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XMMATLAS - XMM-Newton Survey Catalog in the Herschel-ATLAS Field |
HEASARC Archive |
Overview
Wide area X-ray and far-infrared surveys are a fundamental tool to investigate the link between AGN growth and star formation, especially in the low-redshift universe (z < 1). The Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) has covered 550 deg2 in five far-infrared and sub-mm bands, 16 deg2 of which have been presented in the Science Demonstration Phase (SDP) catalogue. The reference paper cited below introduces the XMM-Newton observations in the H-ATLAS SDP area, covering 7.1 deg2 with flux limits of 2 x 10-15, 6 x 10-15, and 9 x 10-15 erg/s/cm2 in the 0.5-2, 0.5-8 and 2-8keV bands, respectively.The paper presents the source detection techniques and the "main" catalog, which includes 1700, 1582 and 814 sources detected by EMLDetect in the 0.5-8, 0.5-2 and 2-8keV bands, respectively; the number of unique sources is 1816. The authors extract spectra and derive fluxes from power-law fits for 398 sources with more than 40 counts in the 0.5-8 keV band. They compare the best-fit fluxes with those in the catalog, which were obtained assuming a common photon index Gamma of 1.7; the authors find no bulk difference between the fluxes, and a moderate dispersion s of 0.33 dex. Using wherever possible the fluxes from the spectral fits, the authors derive the 2-10 keV Log N-Log S distribution, which is consistent with a Euclidean distribution. Finally, they release the computer code for the tools which they developed for this project.
Sources were detected with a two-stage process. With the first pass at low significance, the authors got a list of candidate detections; and on the second pass they raised the significance threshold and derived accurate source parameters. Between the two passes, and because the second pass needs an input catalog, they identified the sources detected in more than one band. In the first pass, the SAS wavelet detection program ewavelet was run separately on each of the 0.5-2, 2-8 and 0.5-8 keV images of the entire mosaic, with a significance threshold of 4 sigma and the default wavelet scales (minimum 2 pixels, maximum 8 pixels, with a pixel size of 4). All parameters in this catalog which were derived from ewavelet have been given a prefix of 'wav' in this HEASARC representation so as to distinguish them from the parameters derived using EMLDetect. In the second pass, the authors used the SAS EMLDetect program to validate the detections, refine the coordinates and obtain maximum-likelihood estimates of the source counts, count rates and fluxes. The EMLDetect minimum likelihood was set at L = 4.6, as in Ranalli et al. (2013, A&A, 555, A42), which corresponds to a false-detection probability of 1.01 x 10-2. Together with the 4-sigma threshold for ewavelet, for the final catalog this yields a joint significance between 4 sigma and 5 sigma, but which cannot be further constrained without simulations.
This table contains the X-ray sources which were detected in the 7.1 deg2 XMM-Newton observations of the H-ATLAS field. The 1816 sources which were detected by both programs were presented in the main table in the reference paper (and are included in this HEASARC table where they are indicated by a value of the source_sample parameter of 'main'), while the 234 sources which were only detected by ewavelet were presented in the supplementary table in the reference paper (and are included in this HEASARC table where they are indicated by a value of the source_sample parameter of 'supp'). The same parameters were present in both the main and supplementary tables in the reference paper, but those parameters which came from EMLDetect are empty for the sources in the supplementary table. The parameters obtained using ewavelet (those parameters with the 'wav' prefix in their names) containing the source properties (counts, count rates, fluxes, exposure times, background, wavelet detection scale and source extent), while reported in this table for all sources, are actually only interesting for supplementary sources, according to the authors.
Catalog Bibcode
2015A&A...577A.121RReferences
The XMM-Newton survey in the H-ATLAS field.
Ranalli P., Georgantopoulos I., Corral A., Koutoulidis L., Rovilos M.,
Carrera F.J., Akylas A., Del Moro A., Georgakakis A., Gilli R., Vignali C.
<Astron. Astrophys. 577, A121 (2015)>
=2015A&A...577A.121R (SIMBAD/NED BibCode)
Provenance
This table was created by the HEASARC in May 2015 based on the union of CDS Catalog J/A+A/577/A121 files main.dat (which contain 1816 sources detected by both detection algorithms) and suppl.dat (which contains 234 'supplementary' sources detected only by the wavelet detection algorithm ewavelet). It thus contains a total of 2050 sources.HEASARC Implementation
The HEASARC added a parameter called "source_sample" to identify the original table from which the entry was taken. See the Overview and Provenance sections for more details.Parameters
Name
The X-ray J2000.0 position-based source designation, viz., 'XMMATLAS
JHHMMSS.s+DDMMSS.s', where the prefix stands for XMM-Newton source in the
Herschel-Astrophysical Terahertz Large Area Survey.
