Browse
this table...

XMMSSC - XMM-Newton Serendipitous Source Catalog (3XMM DR4 Version)

HEASARC
Archive

Overview

This table contains the Third XMM-Newton Serendipitous Source Catalog, Fourth Data Release, or 3XMM-DR4.

3XMM-DR4 is the third generation catalog of serendipitous X-ray sources from the European Space Agency's (ESA) XMM-Newton observatory, and has been created by the XMM-Newton Survey Science Centre (SSC) on behalf of ESA. The catalog has 2474 more observations and about 178,000 (50%) more detections than the preceding 2XMMi-DR3 catalog, which was made public in April 2010. Significant changes have been made to the processing system to generate the 3XMM-DR4 catalog and the changes are described in Section 3 of the 3XMM-DR4 User Guide at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/UserGuide_xmmcat.html#Diff3XMMDR4.

The catalog contains source detections drawn from a total of 7,427 XMM-Newton EPIC observations made between 2000 February 3 and 2012 December 8; all datasets included were publicly available by 2012 December 31 but not all public observations are included in this catalog. For net exposure time >= 1 ksec, the total area of the catalog fields is ~ 1397 deg2 but taking account of the substantial overlaps between observations, the net sky area covered independently is ~ 794 deg2.

The catalog contains 531,261 X-ray source detections above the processing likelihood threshold of 6. These X-ray source detections relate to 372,728 unique X-ray sources, that is, a significant fraction of sources (66,728) have more than one detection in the catalog (up to 44 repeat observations in a few cases).

The catalog distinguishes between extended emission and point-like detections. Parameters of detections of extended sources are only reliable up to the maximum extent measure of 80 arcseconds. There are 52,168 detections of extended emission, of which 10,915 are 'clean' (in the sense that they were not manually flagged) and 7,698 comprise the 'cleanest' set where no flags are set and they are not in fields with high background levels

Due to intrinsic features of the instrumentation as well as some shortcomings of the source detection process, some detections are considered to be spurious or their parameters are considered to be unreliable. It is recommended to use either a detection flag or an observation flag (and, possibly, a high background flag) as filters to obtain what can be considered a 'clean' sample. There are 432,321 out of 531,261 detections that are considered to be clean (i.e., summary flag < 3) and 3,625 out of 7,427 fields are considered to have no, or at most a couple, of spurious detections in them (observation class < 2 and not a high-background field).

For about 123,860 detections, EPIC spectra and time series were automatically extracted during processing, and a Chi-Squared variability test was applied to the time series. 4,612 detections in the catalog are considered variable, within the time span of the specific observation, at a probability of 10-5 or less based on the null-hypothesis that the source is constant. Of these, 2,580 have a summary flag < 3.

The median flux (in the total photon-energy band 0.2 - 12 keV) of the catalog detections is ~ 2.4 x 10-14 erg/cm2/s; in the soft energy band (0.2 - 2 keV) the median flux is ~ 5.7 x 10-15, and in the hard band (2 - 12 keV) it is ~ 1.3 x 10-14. About 20% have fluxes below 1 x 10-14 erg/cm2/s. The flux values from the three EPIC cameras are, overall, in agreement to ~ 10% for most energy bands. The positional accuracy of the catalog point source detections is generally < 3 arcseconds (90% confidence radius) and 90% of point sources have 1-sigma positional uncertainties < 2.4 arcseconds.

The energy bands used in the 3XMM-DR4 processing were the same as for the 2XMM catalog. The following are the basic energy bands:

1       =       0.2 -   0.5 keV
2       =       0.5 -   1.0 keV
3       =       1.0 -   2.0 keV
4       =       2.0 -   4.5 keV
5       =       4.5 -  12.0 keV

while these are the broad energy bands:

6       =       0.2 -   2.0 keV                 soft band, no images made
7       =       2.0 -  12.0 keV                 hard band, no images made
8       =       0.2 -  12.0 keV                 total band
9       =       0.5 -   4.5 keV                 XID band

Since the release of this catalog on 2013 July 23, a number of issues have come to light. These are

(1) The vignetting values in the catalogue table are wrong.

(2) The timeseries (TS) products extracted for some objects are not corrected to on-axis (true for 3XMM-DR4 and all earlier catalogues too).

(3) A subset of the mosaic mode observations are either wrong or partially wrong.

Issues (1) and (3) are discussed more extensively at http://xmmssc-www.star.le.ac.uk/Catalogue/xcat_public_3XMM-DR4.html#watchouts. Issue (2) is discussed in Section 6.1.4 of the 3XMM-DR4 User Guide at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/UserGuide_xmmcat.html#TSuncorr.


Catalog Bibcode

2009A&A...493..339W

References

The following is the preferred citation of this version (3XMM-DR4) of the catalog:
    Watson et al. (2013), "The XMM-Newton Serendipitous Survey. VII. The Third
    XMM-Newton Serendipitous Source Catalogue", in preparation.
The following is the preferred citation of the previous 2XMM version of the catalog:
    Watson et al. (2009), "The XMM-Newton Serendipitous Survey. V. The Second
    XMM-Newton Serendipitous Source Catalogue", A&A, 493, 339-373.

Provenance

This HEASARC database table contains the 3XMM-DR4 catalog, released by ESA on 2013 July 23, and obtained from the XMM-Newton Survey Science Center (http://xmmssc-www.star.le.ac.uk). It is also available as a gzipped FITS file: http://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/3XMMDR4cat_v1.0.fits.gz. The previous versions of the Serendipitous Source Catalog, 1XMM, 2XMMp, 2XMM, 2XMMi and 2XMMi-DR3 are also available in the same directory for comparison purposes in the files ssc_xmmcat_v1.1.0.fits.gz, ssc_2xmmpcat_v1.0.fits.gz, 2XMMcat_v1.0.fits.gz, 2XMMicat_v1.1.fits.gz and 2XMMiDR3cat_v1.0.fits.gz, respectively.

Description

Pointed observations with the XMM-Newton Observatory detect significant numbers of previously unknown 'serendipitous' X-ray sources in addition to the proposed target. Combining the data from many observations thus yields a serendipitous source catalog which, by virtue of the large field of view of XMM-Newton and its high sensitivity, represents a significant resource. The serendipitous source catalog enhances our knowledge of the X-ray sky and has the potential for advancing our understanding of the nature of various Galactic and extragalactic source populations.

The 3XMM-DR4 catalog is the sixth publicly released XMM X-ray source catalog produced by the XMM Survey Science Centre (SSC) consortium. It follows the 1XMM (released in April 2003), 2XMMp (July 2006), 2XMM (August 2007), 2XMMi (August 2008) and 2XMMi-DR3 (April 2010) catalogs: 2XMMp was a preliminary version of 2XMM. 2XMMi and 2XMMi-DR3 are incremental versions of the 2XMM catalog.

The 3XMM-DR4 catalog is about 50% larger than the 2XMMi-DR3 catalog, which it supersedes. This is principally because of the ~3.2-year longer baseline of observations included, though some sensitivity enhancements also contribute. In terms of the number of X-ray sources, the 3XMM-DR4 catalog is the largest ever produced. 3XMM-DR4 complements deeper Chandra and XMM-Newton small area surveys, probing a large sky area at the flux limit where the bulk of the objects that contribute to the X-ray background lie. The 3XMM-DR4 catalog provides a rich resource for generating large, well-defined samples for specific studies, utilizing the fact that X-ray selection is a highly efficient (arguably the most efficient) way of selecting certain types of object, notably active galaxies (AGN), clusters of galaxies, interacting compact binaries and active stellar coronae. The large sky area covered by the serendipitous survey, or equivalently the large size of the catalog, also means that 3XMM-DR4 is a superb resource for exploring the variety of the X-ray source population and identifying rare source types.

