in the stack.

src_rate_aper90_lolim double[6] counts s-1
aperture-corrected detection net count rate inferred from the PSF 90% ECF aperture (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source count rates and associated two-sided confidence limits are defined as the average background-subtracted source count rates in the modified source region (src_rate_aper) and in the modified elliptical aperture (src_rate_aper90), corrected by the appropriate PSF aperture fractions and livetime, for all valid source observations in the stack.

src_rate_aper90_hilim double[6] counts s-1
aperture-corrected detection net count rate inferred from the PSF 90% ECF aperture (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source count rates and associated two-sided confidence limits are defined as the average background-subtracted source count rates in the modified source region (src_rate_aper) and in the modified elliptical aperture (src_rate_aper90), corrected by the appropriate PSF aperture fractions and livetime, for all valid source observations in the stack.

photflux_aper90 double[6] photons s-1 cm-2
aperture-corrected detection net photon flux inferred from the PSF 90% ECF aperture, calculated by counting X-ray events for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

photflux_aper90_lolim double[6] photons s-1 cm-2
aperture-corrected detection net photon flux inferred from the PSF 90% ECF aperture, calculated by counting X-ray events (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

photflux_aper90_hilim double[6] photons s-1 cm-2
aperture-corrected detection net photon flux inferred from the PSF 90% ECF aperture, calculated by counting X-ray events (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

flux_aper90 double[6] ergs s-1 cm-2
aperture-corrected detection net energy flux inferred from the PSF 90% ECF aperture, calculated by counting X-ray events for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

flux_aper90_lolim double[6] ergs s-1 cm-2
aperture-corrected detection net energy flux inferred from the PSF 90% ECF aperture, calculated by counting X-ray events (68% lower confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.

flux_aper90_hilim double[6] ergs s-1 cm-2
aperture-corrected detection net energy flux inferred from the PSF 90% ECF aperture, calculated by counting X-ray events (68% upper confidence limit) for each science energy band

From the 'Aperture Photometry Fluxes' section of the Source Fluxes column descriptions page:

Aperture photometry quantities are derived from counts in source regions or elliptical apertures, with background estimated from counts in surrounding background regions. Corrections are made for PSF aperture fractions, livetime, and exposure. In the case of energy fluxes, the conversion from 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. For all aperture photometry quantities, a Bayesian statistical analysis is performed to determine background-marginalized posterior probability distribution for the flux quantity, and the mode and 68% percentiles of the distribution are reported as the flux value and confidence limits.

Fluxes are determined for each per-observation detection, for each stack, and for the master source. At the stack level, aperture data from all valid source observations in the stack are combined. At the master source level, a Bayesian Blocks analysis is performed to determine the sets of source observations consistent with a constant source flux. Aperture data from the set with the largest total exposure are then combined to determine master source 'best estimate' fluxes and confidence limits. In addition, aperture data from all source observations in which the master source was detected or in the field of view are combined to determine master source average fluxes and confidence limits.

The aperture source photon and energy fluxes and associated two-sided confidence limits represent the average background-subtracted fluxes in the modified source region (photflux_aper, flux_aper) and in the modified elliptical aperture (photflux_aper90, flux_aper90), corrected by the appropriate PSF aperture fractions, livetime, and exposure for all valid observations in the stack. The conversion from 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.


Source Aperture ra_aper double deg
center of the source region and background region apertures, ICRS right ascension

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

dec_aper double deg
center of the source region and background region apertures, ICRS declination

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

mjr_axis_aper double arcsec
semi-major axis of the elliptical source region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

mnr_axis_aper double arcsec
semi-minor axis of the elliptical source region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

pos_angle_aper double deg
position angle (referenced from local true north) of the semi-major axis of the elliptical source region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

mjr_axis1_aperbkg double arcsec
semi-major axis of the inner ellipse of the annular background region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

mnr_axis1_aperbkg double arcsec
semi-minor axis of the inner ellipse of the annular background region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

mjr_axis2_aperbkg double arcsec
semi-major axis of the outer ellipse of the annular background region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

mnr_axis2_aperbkg double arcsec
semi-minor axis of the outer ellipse of the annular background region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

pos_angle_aperbkg double deg
position angle (referenced from local true north) of the semi-major axes of the annular background region aperture

From the 'Source Region' section of the Source Extent and Errors column descriptions page:

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. The parameter values that define the source region and background region for each source are the ICRS right ascension and signed ICRS declination of the center of the source region and background region; the semi-major and semi-minor axes of the source region ellipse and of the inner and outer annuli of the background region ellipse; and the position angles of the semi-major axes defining the source and background region ellipses.

phot_nsrcs integer[6] number of detections fit simultaneously to compute aperture photometry quantities

Hardness Ratios hard_hm double ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio
hard_hm_lolim double ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio (68% lower confidence limit)
hard_hm_hilim double ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio (68% upper confidence limit)
var_inter_hard_prob_hm double
inter-stacked-observation ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio variability probability

From the Source Variability column descriptions page:

The inter-observation spectral variability probability (var_inter_hard_prob) is a value that 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 this probability is identical to that of the inter-observation source variability (var_inter_prob), and also utilizes the same hypothesis rejection test, but based on the probability distributions (PDFs) for the hardness ratios, rather than the probability distributions for the fluxes. The definition of the hardness ratio PDFs can be found in the memo, and also in the hardness ratios columns page. High values of var_inter_hard_prob indicate that the source is spectrally variable in the corresponding combination of bands.

var_inter_hard_sigma_hm double
inter-stacked-observation ACIS hard (2.0-7.0 keV) - medium (1.2-2.0 keV) energy band hardness ratio variability standard deviation

From the Source Variability column descriptions page:

Similarly to var_inter_sigma, the inter-observation hardness ratio variability parameter (var_inter_hard_sigma) is the absolute value of the difference between the error weighted mean of the source region hardness ratio 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:

\[ \left| hard_{\left\langle band_{1}band_{2}\right\rangle}^{\mathrm{max}} - hard_{\left\langle band_{1}band_{2}\right\rangle}^{\mathrm{i,max}} \right| \]

Of all contributing observations, the observation that yields the highest value for this equation, is used in computing this value, which is recorded in var_inter_hard_sigma. Intuitively, this quantity can be interpreted as the variance of the individual observation hardness ratios.

hard_hs double ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio
hard_hs_lolim double ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% lower confidence limit)
hard_hs_hilim double ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% upper confidence limit)
var_inter_hard_prob_hs double
inter-stacked-observation ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability probability

From the Source Variability column descriptions page:

The inter-observation spectral variability probability (var_inter_hard_prob) is a value that 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 this probability is identical to that of the inter-observation source variability (var_inter_prob), and also utilizes the same hypothesis rejection test, but based on the probability distributions (PDFs) for the hardness ratios, rather than the probability distributions for the fluxes. The definition of the hardness ratio PDFs can be found in the memo, and also in the hardness ratios columns page. High values of var_inter_hard_prob indicate that the source is spectrally variable in the corresponding combination of bands.

var_inter_hard_sigma_hs double
inter-stacked-observation ACIS hard (2.0-7.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability standard deviation

From the Source Variability column descriptions page:

Similarly to var_inter_sigma, the inter-observation hardness ratio variability parameter (var_inter_hard_sigma) is the absolute value of the difference between the error weighted mean of the source region hardness ratio 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:

\[ \left| hard_{\left\langle band_{1}band_{2}\right\rangle}^{\mathrm{max}} - hard_{\left\langle band_{1}band_{2}\right\rangle}^{\mathrm{i,max}} \right| \]

Of all contributing observations, the observation that yields the highest value for this equation, is used in computing this value, which is recorded in var_inter_hard_sigma. Intuitively, this quantity can be interpreted as the variance of the individual observation hardness ratios.

hard_ms double ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio
hard_ms_lolim double ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio (68% lower confidence limit)
hard_ms_hilim double ACIS medium (1.2-2.0 keV)- soft (0.5-1.2 keV) energy band hardness ratio (68% upper confidence limit)
var_inter_hard_prob_ms double
inter-stacked-observation ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability probability

From the Source Variability column descriptions page:

The inter-observation spectral variability probability (var_inter_hard_prob) is a value that 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 this probability is identical to that of the inter-observation source variability (var_inter_prob), and also utilizes the same hypothesis rejection test, but based on the probability distributions (PDFs) for the hardness ratios, rather than the probability distributions for the fluxes. The definition of the hardness ratio PDFs can be found in the memo, and also in the hardness ratios columns page. High values of var_inter_hard_prob indicate that the source is spectrally variable in the corresponding combination of bands.

var_inter_hard_sigma_ms double
inter-stacked-observation ACIS medium (1.2-2.0 keV) - soft (0.5-1.2 keV) energy band hardness ratio variability standard deviation

From the Source Variability column descriptions page:

Similarly to var_inter_sigma, the inter-observation hardness ratio variability parameter (var_inter_hard_sigma) is the absolute value of the difference between the error weighted mean of the source region hardness ratio 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:

\[ \left| hard_{\left\langle band_{1}band_{2}\right\rangle}^{\mathrm{max}} - hard_{\left\langle band_{1}band_{2}\right\rangle}^{\mathrm{i,max}} \right| \]

Of all contributing observations, the observation that yields the highest value for this equation, is used in computing this value, which is recorded in var_inter_hard_sigma. Intuitively, this quantity can be interpreted as the variance of the individual observation hardness ratios.