Source_Number
A unique sequential identification number for each source in the catalog.
This is the same as the fb_source_number for those sources which were
detected in the 0.5-8.0 keV band and is in the range from 1 to 1661. For
sources detected in the 0.5-2.0 keV band, it is the same as the
sb_source_number and is in the range from 10001 to 11524, while for sources
detected in the 2.0-8.0 keV band, it is the same as the hb_source_number and
is in the range from 20001 to 20630.
FB_Source_Number
A unique source number for the 0.5-8 keV source detection in the range from 1
to 1661.
SB_Source_Number
A unique source number for the 0.5-2 keV source detection in the range from
10001 to 11524.
HB_Source_Number
A unique source number for the 2-8 keV source detection in the range from
20001 to 20630.
RA
The Right Ascension of the X-ray source in the selected equinox. This was
given in J2000.0 decimal degrees to a precision of 10-5 degrees (0.036
arcseconds) in the original table. The position of the source given here is
that derived from running EMLDetect in the 0.5-8 keV band, if available, else
from running EMLDetect in the 0.5-2 keV band, if available, else from running
EMLDetect in the 2-8 keV band. This parameter and the corresponding 'dec'
parameter have been corrected for astrometry and registered to the SDSS-DR7
QSO reference frame (Schneider et al. 2010, AJ, 139, 2360). All other
coordinate pairs are not registered and may present a minimal, residual
shift.
Dec
The Declination of the X-ray source in the selected equinox. This was given
in J2000.0 decimal degrees to a precision of 10-5 degrees (0.036
arcseconds) in the original table. The position of the source given here is
that derived from running EMLDetect in the 0.5-8 keV band, if available, else
from running EMLDetect in the 0.5-2 keV band, if available, else from running
EMLDetect in the 2-8 keV band. This parameter and the corresponding 'ra'
parameter have been corrected for astrometry and registered to the SDSS-DR7
QSO reference frame (Schneider et al. 2010, AJ, 139, 2360). All other
coordinate pairs are not registered and may present a minimal, residual
shift.
LII
The Galactic Longitude of the X-ray source (based on the 'ra' and 'dec'
parameters).
BII
The Galactic Latitude of the X-ray source (based on the 'ra' and 'dec'
parameters).
Error_Radius
The 1-sigma uncertainty in the position of the X-ray source given in the ra
and dec parameters, in arcseconds. This was obtained by dividing the
EMLDetect parameter RADec_ERR by sqrt(2). The RADec_ERR from EMLDetect is
computed as sqrt(RA_ERR2 + Dec_ERR2). However, when two normalized
one-dimensional Gaussians of sigma s are combined, the corresponding
normalized bi-dimensional Gaussian also has a sigma of s, not sqrt(2) x s,
which is what one would get with the expression above. Therefore, the authors
divided the EMLDetect value by sqrt(2).
Wav_RA
The merged Right Ascension of the X-ray source in the selected equinox that
was obtained from ewavelet. This was given in J2000.0 decimal degrees to a
precision of 10-5 degrees (0.036 arcseconds) in the original table.
Wav_Dec
The merged Declination of the X-ray source in the selected equinox that was
obtained from ewavelet. This was given in J2000.0 decimal degrees to a
precision of 10-5 degrees (0.036 arcseconds) in the original table.
Wav_Error_Radius
The 1-sigma uncertainty in the merged position of the X-ray source that was
obtained from ewavelet and is given in the wav_ra and wav_dec parameters, in
arcseconds.
Wav_FB_RA
The Right Ascension of the X-ray source in the selected equinox that was
obtained from ewavelet in the full 0.5-8 keV band. This was given in J2000.0
decimal degrees to a precision of 10-5 degrees (0.036 arcseconds) in the
original table.
Wav_FB_Dec
The Declination of the X-ray source in the selected equinox that was obtained
from ewavelet in the full 0.5-8 keV band. This was given in J2000.0 decimal
degrees to a precision of 10-5 degrees (0.036 arcseconds) in the original
table.
Wav_SB_RA
The Right Ascension of the X-ray source in the selected equinox that was
obtained from ewavelet in the soft 0.5-2 keV band. This was given in J2000.0
decimal degrees to a precision of 10-5 degrees (0.036 arcseconds) in the
original table.