The production of the 3XMM-DR4 catalog has been undertaken by the XMM-Newton SSC consortium in fulfillment of one of its major responsibilities within the XMM-Newton project. The catalog production process has been designed to exploit fully the capabilities of the XMM-Newton EPIC cameras and to ensure the integrity and quality of the resultant catalog through rigorous screening of the data.

The 3XMM-DR4 catalog is the result of a bulk reprocessing of all the available XMM-Newton data. It is based on a pipeline (cat9.0 - configuration 00000004_04_cat9.0_20121220.153800) that contains significant changes to the processing approach to enhance the quality of the catalog. It makes use of the latest SAS version (12.0.1, but with a small number of specifically updated SAS tasks) and the latest calibration files available at the time of the bulk reprocessing. For the bulk reprocessing run, the pipeline, SAS and calibration components were static throughout the run.

Users of the 3XMM-DR4 catalog should be aware that the DETID and SRCID values bear no relation to those in the previous 2XMM series of catalogs. However, a cross-matching is provided in 3XMM-DR4 via the DR3_DETID and DR3_SRCID columns.


Catalog Properties

The catalog contains source detections drawn from 7,427 XMM-Newton EPIC observations made between 2000 February 3 and 2012 December 8 and which were publicly available by 2012 December 31. Net exposure times in these observations range from < 1,000 up to ~ 130,000 seconds (that is, a full orbit of the satellite). Figure 5.1 at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/fig_5.1.html shows the distribution of the net exposure time of the fields included, while Figure 5.2 at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/fig_5.2.html shows the distribution of fields on the sky. The total sky area of the catalog observations with effective exposure > 1 ks is ~ 1,397 deg2 which translates to ~ 793 deg2 when corrected for field overlaps. Figure 5.3 at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/fig_5.3.html shows the sky area as a function of net exposure time. For Figs. 5.1-5.3 the equivalent data for the previous 2XMMi-DR3 catalog are shown for comparison. The catalog contains 531,261 X-ray detections with total-band (0.2 -12 keV) likelihood values >= 6. These are detections of 372,728 unique X-ray sources, that is, 66,728 X-ray sources have multiple detections in separate observations (up to 44 detections). Of the 531,261 X-ray detections, 52,168 are classified as extended with 10,915 of these being in regions considered to be 'clean'. (SUM_FLAG < 3).

Data Quality: As part of extensive quality evaluation for the catalog, each field has been visually screened. Regions where there were obvious deficiencies with the automatic source detection and parametrization process were identified and all detections within those regions were flagged. Such flagged detections include clearly spurious detections (many of which are classified as extended) as well as detections where the source parameters may be unreliable. Each XMM-Newton field is also evaluated to assess the fractional area of the observation that is affected by flagged detections, as reflected by the OBS_CLASS parameter. For most uses of the catalog it is recommended to use either a detection flag (SUM_FLAG, EP_FLAG or SC_SUM_FLAG) or an observation flag (OBS_CLASS) as a filter to obtain what can be considered a 'clean' sample. There are 375,273 detections (71%) that have not received any flag (i.e. no issues noted, SUM_FLAG =0), while 432,321 detections (81%) can be considered to be reasonably 'clean', i.e. have SUM_FLAG < 3. In terms of the overall field properties, 6,369 out of 7,427 fields (86%) have only small fraction of flagged detections (i.e OBS_CLASS < 4). Note that no attempt is made to flag spurious detections arising from statistical fluctuations in the background. An updated analysis of the false detection rate will be presented in the forthcoming 3XMM catalog paper.

Sensitivity and Photometry: Figure 5.4 at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/fig_5.4.html presents, for each of the three cameras, the distributions of flux for energy bands 1 to 5 and also for the combined (EPIC) data. These give an indication of the limiting flux available in the catalogs for each of the bands. Comparison of the detection count rates and fluxes in the 3XMM-DR4 and the previous 2XMMi-DR3 version shows good agreement between the two catalogs. A more detailed analysis of photometric issues will be presented in the forthcoming 3XMM catalog paper.

Astrometry: The 3XMM-DR4 catalog benefits from a number of improvements to the astrometry, several of which resulted from effects only discovered in the process of compiling the catalog. The net effect for 3XMM-DR4 source positions is a small improvement in the statistical position errors, a reduction in the position error systematics and increased confidence in the reliability of the position errors. A more detailed analysis of these issues will again be presented in the forthcoming 3XMM catalog paper.


Visual Screening

As for previous catalogs, every XMM-Newton observation in 3XMM-DR4 has been visually inspected with the purpose of identifying problematic areas where source detection or source characterization are potentially suspect. The manual screening process generates mask files that define the problematic regions. These may be confined regions around individual suspect detections or larger areas enclosing multiple affected detections, up to the full area of the field where serious problems exist. Detections in such regions are subsequently assigned a manual flag (flag 11) in the flag columns (PN_FLAG, M1_FLAG, M2_FLAG, EP_FLAG). A source with flag 11 set to (T)rue does not indicate that the detections are necessarily spurious.

The masked area of each image is an indicator of the quality of the field as a whole. The distribution of the six observation classes (OBS_CLASS) has changed with respect to 2XMMi-DR3. The dominant change is in the split of fields assigned observation classes (OBS_CLASS) 0 and 1. The largest change with respect to 2XMMi-DR3 is in OBS_CLASS 1 cases; this is mainly due to the fact that during visual screening for 3XMM-DR4, individual suspect objects in the wings of bright sources were individually masked rather than the whole region.

The able below lists the observation class, the fractional area of exclusion with respect to the total detection area, and the percentage of observations affected for the 3XMM-DR4 and 2XMMi-DR3 catalogs:

Table 4:  Distribution of observation class for the 7427 observation sets used
          in 3XMM-DR4, compared with that for the observations in the 2XMMi-DR3
          catalog

Obs class 	'bad' area fraction 	      3XMM-DR4 	      2XMMi-DR3
   0 	        0% area 	                27% 	         35%
   1 	        0% < area < 0.1% 	        22% 	         12%
   2 	        0.1% <= area < 1% 	        12% 	         10%
   3 	        1% <= area < 10% 	        24% 	         28%
   4 	        10% <= area < 100% 	        11% 	         12%
   5 	        100% 	                         4% 	          4%

Total number of observations 	              7,427 	       4,953

Credits

The production of the 3XMM catalog was a collaborative project involving the whole SSC Consortium:
    University of Leicester, UK

    Mullard Space Science Laboratory, University College London, UK

    Institute of Astronomy, Cambridge, UK

    Max-Planck Institut fuer extraterrestrische Physik, Germany

    Astrophysikalisches Institut Potsdam, Germany

    Service d'Astrophysique, CEA/DSM/DAPNIA, Saclay, France

    Centre d'Etude Spatiale des Rayonnements, Toulouse, France

    Observatoire Astronomique de Strasbourg, France

    Instituto de Fisica de Cantabria, Santander, Spain

    Osservatorio Astronomico di Brera, Milan, Italy

The SSC team is pleased to acknowledge the contributions to the SAS software, on which the catalog processing is based, made by ESA's Science Operations Centre staff. Significant contributions to the production of the catalog were also made by the NASA/Goddard Space Flight Center/HEASARC staff resident for much of the project at the University of Leicester.


Documentation

The User Guide for the 3XMM-DR4 Catalog, available at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/UserGuide_xmmcat.html, contains details of the catalog production process and content. A complete description of this catalog and the parameters listed therein can be found there, as well as the list of observations used in the catalog at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/xcat_summary.html. The user should particularly refer to section 6 of the 3XMM-DR4 UG, 'Known Problems and Other Issues' at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/UserGuide_xmmcat.html#Problems as this material is not included in this HEASARC document.