Temporal Variability var_intra_index integer[6]
intra-observation Gregory-Loredo variability index in the range [0, 10]: indicates whether the source region photon flux is constant within an observation (highest value across all stacked observations) for each science energy band

The intra-observation variability index (var_intra_index) represents the highest value of the variability indices (var_index) calculated for each of the contributing observations.

var_intra_prob double[6]
intra-observation Gregory-Loredo variability probability (highest value across all stacked observations for each science energy band

The Gregory-Loredo, Kolmogorov-Smirnov (K-S) test, and Kuiper's test intra-observation variability probabilities represent the highest values of the variability probabilities (var_prob, ks_prob, kp_prob) calculated for each of the contributing observations (i.e., the highest level of variability among the observations contributing to the master source entry).

ks_intra_prob double[6]
intra-observation Kolmogorov-Smirnov test variability probability (highest value across all observations) for each science energy band

The Gregory-Loredo, Kolmogorov-Smirnov (K-S) test, and Kuiper's test intra-observation variability probabilities represent the highest values of the variability probabilities (var_prob, ks_prob, kp_prob) calculated for each of the contributing observations (i.e., the highest level of variability among the observations contributing to the master source entry).

kp_intra_prob double[6]
intra-observation Kuiper's test variability probability (highest value across all stacked observations) for each science energy band

The Gregory-Loredo, Kolmogorov-Smirnov (K-S) test, and Kuiper's test intra-observation variability probabilities represent the highest values of the variability probabilities (var_prob, ks_prob, kp_prob) calculated for each of the contributing observations (i.e., the highest level of variability among the observations contributing to the master source entry).

var_inter_index integer[6]
inter-stacked-observation variability index in the range [0, 10]: indicates whether the source region photon flux is constant between observations for each science energy band

From the Source Variability column descriptions page:

The inter-observation variability index (var_inter_index) is an integer value in the range \([0,8]\) that is derived according to the estimated value of the quantity \(D/(N-1)\) defined above. 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. Below we tabulate the association between the value of \(D/(N-1)\) and inter-observation variability index.

Variability Index \(\frac{D}{N-1}\)
2 observations >2 observations
0 < 0.4 < 0.8
3 ≥ 0.4 < 0.7 ≥ 0.8 < 1.0
4 ≥ 0.7 < 1.0 ≥ 1.0 < 1.15
5 ≥ 1.0 < 2.7 ≥ 1.15 < 2.1
6 ≥ 2.7 < 7.0 ≥ 2.1 < 3.8
7 ≥ 7.0 < 12.0 ≥ 3.8 < 5.5
8 ≥ 12.0 ≥ 5.5
var_inter_prob double[6]
inter-stacked observation variability probability, calculated from the χ2 distribution of the photon fluxes of the individual observations for each science energy band

The inter-observation variability probability (var_inter_prob) is a value that 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. Given the \(N\) individual Bayesian probability distribution of the aperture fluxes for the same source in \(N\) different observations (their means and standard deviations), we estimate for each band the maximum likelihood \(\mathcal{L}_{1}^{\mathrm{max}}\) and the corresponding maximizing arguments \(F_{\left\langle band \right\rangle}^{i,\mathrm{max}}\), of the observed fluxes assuming a different flux for each observation, as well as the maximum likelihood \(\mathcal{L}_{2}^{\mathrm{max}}\) and the corresponding maximizing argument \(F_{\left\langle band \right\rangle}^{\mathrm{max}}\) of the observed fluxes assuming a single flux (the latter is the null hypothesis of no variability). As per Wilks' theorem, the quantity:

\[ D \equiv 2 \left( \log{\mathcal{L}_{1}^{\mathrm{max}}} - \log{\mathcal{L}_{2}^{\mathrm{max}}} \right) \]

follows \(\chi^{2}\) distribution with \(N-1\) degrees of freedom, under the null hypothesis. Therefore, the null hypothesis (non-variability) is rejected with a probability proportional to the cumulative distribution of the \(\chi^{2}\) statistic for values smaller than the estimated \(D\). The quantity var_inter_prob represents this cumulative probability, and therefore gives the probability that the source is variable.

The reason for this careful definition is that the probabilities for intra-observation and inter-observation variability are, by necessity, of a different nature. Whereas one can say with reasonable certainty whether a source was variable during an observation covering a contiguous time interval, when comparing measured fluxes from different observations one knows nothing about the source's behavior during the intervening interval(s). Consequently, when the inter-observation variability probability is high (e.g., var_inter_prob > 0.7), one can confidently state that the source is variable on longer time scales, but when the probability is low, all one can say is that the observations are consistent with a constant flux.

var_inter_sigma double[6] photons s-1 cm-2
inter-stacked-observation flux variability standard deviation; the spread of the individual observation photon fluxes about the error weighted mean for each science energy band

From the Source Variability column descriptions page:

The inter-observation flux variability (var_inter_sigma) 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 \(\left( F_{\left\langle band \right\rangle}^{\mathrm{max}} \right)\), and the mean of the source region photon flux density PDF for the individual observation that maximizes the absolute value of the difference \(\left( F_{\left\langle band \right\rangle}^{i,\mathrm{max}} \right)\):

\[ \left| F_{\left\langle band \right\rangle}^{\mathrm{max}} - F_{\left\langle band \right\rangle}^{i,\mathrm{max}} \right| \]

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.


Timing Information livetime double s effective stacked observation exposure time, after applying the good time intervals and deadtime correction factor; vignetting and dead area corrections are NOT applied