Wav_SB_Dec
The Declination of the X-ray source in the selected equinox that was obtained
from ewavelet in the soft 0.5-2 keV band. This was given in J2000.0 decimal
degrees to a precision of 10-5 degrees (0.036 arcseconds) in the original
table.
Wav_HB_RA
The Right Ascension of the X-ray source in the selected equinox that was
obtained from ewavelet in the hard 2-8 keV band. This was given in J2000.0
decimal degrees to a precision of 10-5 degrees (0.036 arcseconds) in the
original table.
Wav_HB_Dec
The Declination of the X-ray source in the selected equinox that was obtained
from ewavelet in the hard 2-8 keV band. This was given in J2000.0 decimal
degrees to a precision of 10-5 degrees (0.036 arcseconds) in the original
table.
FB_RA
The Right Ascension of the X-ray source in the selected equinox that was
obtained from EMLDetect in the full 0.5-8 keV band. This was given in J2000.0
decimal degrees to a precision of 10-5 degrees (0.036 arcseconds) in the
original table.
FB_Dec
The Declination of the X-ray source in the selected equinox that was obtained
from EMLDetect in the full 0.5-8 keV band. This was given in J2000.0 decimal
degrees to a precision of 10-5 degrees (0.036 arcseconds) in the original
table.
SB_RA
The Right Ascension of the X-ray source in the selected equinox that was
obtained from EMLDetect in the soft 0.5-2 keV band. This was given in J2000.0
decimal degrees to a precision of 10-5 degrees (0.036 arcseconds) in the
original table.
SB_Dec
The Declination of the X-ray source in the selected equinox that was obtained
from EMLDetect in the soft 0.5-2 keV band. This was given in J2000.0 decimal
degrees to a precision of 10-5 degrees (0.036 arcseconds) in the original
table.
HB_RA
The Right Ascension of the X-ray source in the selected equinox that was
obtained from EMLDetect in the hard 2-8 keV band. This was given in J2000.0
decimal degrees to a precision of 10-5 degrees (0.036 arcseconds) in the
original table.
HB_Dec
The Declination of the X-ray source in the selected equinox that was obtained
from EMLDetect in the hard 2-8 keV band. This was given in J2000.0 decimal
degrees to a precision of 10-5 degrees (0.036 arcseconds) in the original
table.
Wav_FB_SB_Assoc_Reliab
The association reliability between the 0.5-8 keV and the 0.5-2 keV source
detections. Sources detected in more than one band were identified with the
likelihood ratio (LR) technique. Given a distance r between two candidate
counterparts, normalized by the uncertainty on the position, LR(r) is defined
as the ratio between the probability of having a real counterpart at r over
the probability of having a spurious counterpart at r (Pineau et al. 2011,
A&A, 527, A126). Similarly, the association reliability is defined as the
probability P(Htrue|r) of the association being true (Htrue) conditioned on r
(the relationship between LR and reliability is explained in Pineau et al.
2011, Eq. (11) and Appendix C).
Wav_FB_HB_Assoc_Reliab
The association reliability between the 0.5-8 keV and the 2-8 keV source
detections. Sources detected in more than one band were identified with the
likelihood ratio (LR) technique. Given a distance r between two candidate
counterparts, normalized by the uncertainty on the position, LR(r) is defined
as the ratio between the probability of having a real counterpart at r over
the probability of having a spurious counterpart at r (Pineau et al. 2011,
A&A, 527, A126). Similarly, the association reliability is defined as the
probability P(Htrue|r) of the association being true (Htrue) conditioned on r
(the relationship between LR and reliability is explained in Pineau et al.
2011, Eq. (11) and Appendix C).
FB_Counts
The sum of the net source counts from MOS1+MOS2+PN in the 0.5-8 keV band, as
derived from EMLDetect.
SB_Counts
The sum of the net source counts from MOS1+MOS2+PN in the 0.5-2 keV band, as
derived from EMLDetect.
HB_Counts
The sum of the net source counts from MOS1+MOS2+PN in the 2-8 keV band, as
derived from EMLDetect.
FB_Counts_Error
The 1-sigma uncertainty in the sum of the net source counts from MOS1+MOS2+PN
in the 0.5-8 keV band, as derived from EMLDetect.
SB_Counts_Error
The 1-sigma uncertainty in the sum of the net source counts from MOS1+MOS2+PN
in the 0.5-2 keV band, as derived from EMLDetect.
HB_Counts_Error
The 1-sigma uncertainty in the sum of the net source counts from MOS1+MOS2+PN
in the 2-8 keV band, as derived from EMLDetect.