Key Changes in 3XMM-DR4 with Respect to the 2XMMi-DR3 Catalog

XMM-Newton observations considered for inclusion in the 3XMM-DR4 catalog were those with ODFs available for processing up to 2012 December 08 and which had public release dates up to 2012 December 31. No observations taken after the suspected MOS1 event on 2012 December 11 (revolution 2382) have been included. After allowing for a small number (< 100) of observations which failed in processing for a variety of reasons, 7,427 observations were available to make the 3XMM-DR4 catalog. Table 2.1 at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/xcat_summary.html gives the list of the final 7,427 observations which are included in the 3XMM-DR4 catalog.

3XMM-DR4 contains 2,505 observations that are not in 2XMMi-DR3, of which around 440 were public and available for inclusion in 2XMMi-DR3 but were not included in 2XMMi-DR3. Many of these latter cases are fields with high backgrounds, while others are cases that failed in previous processing but processed satisfactorily during the processing for 3XMM-DR4. There are 31 observations in 2XMMi-DR3 that did not make it in to 3XMM-DR4, mainly due to software/pipeline errors during processing. Typical examples of the latter problems are due to revised ODFs (e.g. with no useful time-correlation information), more sophisticated SAS software that identified issues hitherto not trapped, or issues with exposure corrections of background flare light curves and pn time-jumps.

Following the release of the 2XMMi-DR3 catalog, the opportunity was taken to review software and calibration upgrades and to explore developments that could enhance the scientific quality of the next catalog. Here we summarize the key changes that have been implemented in to the cat9.0 pipeline that was used to perform the bulk-reprocessing of all XMM-Newton EPIC data for the 3XMM-DR4 catalog. Further details of these changes are provided at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/UserGuide_xmmcat.html#Diff3XMMDR4, along with explanations of other, more general differences for this bulk reprocessing. The 2XMM User Guide cited above is a useful reference for other elements of the process that have not changed, and provides a background context for those that have.

1. Use of empirical Point Spread Function (PSF) models (section 3.3 of the 3XMM-DR4 UG): Recent, empirical characterizations of the EPIC pn, MOS1 and MOS2 telescope PSFs (contained in the calibration data) have been exploited in the source detection process. These PSFs provide better representations of the polygonal core structures and the spoke patterns of the EPIC PSFs, which helps improve source parametrization, reduces the detection of spurious objects in the wings of bright objects and contributes to improvements in the astrometric accuracy of sources.

2. Improved field rectification (section 3.4.1 of the 3XMM-DR4 UG): The SAS task, catcorr, is used to provide enhanced field rectification (i.e. field frame-shift corrections) against external absolute astrometric reference catalogs. This involves i) the use of 3 possible reference catalogs (USNO B1.0, 2MASS and SDSS (DR8)), ii) improvements to the process of matching XMM detections with reference catalog objects and iii) better algorithms for determining the frame-shift and rotation corrections and errors. The result is more fields that can be successfully rectified, greater accuracy of the results and improved error analysis.

3. Exploitation of a time-dependent boresight (section 3.4.2 of the 3XMM-DR4 UG): Extensive analysis of the spatial displacements of a subset of 2XMMi-DR3 X-ray detections, with respect to counterparts in the SDSS spectroscopic and photometric quasar catalogs, revealed systematic time-dependent offsets with a semi-amplitude ~ 1 arcsecond. These variations have been used by the XMM calibration teams to create a time-dependent correction to the spacecraft boresight, which is applied to event coordinates during event processing.

4. Optimized global background flare filtering (section 3.2 of the 3XMM-DR4 UG): In previous pipeline processing, background flares were filtered out by deriving Good-Time-Intervals (GTIs) during which high-energy (> 7 keV) background timeseries count rates, obtained from the whole imaged field-of-view, were below instrument-specific, constant cut thresholds. In the current pipeline, GTIs to exclude flares are derived from a 0.5-7.5 keV (in-band) background flare timeseries from the imaged field of view, from which prominent sources have been excluded. The new algorithm employs the SAS task, bkgoptrate, to determine an optimum cut threshold that seeks to maximize the Signal-to-Noise of sources in the field. This analysis is applied to each exposure for each instrument and is used to create the background flare GTIs for downstream processing.

5. Optimized extraction of spectra and timeseries (section 3.6 of the 3XMM-DR4 UG). Two new approaches are applied to the extraction of EPIC spectra and timeseries from suitably bright detections. Firstly, the SAS task, eregionanalyse, is used to establish an extraction radius that maximizes the total Signal-to-Noise of the extracted source data - previously a fixed aperture of 28 arcsecond radius was used. Furthermore, the count threshold above which spectra and timeseries are extracted, has been reduced to requiring > 100 'good' spectrum counts for the instrument/exposure (previously > 500 EPIC counts were required). Secondly, in previous pipelines, in some circumstances, especially objects located in the central window in MOS small-window mode observations, the annular background region used, which was co-centered with the source, could yield empty, or near-empty, background spectra, which would cause downstream problems for spectral fitting and timeseries analyses. In the current cat9.0 pipeline, the location of a circular background region is moved around the source in radial and azimuthal steps until an acceptable fraction (> 70%) of usable background area is identified.

6. Automated flagging of detections affected by Out-of-Time and RGA scattered light features (section 3.7 of the 3XMM-DR4 UG): A simple algorithm has been implemented in the SAS task, eootepileupmask, to detect the presence of piled up sources and create a mask that indicates where associated Out-of-Time (OoT) events may be inadequately modeled, which can lead to spurious source detections. The same SAS task also attempts to identify the linear features in MOS images arising from X-rays from bright objects that are scattered by the RGAs. These masks are subsequently used by the SAS task, dpssflag, to set a flag (flag 10) for detections whose centers lie on such features.

7. Improved pn low energy noise filtering (section 3.5 of the 3XMM-DR4 UG): The SAS task, epreject, is used to suppress, in particular, the detection of features in pn band 1 images that arise from Minimum Ionizing Particles (MIPs).

8. Improved detection matching for unique sources (section 3.8 of the 3XMM-DR4 UG): A revised approach has been adopted for matching separate source detections in to unique sources on the sky. This employs Bayesian methodology.

9. Addition of fractional excess variance measures (section 3.9 of the 3XMM-DR4 UG): The fractional excess variance (and error) is computed by the SAS task, ekstest, for each extracted EPIC timeseries; the catalog provides values, where this value was computable, for the most variable exposure available for each instrument. This provides a measure of the amplitude of variability above statistical fluctuations of the background.


User Guide for 2XMM

The extensive User Guide (UG) for the 2XMM catalog at http://xmmssc-www.star.le.ac.uk/Catalogue/2XMM/UserGuide_xmmcat.html still describes many of the details of the data processing and compilation approach applicable to the 3XMM-DR4 catalog. However, a significant number of changes to the processing have been implemented for 3XMM-DR4 and these are described in the 'Differences' section of the 3XMM-DR4 User Guide at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/UserGuide_xmmcat.html#Diff3XMMDR4 and summarized in the previous section.

Catalog Content and Organization

There are 318 parameters in the catalog. For each observation, there are up to three cameras with one or more exposures which were merged when the filter and sub-modes were the same. The data in each exposure are accumulated in several distinct energy bands (Table 1 above). Camera-level measurements can further be combined into observation-level parameters. Consequently, the source parameters can refer to some or all of these levels: on the observation level there are the final mean parameters of the source (prefix 'EP'); on the camera level the data for each of the three cameras (where available) are given (prefix 'PN', 'M1', or 'M2'), and on the energy band level the energy-dependent details of the source parameters are given (indicated by a 'b' in the column name where b = 1, 2, 3, 4, 5, 8 or 9). Finally, on a meta-level, some parameters of sources that were detected more than once (prefix 'SC') were combined. Entries with NULL are given when no detection was made with the respective camera, that is, ca_MASKFRAC < 0.15 or NULL (i.e., a camera was not used in an observation).

Parameters

Detid
A consecutive number which identifies each entry (detection) in the catalog. The correct nomenclature for references to detections in the catalog is the source name followed by a colon and the detection identification number DETID (with six digits), that is: '3XMM Jhhmmss.sSddmmss:detid'. The DETID numbering assignments in 3XMM-DR4 bear no relation to those in 2XMMi-DR3 but the DETID of the nearest matching detection from the 2XMMi-DR3 catalog to the 3XMM-DR4 detection is provided via the DR3_DETID parameter.

SrcID
A unique number assigned to a group of catalog entries which are assumed to be the same source. The process of grouping detections in to unique sources has changed since the 2XMM catalogue series and is described in Section 3.8 of the 3XMM-DR4 UG at http://xmmssc-www.star.le.ac.uk/Catalogue/3XMM-DR4/UserGuide_xmmcat.html#DiffUniqueId. The SRCID assignments in 3XMM-DR4 bear no relation to those in 2XMMi-DR3, but the nearest unique sources from the 2XMMi-DR3 catalogue to the 3XMM-DR4 unique source is provided via the DR3_SRCID column.

DR3_SrcID
The 2XMMi-DR3 source identifier of the nearest unique 2XMMi-DR3 source that lies within 10 arcseconds of the 3XMM-DR4 unique source position.

DR3_Detid
The 2XMMi-DR3 detection identifier of the nearest 2XMMi-DR3 detection that lies within 10 arcseconds of the detection position in 3XMM-DR4.

DR3_Detdist
The distance in arcseconds between the 3XMM-DR4 detection position and the nearest detection (within 10 arcseconds) in the 2XMMi-DR3 catalog.

DR3_Srcdist
The distance in arcseconds between the 3XMM-DR4 unique source position and the nearest unique source (within 10 arcseconds) in the 2XMMi-DR3 catalog.

DR3_Mult
The number of unique sources from the 2XMMi-DR3 catalog that lie within 10 arcseconds of the unique source position in 3XMM-DR4.

Name
The IAU designation assigned to the unique SRCID. An IAU-style identification, NAME, has been assigned to each unique source (SRCID) based upon the IAU registered classification, 3XMM, and the J2000.0 source coordinates. The form of the IAU names is '3XMM Jhhmmss.sSddmmss' where hhmmss.s is taken from the Right Ascension coordinate given in the RA parameter and Sddmmss is the Declination taken from the Dec parameter.

Src_Num
The decimal source number in the individual source list for this observation; when expressed in hexadecimal it identifies the source-specific product files belonging to this detection. (See Appendix A.1 of the 2XMM UG at http://xmmssc-www.star.le.ac.uk/Catalogue/2XMM/UserGuide_xmmcat.html#AppProd for more details).

ObsID
The XMM-Newton observation identification.

XMM_Revolution
The XMM-Newton revolution number of the observation.

Time
The start time of the observation (converted from the Modified Julian Date format given in the original input file).

End_Time
The end time of the observation (converted from the Modified Julian Date format given in the original input file).

Obs_Class
The quality classification of the whole observation based on the area flagged as bad in the manual flagging process as compared to the whole detection area. 0 means nothing has been flagged; 1 indicates that 0% < area < 0.1% of the total detection mask has been flagged; 2 indicates that 0.1% <= area < 1% has been flagged; 3 indicates that 1% <= area < 10% has been flagged; 4 indicates that 10% <= area < 100% has been flagged; and 5 means that the whole field was flagged as bad.

PN_Filter
The type of PN filter used. The options are Thick, Medium, Thin1, Thin2, and Open, depending on the efficiency of the optical blocking.

M1_Filter
The type of M1 filter used. The options are Thick, Medium, Thin1, and Open, depending on the efficiency of the optical blocking.

M2_Filter
The type of M2 filter used. The options are Thick, Medium, Thin1, and Open, depending on the efficiency of the optical blocking.

PN_Submode
The PN observing mode. The options are full frame mode with the full FOV exposed (in two sub-modes), and large window mode with only parts of the FOV exposed.

M1_Submode
The M1 observing mode. The options are full frame mode with the full FOV exposed, partial window mode with only parts of the central CCD exposed (in different sub-modes), and timing mode where the central CCD was not exposed ('Fast Uncompressed').

M2_Submode
The M2 observing mode. The options are full frame mode with the full FOV exposed, partial window mode with only parts of the central CCD exposed (in different sub-modes), and timing mode where the central CCD was not exposed ('Fast Uncompressed').

RA
The corrected Right Ascension of the detection in the selected equinox after statistical correlation of the emldetect coordinates, RA_UNC and DEC_UNC, with the USNO B1.0, 2MASS or SDSS (DR8) optical/IR source catalogs using the SAS task catcorr (the process of correcting the coordinates is also referred to as field rectification). In cases where the cross-correlation is determined to be unreliable, no correction is applied and this value is therefore the same as RA_UNC. The RA was given in J2000.0 decimal degrees in the original table.

Dec
The corrected Declination of the detection in the selected equinox after statistical correlation of the emldetect coordinates, RA_UNC and DEC_UNC, with the USNO B1.0, 2MASS or SDSS (DR8) optical/IR source catalogs using the SAS task catcorr (the process of correcting the coordinates is also referred to as field rectification). In cases where the cross-correlation is determined to be unreliable, no correction is applied and this value is therefore the same as DEC_UNC. The Declination was given in J2000 decimal degrees in the original table.

Error_Radius
The total positional uncertainty, in arcseconds, (called POSERR in the original table) calculated by combining the statistical error RADEC_ERROR (called RADEC_ERR in the original table) and the error arising from the field rectification process SYSERRCC as follows:

     POSERR = SQRT (RADEC_ERROR2 + SYSERRCC2 ).
  

LII
The corrected Galactic Longitude of the detection in degrees.

BII
The corrected Galactic Latitude of the detection in degrees.

RADec_Error
The statistical 1-sigma error in the detection position, in arcseconds.

Syserrcc
The estimated 1-sigma error arising from the field rectification process, in arcseconds. If the SAS task catcorr results in a statistically reliable cross-correlation with the USNO B1.0, 2MASS or SDSS (DR8) optical/IR catalogs, SYSERRCC combines the errors on the translational shifts in the RA (rashift_error) and DEC (decshift_error) directions, together with the rotational error component, derived from from the catalog that yields the 'best' solution, as follows:

     SYSERRCC = SQRT (rashift_error2 + decshift_error2 +
                       (r * thetarot_error)2)
  
where r is the radial off-axis angle of the detection from the spacecraft boresight, in arcseconds, and thetarot_error is the error on the rotational correction, in radians. Where catcorr fails to obtain a statistically reliable result, SYSERRCC is set to 1.5 arcseconds (see 3XMM-DR4 UG, Sec. 3.5 for details). Note that rashift_error, decshift_error and thetarot_error are not provided separately in the catalog.

Refcat
An integer code reflecting the absolute astrometric reference catalog which gave the statistically 'best' result for the field rectification process (from which the corrections are taken). It is 1 for the USNO B1.0 catalog, 2 for 2MASS and 3 for SDSS (DR8). Where catcorr fails to produce a reliable solution, REFCAT is a negative number, indicating the cause of the failure. The failure codes are

  -1 = Too few matches (< 10),
  -2 = poor fit (goodness of fit parameter in catcorr < 5.0),
  -3 = error on the field positional rectification correction is > 0.75
       arcseconds
  
See 3XMM-DR4 UG, Sec. 3.5 for more details.