FB_Count_Rate
The net count rate of the X-ray source in the 0.5-8 keV band, averaged over
the three XMM-Newton cameras, in count s-1, as derived from EMLDetect.
SB_Count_Rate
The net count rate of the X-ray source in the 0.5-2 keV band, averaged over
the three XMM-Newton cameras, in count s-1, as derived from EMLDetect.
HB_Count_Rate
The net count rate of the X-ray source in the 2-8 keV band, averaged over the
three XMM-Newton cameras, in count s-1, as derived from EMLDetect.
FB_Exposure
The exposure time at the location of the source in the 0.5-8 keV band, summed
over the three XMM-Newton cameras, in seconds.
SB_Exposure
The exposure time at the location of the source in the 0.5-2 keV band, summed
over the three XMM-Newton cameras, in seconds.
HB_Exposure
The exposure time at the location of the source in the 2-8 keV band, summed
over the three XMM-Newton cameras, in seconds.
FB_Bck_SB
The background surface brightness in the 0.5-8 keV band, in counts
arcsec-2, and summed over the three XMM-Newton cameras, as derived from
EMLDetect.
SB_Bck_SB
The background surface brightness in the 0.5-2 keV band, in counts
arcsec-2, and summed over the three XMM-Newton cameras, as derived from
EMLDetect.
HB_Bck_SB
The background surface brightness in the 2-8 keV band, in counts arcsec-2,
and summed over the three XMM-Newton cameras, as derived from EMLDetect.
FB_Flux
The flux of the X-ray source in the 0.5-8 keV band averaged over the three
XMM-Newton cameras, in erg s-1 cm-2^. The authors derived the count rate to
flux conversion factors CF assuming a power-law spectrum with a photon index
Gamma of 1.7 and a Galactic absorption of NH = 2.3 x 1020 cm-2, and by
weighting the responses of the MOS1, MOS2, and PN cameras; the values of CF
are 5.83 x 10-12, 3.25 x 10-12, and 1.17 x 10-11 erg cm-2 count-1,
for the 0.5-8, 0.5-2 and 2-8 keV bands, respectively.
SB_Flux
The flux of the X-ray source in the 0.5-2 keV band averaged over the three
XMM-Newton cameras, in erg s-1 cm-2^. The authors derived the count rate to
flux conversion factors CF assuming a power-law spectrum with a photon index
Gamma of 1.7 and a Galactic absorption of NH = 2.3 x 1020 cm-2, and by
weighting the responses of the MOS1, MOS2, and PN cameras; the values of CF
are 5.83 x 10-12, 3.25 x 10-12, and 1.17 x 10-11 erg cm-2 count-1,
for the 0.5-8, 0.5-2 and 2-8 keV bands, respectively.
HB_Flux
The flux of the X-ray source in the 2-8 keV band averaged over the three
XMM-Newton cameras, in erg s-1 cm-2^. The authors derived the count rate to
flux conversion factors CF assuming a power-law spectrum with a photon index
Gamma of 1.7 and a Galactic absorption of NH = 2.3 x 1020 cm-2, and by
weighting the responses of the MOS1, MOS2, and PN cameras; the values of CF
are 5.83 x 10-12, 3.25 x 10-12, and 1.17 x 10-11 erg cm-2 count-1,
for the 0.5-8, 0.5-2 and 2-8 keV bands, respectively.
FB_Flux_Error
The 1-sigma uncertainty in the flux of the X-ray source in the 0.5-8 keV band
averaged over the three XMM-Newton cameras, in erg s-1 cm-2^.
SB_Flux_Error
The 1-sigma uncertainty in the flux of the X-ray source in the 0.5-2 keV band
averaged over the three XMM-Newton cameras, in erg s-1 cm-2^.
HB_Flux_Error
The 1-sigma uncertainty in the flux of the X-ray source in the 2-8 keV band
averaged over the three XMM-Newton cameras, in erg s-1 cm-2^.
FB_Detect_Likelihood
The EMLDetect detection likelihood of the X-ray source in the 0.5-8 keV band.
SB_Detect_Likelihood
The EMLDetect detection likelihood of the X-ray source in the 0.5-2 keV band.
HB_Detect_Likelihood
The EMLDetect detection likelihood of the X-ray source in the 2-8 keV band.
FB_Extent
The EMLDetect X-ray source extent in the 0.5-8 keV band. This is the sigma of
a Gaussian model fit to the source, in pixels, where 1 pixel = 4 arcseconds.
None of the X-ray sources were found to be extended in the 2-8 keV band, so
there is no equivalent hb_extent parameter.
SB_Extent
The EMLDetect X-ray source extent in the 0.5-2 keV band. This is the sigma of
a Gaussian model fit to the source, in pixels, where 1 pixel = 4 arcseconds.
None of the X-ray sources were found to be extended in the 2-8 keV band, so
there is no equivalent hb_extent parameter.
FB_Extent_Error
The 1-sigma uncertainty in the EMLDetect X-ray source extent in the 0.5-8 keV
band, in terms of 4" pixels.
SB_Extent_Error
The 1-sigma uncertainty in the EMLDetect X-ray source extent in the 0.5-2 keV
band, in terms of 4" pixels.
FB_Extent_Likelihood
The EMLDetect likelihood of the X-ray source being extended, in the 0.5-8 keV
band. None of the X-ray sources were found to be extended in the 2-8 keV
band, so there is no equivalent hb_extent_likelihood parameter.
SB_Extent_Likelihood
The EMLDetect likelihood of the X-ray source being extended, in the 0.5-2 keV
band. None of the X-ray sources were found to be extended in the 2-8 keV
band, so there is no equivalent hb_extent_likelihood parameter.
Hardness_Ratio
The hardness ratio, HR, of the X-ray source as computed from S = sb_counts
and H = hb_counts, where HR = (H - S)/(H + S).
Hardness_Ratio_Error
The 1-sigma uncertainty in the hardness ratio, HR, of the X-ray source. This
was calculated using equation (1) in Section 4 of the reference paper.
Wav_FB_Counts
The net X-ray source counts from ewavelet in the 0.5-8 keV band summed over
MOS1+MOS2+PN.
Wav_SB_Counts
The net X-ray source counts from ewavelet in the 0.5-2 keV
band summed over MOS1+MOS2+PN.
Wav_HB_Counts
The net X-ray source counts from ewavelet in the 2-8 keV band summed over
MOS1+MOS2+PN.
Wav_FB_Counts_Error
The 1-sigma uncertainty in the net X-ray source counts from ewavelet in the
0.5-8 keV band summed over MOS1+MOS2+PN.
Wav_SB_Counts_Error
The 1-sigma uncertainty in the net X-ray source counts from ewavelet in the
0.5-2 keV band summed over MOS1+MOS2+PN.
Wav_HB_Counts_Error
The 1-sigma uncertainty in the net X-ray source counts from ewavelet in the
2-8 keV band summed over MOS1+MOS2+PN.
Wav_FB_Count_Rate
The net count rates of the X-ray source from ewavelet in the 0.5-8 keV band
averaged over the three cameras.
Wav_SB_Count_Rate
The net count rates of the X-ray source from ewavelet in the 0.5-2 keV band
averaged over the three cameras.
Wav_HB_Count_Rate
The net count rates of the X-ray source from ewavelet in the 2-8 keV band
averaged over the three cameras.
Wav_FB_Exposure
The exposure time at the location of the source from ewavelet in the 0.5-8
keV band, in seconds, and summed over the three cameras.
Wav_SB_Exposure
The exposure time at the location of the source from ewavelet in the 0.5-2
keV band, in seconds, and summed over the three cameras.
Wav_HB_Exposure
The exposure time at the location of the source from ewavelet in the 2-8 keV
band, in seconds, and summed over the three cameras.
Wav_FB_Bck_SB
The background surface brightness in the 0.5-8 keV band, in counts
arcsec-2, and summed over the three XMM-Newton cameras, as derived from
ewavelet.
Wav_SB_Bck_SB
The background surface brightness in the 0.5-2 keV band, in counts
arcsec-2, and summed over the three XMM-Newton cameras, as derived from
ewavelet.
Wav_HB_Bck_SB
The background surface brightness in the 2-8 keV band, in counts arcsec-2,
and summed over the three XMM-Newton cameras, as derived from ewavelet.
Wav_FB_Flux
The flux of the X-ray source in the 0.5-8 keV band averaged over the three
XMM-Newton cameras, in erg s-1 cm-2^, as derived from ewavelet. The authors
derived the count rate to flux conversion factors CF assuming a power-law
spectrum with a photon index Gamma of 1.7 and a Galactic absorption of NH =
2.3 x 1020 cm-2, and by weighting the responses of the MOS1, MOS2, and PN
cameras; the values of CF are 5.83 x 10-12, 3.25 x 10-12, and 1.17 x
10-11 erg cm-2 count-1, for the 0.5-8, 0.5-2 and 2-8 keV bands,
respectively.