Poscorok_Flag
This Boolean flag [T/F] parameter signifies whether catcorr obtained a statistically reliable solution or not. This parameter is redundant in the sense that if REFCAT is positive, then a reliable solution was considered to have been found (see 3XMM-DR4 UG, Sec. 3.5 for details).

RA_Unc
The Right Ascension of the detection in the selected equinox, as determined by the SAS task emldetect by fitting a detection simultaneously in all cameras and energy bands. This was given in J2000.0 decimal degrees in the original SSC table.

Dec_Unc
The Declination of the detection in the selected equinox, as determined by the SAS task emldetect by fitting a detection simultaneously in all cameras and energy bands. This was given in J2000.0 decimal degrees in the original SSC table.

EP_1_Flux
The EPIC band 1 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. The EPIC flux in each band is the mean of the band-specific detections in all cameras weighted by the errors.

EP_1_Flux_Error
The uncertainty in EPIC band 1 flux (erg/cm2/s). The error in the weighted mean of the EPIC flux in band b is given by:

            EP_b_FLUX_ERR = SQRT (1.0 / SUM (1 / ca_b_FLUX_ERR2 ))
  
where ca = PN, M1, M2, and b is the band (1, 2, 3, 4, 5, 8, 9).

EP_2_Flux
The EPIC band 2 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. The EPIC flux in each band is the mean of the band-specific detections in all cameras weighted by the errors.

EP_2_Flux_Error
The uncertainty in EPIC band 2 flux (erg/cm2/s). The error in the weighted mean of the EPIC flux in band b is given by:

            EP_b_FLUX_ERR = SQRT (1.0 / SUM (1 / ca_b_FLUX_ERR2 ))
  
where ca = PN, M1, M2, and b is the band (1, 2, 3, 4, 5, 8, 9).

EP_3_Flux
The EPIC band 3 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. The EPIC flux in each band is the mean of the band-specific detections in all cameras weighted by the errors.

EP_3_Flux_Error
The uncertainty in the EPIC band 3 flux (erg/cm2/s). The error in the weighted mean of the EPIC flux in band b is given by:

            EP_b_FLUX_ERR = SQRT (1.0 / SUM (1 / ca_b_FLUX_ERR2 ))
  
where ca = PN, M1, M2, and b is the band (1, 2, 3, 4, 5, 8, 9).

EP_4_Flux
The EPIC band 4 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. The EPIC flux in each band is the mean of the band-specific detections in all cameras weighted by the errors.

EP_4_Flux_Error
The uncertainty in the EPIC band 4 flux (erg/cm2/s). The error in the weighted mean of the EPIC flux in band b is given by:

            EP_b_FLUX_ERR = SQRT (1.0 / SUM (1 / ca_b_FLUX_ERR2 ))
  
where ca = PN, M1, M2, and b is the band (1, 2, 3, 4, 5, 8, 9).

EP_5_Flux
The EPIC band 5 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. The EPIC flux in each band is the mean of the band-specific detections in all cameras weighted by the errors.

EP_5_Flux_Error
The uncertainty in the EPIC band 5 flux (erg/cm2/s). The error in the weighted mean of the EPIC flux in band b is given by:

            EP_b_FLUX_ERR = SQRT (1.0 / SUM (1 / ca_b_FLUX_ERR2 ))
  
where ca = PN, M1, M2, and b is the band (1, 2, 3, 4, 5, 8, 9).

EP_8_Flux
The EPIC combined band 8 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. The EPIC flux in each band is the mean of the band-specific detections in all cameras weighted by the errors. Combined band fluxes for the individual cameras are the sum of the fluxes and errors from each band (1 - 5).

EP_8_Flux_Error
The uncertainty in the EPIC combined band flux (erg/cm2/s). The error in the weighted mean of the EPIC flux in band b is given by:

            EP_b_FLUX_ERR = SQRT (1.0 / SUM (1 / ca_b_FLUX_ERR2 ))
  
where ca = PN, M1, M2, and b is the band (1, 2, 3, 4, 5, 8, 9).

EP_9_Flux
The EPIC band 9 (XID) flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. The EPIC flux in each band is the mean of the band-specific detections in all cameras weighted by the errors.

EP_9_Flux_Error
The uncertainty in the EPIC band 9 flux (erg/cm2/s). The error in the weighted mean of the EPIC flux in band b is given by:

            EP_b_FLUX_ERR = SQRT (1.0 / SUM (1 / ca_b_FLUX_ERR2 ))
  
where ca = PN, M1, M2, and b is the band (1, 2, 3, 4, 5, 8, 9).

PN_1_Flux
The PN band 1 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

PN_1_Flux_Error
The uncertainty in the PN band 1 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

PN_2_Flux
The PN band 2 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

PN_2_Flux_Error
The uncertainty in the PN band 2 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

PN_3_Flux
The PN band 3 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

PN_3_Flux_Error
The uncertainty in the PN band 3 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

PN_4_Flux
The PN band 4 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

PN_4_Flux_Error
The uncertainty in the PN band 4 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

PN_5_Flux
The PN band 5 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

PN_5_Flux_Error
The uncertainty in the PN band 5 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

PN_8_Flux
The PN combined band flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. Combined band fluxes (band 8) for the individual cameras are the sum of the fluxes from each band (1 - 5).

PN_8_Flux_Error
The uncertainty in the PN combined band flux (erg/cm2/s). Combined band fluxes and errors (band 8) for the individual cameras are the sum of the fluxes and errors from each band (1 - 5).

PN_9_Flux
The PN band 9 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

PN_9_Flux_Error
The uncertainty in the PN band 9 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M1_1_Flux
The M1 band 1 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M1_1_Flux_Error
The uncertainty in the M1 band 1 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M1_2_Flux
The M1 band 2 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M1_2_Flux_Error
The uncertainty in the M1 band 2 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M1_3_Flux
The M1 band 3 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M1_3_Flux_Error
The uncertainty in the M1 band 3 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M1_4_Flux
The M1 band 4 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M1_4_Flux_Error
The uncertainty in the M1 band 4 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M1_5_Flux
The M1 band 5 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M1_5_Flux_Error
The uncertainty in the M1 band 5 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M1_8_Flux
The M1 combined band flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. Combined band fluxes and errors (band 8) for the individual cameras are the sum of the fluxes and errors from each band (1 - 5).

M1_8_Flux_Error
The uncertainty in the M1 combined band flux (erg/cm2/s). Combined band fluxes and errors (band 8) for the individual cameras are the sum of the fluxes and errors from each band (1 - 5).

M1_9_Flux
The M1 band 9 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M1_9_Flux_Error
The uncertainty in the M1 band 9 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M2_1_Flux
The M2 band 1 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M2_1_Flux_Error
The uncertainty in the M2 band 1 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M2_2_Flux
The M2 band 2 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M2_2_Flux_Error
The uncertainty in the M2 band 2 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M2_3_Flux
The M2 band 3 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M2_3_Flux_Error
The uncertainty in the M2 band 3 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M2_4_Flux
The M2 band 4 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M2_4_Flux_Error
The uncertainty in the M2 band 4 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M2_5_Flux
The M2 band 5 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M2_5_Flux_Error
The uncertainty in the M2 band 5 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

M2_8_Flux
The M2 combined band flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. Combined band fluxes and errors (band 8) for the individual cameras are the sum of the fluxes and errors from each band (1 - 5).

M2_8_Flux_Error
The uncertainty in the M2 combined band flux (erg/cm2/s). Combined band fluxes and errors (band 8) for the individual cameras are the sum of the fluxes and errors from each band (1 - 5).