Wav_SB_Flux
The flux of the X-ray source in the 0.5-2 keV band averaged over the three
XMM-Newton cameras, in erg s-1 cm-2^, as derived from ewavelet. The authors
derived the count rate to flux conversion factors CF assuming a power-law
spectrum with a photon index Gamma of 1.7 and a Galactic absorption of NH =
2.3 x 1020 cm-2, and by weighting the responses of the MOS1, MOS2, and PN
cameras; the values of CF are 5.83 x 10-12, 3.25 x 10-12, and 1.17 x
10-11 erg cm-2 count-1, for the 0.5-8, 0.5-2 and 2-8 keV bands,
respectively.
Wav_HB_Flux
The flux of the X-ray source in the 2-8 keV band averaged over the three
XMM-Newton cameras, in erg s-1 cm-2^, as derived from ewavelet. The authors
derived the count rate to flux conversion factors CF assuming a power-law
spectrum with a photon index Gamma of 1.7 and a Galactic absorption of NH =
2.3 x 1020 cm-2, and by weighting the responses of the MOS1, MOS2, and PN
cameras; the values of CF are 5.83 x 10-12, 3.25 x 10-12, and 1.17 x
10-11 erg cm-2 count-1, for the 0.5-8, 0.5-2 and 2-8 keV bands,
respectively.
Wav_FB_Flux_Error
The 1-sigma uncertainty in the flux of the X-ray source in the 0.5-8 keV band
averaged over the three XMM-Newton cameras, in erg s-1 cm-2^, as derived
from ewavelet.
Wav_SB_Flux_Error
The 1-sigma uncertainty in the flux of the X-ray source in the 0.5-2 keV band
averaged over the three XMM-Newton cameras, in erg s-1 cm-2^, as derived
from ewavelet.
Wav_HB_Flux_Error
The 1-sigma uncertainty in the flux of the X-ray source in the 2-8 keV band
averaged over the three XMM-Newton cameras, in erg s-1 cm-2^, as derived
from ewavelet.
Wav_FB_Detect_Scale
The ewavelet detection scale for the X-ray source, in pixels, in the 0.5-8
keV band (1 pixel = 4 arcsec).
Wav_SB_Detect_Scale
The ewavelet detection scale for the X-ray source, in pixels, in the 0.5-2
keV band (1 pixel = 4 arcsec).
Wav_HB_Detect_Scale
The ewavelet detection scale for the X-ray source, in pixels, in the 2-8 keV
band (1 pixel = 4 arcsec).
Wav_FB_Extent
The X-ray source extent from ewavelet in the 0.5-8 keV band. This is the
sigma of a Gaussian model fit to the source, in pixels, where 1 pixel = 4
arcseconds.
Wav_SB_Extent
The X-ray source extent from ewavelet in the 0.5-2 keV band. This is the
sigma of a Gaussian model fit to the source, in pixels, where 1 pixel = 4
arcseconds.
Wav_HB_Extent
The X-ray source extent from ewavelet in the 2-8 keV band. This is the sigma
of a Gaussian model fit to the source, in pixels, where 1 pixel = 4
arcseconds.
Wav_FB_Extent_Error
The 1-sigma uncertainty in the X-ray source extent from ewavelet in the 0.5-8
keV band, in pixels.
Wav_SB_Extent_Error
The 1-sigma uncertainty in the X-ray source extent from ewavelet in the 0.5-2
keV band, in pixels.
Wav_HB_Extent_Error
The 1-sigma uncertainty in the X-ray source extent from ewavelet in the 02-8
keV band, in pixels.
Source_Sample
This HEASARC-created field indicates from which source set the given entry
originates. The 1816 sources which were detected by both programs were
presented in the main table in the reference paper (and are included in this
HEASARC table where they are indicated by a value of the source_sample
parameter of 'main'), while the 234 sources which were only detected by
ewavelet were presented in the supplementary table in the reference paper
(and are included in this HEASARC table where they are indicated by a value
of the source_sample parameter of 'supp').
Contact Person
Questions regarding the XMMATLAS database table can be addressed to the HEASARC Help Desk.Page Author: Browse Software Development Team
Last Modified: Wednesday, 23-Nov-2022 19:38:06 EST
- HEASARC Director: Dr. Andy Ptak
- NASA Official: Dr. Andy Ptak
- Web Curator: J.D. Myers
- Last Modified: 23-Nov-2022