M2_9_Flux
The M2 band 9 flux (erg/cm2/s). Fluxes are calculated by the SAS tasks emldetect and by srcmatch for the various input bands. Note that they correspond to the flux in the entire PSF and do not need any further corrections for PSF losses. For the individual cameras, individual-band fluxes (bands 1 - 5, 9) are calculated from the respective band count rate using the filter- and camera-dependent energy conversion factors given in Table 3.2 of the 3XMM-DR4 UG and corrected for the dead time due to the read-out phase. These can be 0.0 if the detection has no counts.

M2_9_Flux_Error
The uncertainty in the M2 band 9 flux (erg/cm2/s). These errors are calculated from the respective band count rate error using the respective energy conversion factors.

EP_8_Rate
The EPIC combined band count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable. The combined band count rate (band 8) for each camera is calculated as the sum of the count rates in the individual bands 1 - 5. The EPIC rates are the sum of the camera-specific count rates in the respective band.

EP_8_Rate_Error
The uncertainty in the EPIC combined band 8 count rate (ct/s).

EP_9_Rate
The EPIC band 9 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable. The EPIC rates are the sum of the camera-specific count rates in the respective band.

EP_9_Rate_Error
The uncertainty in the EPIC band 9 count rate (ct/s).

PN_1_Rate
The PN band 1 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

PN_1_Rate_Error
The uncertainty in the PN band 1 count rate (ct/s).

PN_2_Rate
The PN band 2 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

PN_2_Rate_Error
The uncertainty in the PN band 2 count rate (ct/s).

PN_3_Rate
The PN band 3 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

PN_3_Rate_Error
The uncertainty in the PN band 3 count rate (ct/s).

PN_4_Rate
The PN band 4 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

PN_4_Rate_Error
The uncertainty in the PN band 4 count rate (ct/s).

PN_5_Rate
The PN band 5 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

PN_5_Rate_Error
The uncertainty in the PN band 5 count rate (ct/s).

PN_8_Rate
The PN combined band 8 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

PN_8_Rate_Error
The uncertainty in the PN combined band 8 count rate (ct/s).

PN_9_Rate
The PN band 9 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

PN_9_Rate_Error
The uncertainty in the PN band 9 count rate (ct/s).

M1_1_Rate
The M1 band 1 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M1_1_Rate_Error
The uncertainty in the M1 band 1 count rate (ct/s).

M1_2_Rate
The M1 band 2 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M1_2_Rate_Error
The uncertainty in the M1 band 2 count rate (ct/s).

M1_3_Rate
The M1 band 3 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M1_3_Rate_Error
The uncertainty in the M1 band 3 count rate (ct/s).

M1_4_Rate
The M1 band 4 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M1_4_Rate_Error
The uncertainty in the M1 band 4 count rate (ct/s).

M1_5_Rate
The M1 band 5 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M1_5_Rate_Error
The uncertainty in the M1 band 5 count rate (ct/s).

M1_8_Rate
The M1 combined band 8 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M1_8_Rate_Error
The uncertainty in the M1 combined band count rate (ct/s).

M1_9_Rate
The M1 band 1 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M1_9_Rate_Error
The uncertainty in the M1 band 9 count rate (ct/s).

M2_1_Rate
The M2 band 1 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M2_1_Rate_Error
The uncertainty in the M2 band 1 count rate (ct/s).

M2_2_Rate
The M2 band 2 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M2_2_Rate_Error
The uncertainty in the M2 band 2 count rate (ct/s).

M2_3_Rate
The M2 band 3 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M2_3_Rate_Error
The uncertainty in the M2 band 3 count rate (ct/s).

M2_4_Rate
The M2 band 4 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M2_4_Rate_Error
The uncertainty in the M2 band 4 count rate (ct/s).

M2_5_Rate
The M2 band 5 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M2_5_Rate_Error
The uncertainty in the M2 band 5 count rate (ct/s).

M2_8_Rate
The M2 combined band 8 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M2_8_Rate_Error
The uncertainty in the M2 combined band count rate (ct/s).

M2_9_Rate
The M2 band 9 count rate (ct/s), as derived by the SAS task emldetect. The individual-band count rate (bands 1 - 5, 9) is the band-dependent source counts (ca_b_CTS) divided by the exposure map, which combines the mirror vignetting, detector efficiency, bad pixels and CCD gaps, and an OOT-factor (Out Of Time), depending on the PN modes (PN_SUBMODE). The source counts and with it the count rates were implicitly background subtracted during the fitting process. They correspond to the count rate in the entire PSF and do not need any further corrections for PSF losses. Note that rates can be 0.0 (but not negative) if the source is too faint in the respective band to be detectable.

M2_9_Rate_Error
The uncertainty in the M2 band 9 count rate (ct/s).

EP_8_Cts
The EPIC combined band 8 source counts, as derived by the SAS task emldetect. The individual-band source counts (not given in this catalog) are derived under the total PSF (point spread function) and corrected for background. The PSF is fitted on sub-images of radius 60 arcseconds in each band (CUTRAD), which means, that in most cases at least 90% of the PSF (if covered by the detector) was effectively used in the fit. Combined band source counts (band 8) for each camera are calculated as the sum of the source counts in the individual bands 1 - 5. The EPIC band 8 counts are the sum of the (available) individual camera band 8 counts.

EP_8_Cts_Error
The uncertainty in the EPIC combined band source counts, being the statistical 1-sigma error in the total source counts of the detection, as derived by the SAS task emldetect.

PN_8_Cts
The PN combined band 8 source counts, as derived by the SAS task emldetect. The individual-band source counts (not given in this catalog) are derived under the total PSF (point spread function) and corrected for background. The PSF is fitted on sub-images of radius 60 arcseconds in each band (CUTRAD), which means, that in most cases at least 90% of the PSF (if covered by the detector) was effectively used in the fit. Combined band source counts (band 8) for each camera are calculated as the sum of the source counts in the individual bands 1 - 5.

PN_8_Cts_Error
The uncertainty in the PN combined band source counts, being the statistical 1-sigma error in the total source counts of the detection, as derived by the SAS task emldetect.

M1_8_Cts
The M1 combined band 8 source counts, as derived by the SAS task emldetect. The individual-band source counts (not given in this catalog) are derived under the total PSF (point spread function) and corrected for background. The PSF is fitted on sub-images of radius 60 arcseconds in each band (CUTRAD), which means, that in most cases at least 90% of the PSF (if covered by the detector) was effectively used in the fit. Combined band source counts (band 8) for each camera are calculated as the sum of the source counts in the individual bands 1 - 5.

M1_8_Cts_Error
The uncertainty in the M1 combined band 8 source counts, being the statistical 1-sigma error in the total source counts of the detection, as derived by the SAS task emldetect.

M2_8_Cts
The M2 combined band source counts, as derived by the SAS task emldetect. The individual-band source counts (not given in this catalog) are derived under the total PSF (point spread function) and corrected for background. The PSF is fitted on sub-images of radius 60 arcseconds in each band (CUTRAD), which means, that in most cases at least 90% of the PSF (if covered by the detector) was effectively used in the fit. Combined band source counts (band 8) for each camera are calculated as the sum of the source counts in the individual bands 1 - 5.

M2_8_Cts_Error
The uncertainty in the M2 combined band 8 source counts, being the statistical 1-sigma error in the total source counts of the detection, as derived by the SAS task emldetect.

EP_8_Det_ML
The EPIC combined band detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain. To calculate the maximum likelihood values for the combined band 8 and EPIC the sum of the individual likelihoods is being normalized to two degrees of freedom using the function ML_corr = gammaq (ndof/2, ML), where ndof = 2 (for xpos,ypos) + N_images for point sources, ndof = 3 (for xpos,ypos,extent) + N_images for extended sources, gammaq = - ln (Q(a,x)) = - ln (1 - P(a,x)), and P is the incomplete gamma function.

EP_9_Det_ML
The EPIC band 9 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

PN_1_Det_ML
The PN band 1 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

PN_2_Det_ML
The PN band 2 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

PN_3_Det_ML
The PN band 3 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

PN_4_Det_ML
The PN band 4 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

PN_5_Det_ML
The PN band 5 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

PN_8_Det_ML
The PN combined band 8 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

PN_9_Det_ML
The PN band 9 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M1_1_Det_ML
The M1 band 1 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M1_2_Det_ML
The M1 band 2 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M1_3_Det_ML
The M1 band 3 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M1_4_Det_ML
The M1 band 4 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M1_5_Det_ML
The M1 band 5 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M1_8_Det_ML
The M1 combined band 8 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M1_9_Det_ML
The M1 band 9 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M2_1_Det_ML
The M2 band 1 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M2_2_Det_ML
The M2 band 2 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M2_3_Det_ML
The M2 band 3 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M2_4_Det_ML
The M2 band 4 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M2_5_Det_ML
The M2 band 5 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M2_8_Det_ML
The M2 combined band 8 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

M2_9_Det_ML
The M2 band 9 detection likelihood. Maximum likelihoods are derived by the SAS task emldetect. The individual-band maximum likelihood values (bands 1 - 5, 9) stand for the detection likelihood of the source, L = - ln p, where p is the probability of the detection occurring by chance. While the detection likelihood of an extended source is computed in the same way, systematic effects such as deviations between the real background and the model, have a larger effect on extended sources and thus detection likelihoods of extended sources are more uncertain.

EP_Extent
The EPIC extent radius (arcseconds). The extent radius and error as well as the extent likelihood of a source detected as extended is determined by the SAS task emldetect. It is determined by convolving a beta-model profile with the source PSF and fitting the result to the source image. Anything below 6" is considered to be a point source and the extent is set to zero. To avoid non-converging fitting an upper limit of 80" is imposed.

EP_Extent_Error
The uncertainty in the EPIC extent radius (arcseconds). The extent radius and error as well as the extent likelihood of a source detected as extended is determined by the SAS task emldetect. It is determined by convolving a beta-model profile with the source PSF and fitting the result to the source image. Anything below 6" is considered to be a point source and the extent is set to zero. To avoid non-converging fitting an upper limit of 80" is imposed.

EP_Extent_ML
The EPIC extent likelihood. The extent radius and error as well as the extent likelihood of a source detected as extended is determined by the SAS task emldetect. The extent likelihood is the likelihood of the detection being extended as given by EXTENT_ML = - ln(P), where P is the probability of the extent occurring by chance.

EP_HR1
The EPIC hardness ratio HR1 for bands 1 and 2. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

EPIC hardness ratios are calculated by the SAS task srcmatch and are averaged over all three cameras (PN, M1, M2). Note that no energy conversion factor was used and that the EPIC hardness ratios are de facto not hardness ratios but an equivalent number helpful to characterize the hardness of a source.

EP_HR1_Error
The uncertainty in the EPIC hardness ratio for bands 1 and 2. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

EP_HR2
The EPIC hardness ratio HR2 for bands 2 and 3. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

EPIC hardness ratios are calculated by the SAS task srcmatch and are averaged over all three cameras (PN, M1, M2). Note that no energy conversion factor was used and that the EPIC hardness ratios are de facto not hardness ratios but an equivalent number helpful to characterize the hardness of a source.

EP_HR2_Error
The uncertainty in the EPIC hardness ratio for bands 2 and 3. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

EP_HR3
The EPIC hardness ratio HR3 for bands 3 and 4. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

EPIC hardness ratios are calculated by the SAS task srcmatch and are averaged over all three cameras (PN, M1, M2). Note that no energy conversion factor was used and that the EPIC hardness ratios are de facto not hardness ratios but an equivalent number helpful to characterize the hardness of a source.

EP_HR3_Error
The uncertainty in the EPIC hardness ratio for bands 3 and 4. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

EP_HR4
The EPIC hardness ratio HR4 for bands 4 and 5. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

EPIC hardness ratios are calculated by the SAS task srcmatch and are averaged over all three cameras (PN, M1, M2). Note that no energy conversion factor was used and that the EPIC hardness ratios are de facto not hardness ratios but an equivalent number helpful to characterize the hardness of a source.

EP_HR4_Error
The uncertainty in the EPIC hardness ratio for bands 4 and 5. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

PN_HR1
The PN hardness ratio HR1 for bands 1 and 2. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

PN_HR1_Error
The uncertainty in the PN hardness ratio for bands 1 and 2. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

PN_HR2
The PN hardness ratio HR2 for bands 2 and 3. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

PN_HR2_Error
The uncertainty in the PN hardness ratio for bands 2 and 3. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

PN_HR3
The PN hardness ratio HR3 for bands 3 and 4. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

PN_HR3_Error
The uncertainty in the PN hardness ratio for bands 3 and 4. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

PN_HR4
The PN hardness ratio HR4 for bands 4 and 5. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

PN_HR4_Error
The uncertainty in the PN hardness ratio for bands 4 and 5. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M1_HR1
The M1 hardness ratio HR1 for bands 1 and 2. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M1_HR1_Error
The uncertainty in the M1 hardness ratio for bands 1 and 2. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M1_HR2
The M1 hardness ratio HR2 for bands 2 and 3. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M1_HR2_Error
The uncertainty in the M1 hardness ratio for bands 2 and 3. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M1_HR3
The M1 hardness ratio HR3 for bands 3 and 4. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M1_HR3_Error
The uncertainty in the M1 hardness ratio for bands 3 and 4. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M1_HR4
The M1 hardness ratio HR4 for bands 4 and 5. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M1_HR4_Error
The uncertainty in the M1 hardness ratio for bands 4 and 5. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M2_HR1
The M2 hardness ratio HR1 for bands 1 and 2. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M2_HR1_Error
The uncertainty in the M2 hardness ratio for bands 1 and 2. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M2_HR2
The M2 hardness ratio HR2 for bands 2 and 3. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M2_HR2_Error
The uncertainty in the M2 hardness ratio for bands 2 and 3. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M2_HR3
The M2 hardness ratio HR3 for bands 3 and 4. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M2_HR3_Error
The uncertainty in the M2 hardness ratio for bands 3 and 4. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

M2_HR4
The M2 hardness ratio HR4 for bands 4 and 5. The hardness ratios for each camera are derived by the SAS task emldetect. They are defined as the ratio between the bands A and B:

              HR(A,B) = (band B - band A) / (band A + band B).
  

Note that in the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. In cases where the rate in both bands is zero, the hardness ratio is undefined (NULL).

There are four hardness ratios (n) using the following bands:

  HR1:	bands 1 & 2
  HR2:	bands 2 & 3
  HR3:	bands 3 & 4
  HR4:	bands 4 & 5
  

M2_HR4_Error
The uncertainty in the M2 hardness ratio for bands 4 and 5. Errors are the 1-sigma error on the hardness ratio 1 as derived by the SAS task emldetect.

PN_1_Exposure
The PN band 1 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

PN_2_Exposure
The PN band 2 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

PN_3_Exposure
The PN band 3 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

PN_4_Exposure
The PN band 4 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

PN_5_Exposure
The PN band 5 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M1_1_Exposure
The M1 band 1 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M1_2_Exposure
The M1 band 2 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M1_3_Exposure
The M1 band 3 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M1_4_Exposure
The M1 band 4 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M1_5_Exposure
The M1 band 5 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M2_1_Exposure
The M2 band 1 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M2_2_Exposure
The M2 band 2 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M2_3_Exposure
The M2 band 3 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M2_4_Exposure
The M2 band 4 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

M2_5_Exposure
The M2 band 5 exposure map value (s). The exposure maps are made by the SAS task eexpmap; they combine the mirror vignetting, detector efficiency, bad pixels and CCD gaps. The exposure map values in the catalog are given in seconds and are derived by the SAS task emldetect as the PSF weighted mean of the area of the sub-images (radius 60 arcseconds) in the individual-band exposure maps.

PN_1_Bg
The PN band 1 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

PN_2_Bg
The PN band 2 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

PN_3_Bg
The PN band 3 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

PN_4_Bg
The PN band 4 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

PN_5_Bg
The PN band 5 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M1_1_Bg
The M1 band 1 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M1_2_Bg
The M1 band 2 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M1_3_Bg
The M1 band 3 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M1_4_Bg
The M1 band 4 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M1_5_Bg
The M1 band 5 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M2_1_Bg
The M2 band 1 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M2_2_Bg
The M2 band 2 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M2_3_Bg
The M2 band 3 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M2_4_Bg
The M2 band 4 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

M2_5_Bg
The M2 band 5 background map value (ct/pixel). The background maps are made by the SAS task esplinemap; they are made using a 12 x 12 nodes spline fit on the source-free individual-band images. The background map values in the catalog are given in counts per pixel and are derived by the SAS task emldetect as the background map value at the given detection position. Note that the source fitting routine uses the background map itself rather than the single value given here. The value is zero if the detection position lies outside the FOV.

PN_1_Vig
The PN band 1 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

PN_2_Vig
The PN band 2 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

PN_3_Vig
The PN band 3 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

PN_4_Vig
The PN band 4 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

PN_5_Vig
The PN band 5 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M1_1_Vig
The M1 band 1 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M1_2_Vig
The M1 band 2 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M1_3_Vig
The M1 band 3 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M1_4_Vig
The M1 band 4 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M1_5_Vig
The M1 band 5 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M2_1_Vig
The M2 band 1 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M2_2_Vig
The M2 band 2 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M2_3_Vig
The M2 band 3 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M2_4_Vig
The M2 band 4 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

M2_5_Vig
The M2 band 5 vignetting value. The vignetting values in the catalog are derived by the SAS task emldetect; they are a function of energy band and off-axis angle. (Vignetting values used in the source parametrization come from the vignetted exposure maps.)

PN_Ontime
The PN total good exposure time after GTI filtering, in seconds, of the CCD where the detection is positioned. Note that some source positions fall into CCD gaps or outside of the detector and will have therefore a NULL given.

M1_Ontime
The M1 total good exposure time after GTI filtering, in seconds, of the CCD where the detection is positioned. Note that some source positions fall into CCD gaps or outside of the detector and will have therefore a NULL given.

M2_Ontime
The M2 total good exposure time after GTI filtering, in seconds, of the CCD where the detection is positioned. Note that some source positions fall into CCD gaps or outside of the detector and will have therefore a NULL given.

EP_Ontime
The largest total good exposure time after GTI filtering, in seconds, of any of the individual cameras used.

PN_Offax
The distance between the detection position and the on-axis position on the PN detector, in arcminutes. Note that the off-axis angle for a camera can be larger than 15 arcminutes when the detection is located outside the FOV of that camera.

M1_Offax
The distance between the detection position and the on-axis position on the M1 detector, in arcminutes. Note that the off-axis angle for a camera can be larger than 15 arcminutes when the detection is located outside the FOV of that camera.

M2_Offax
The distance between the detection position and the on-axis position on the M2 detector, in arcminutes. Note that the off-axis angle for a camera can be larger than 15 arcminutes when the detection is located outside the FOV of that camera.

EP_Offax
The smallest off-axis angle (the angular distance between the detection position and the on-axis direction) of the individual camera values, in arcminutes.

PN_Maskfrac
The PSF weighted mean of the PN detector coverage of a detection as derived from the detection mask. It depends slightly on energy; only band 8 values are given here which are the minimum of the energy-dependent maskfrac values. Sources which have less than 0.15 of their PSF covered by the detector are considered as being not detected.

M1_Maskfrac
The PSF weighted mean of the M1 detector coverage of a detection as derived from the detection mask. It depends slightly on energy; only band 8 values are given here which are the minimum of the energy-dependent maskfrac values. Sources which have less than 0.15 of their PSF covered by the detector are considered as being not detected.

M2_Maskfrac
The PSF weighted mean of the M2 detector coverage of a detection as derived from the detection mask. It depends slightly on energy; only band 8 values are given here which are the minimum of the energy-dependent maskfrac values. Sources which have less than 0.15 of their PSF covered by the detector are considered as being not detected.

Dist_NN
The distance to the nearest neighbor detection, in arcseconds; it is derived by the SAS task emldetect. Emldetect uses an internal threshold of 6 arcseconds (before positional fitting) for splitting a source into two.

Sum_Flag
The summary flag of the source, derived from the EPIC flag (EP_FLAG). It is 0 if none of the nine flags was set; it is set to 1 if at least one of the warning flags (flag 1, 2, 3, 9) was set but no possible-spurious-detection flag (flag 7, 8); it is set to 2 if at least one of the possible-spurious-detection flags (flag 7, 8) was set but not the manual flag (flag 11); it is set to 3 if the manual flag (flag 11) was set but no possible-spurious-detection flags (flag 7, 8); it is set to 4 if the manual flag (flag 11) as well as one of the possible-spurious-detection flags (flag 7, 8) is set. The meaning is thus:

  0 = good
  1 = source parameters may be affected
  2 = possibly spurious
  3 = located in a area where spurious detection may occur
  4 = located in a area where spurious detection may occur and possibly spurious
  
For details see Sec. 3.2.7 of the UG, but note that flag 12 is no longer used in 3XMM-DR4.

EP_Flag
The EPIC flag string made of the flags 1 - 12 (counted from left to right): it combines the flags in each camera (PN_FLAG, M1_FLAG, M2_FLAG), that is, a flag is set in EP_FLAG if at least one of the camera-dependent flags is set.

PN_Flag
The PN flag string made of the flags 1 - 12 (counted from left to right) for the PN source detection. A flag is set to True according to the conditions summarized in Tab. 3.3a of the 2XMM Users Guide for the automatic flags, and in Tab. 3.3b of the 2XMM Users Guide for the manual flags. In cases where the camera was not used in the source detection, a dash is given. In cases where a source was not detected by the PN, the flags are all set to False (default).

M1_Flag
The M1 flag string made of the flags 1 - 12 (counted from left to right) for the M1 source detection. A flag is set to True according to the conditions summarized in Tab. 3.3a of the 2XMM Users Guide for the automatic flags, and Tab. 3.3b of the 2XMM Users Guide for the manual flags. In cases where the camera was not used in the source detection, a dash is given. In cases where a source was not detected by the M1, the flags are all set to False (default).

M2_Flag
The M2 flag string made of the flags 1 - 12 (counted from left to right) for the M2 source detection. A flag is set to True according to the conditions summarized in Tab. 3.3a of the 2XMM Users Guide for the automatic flags, and Tab. 3.3b of the 2XMM Users Guide for the manual flags. In cases where the camera was not used in the source detection, a dash is given. In cases where a source was not detected by the M2, the flags are all set to False (default).

Tseries_Flag
This flag is set to T(rue) to indicate that the source has a time series made in at least one exposure (see Sec. 3.6 of the UG).

Spectra_Flag
This flag is set to T(rue) to indicate that the source has a spectrum made in at least one exposure (see Sec. 3.6 of the UG).

EP_Chi2prob
The chi2 probability (based on the null hypothesis) that the source, as detected by any of the cameras, is constant. The minimum value of the available camera probabilities (PN_CHI2PROB, M1_CHI2PROB, M2_CHI2PROB) is given.

PN_Chi2prob
The chi2 probability (based on the null hypothesis) that the source as detected by the PN camera is constant. The Pearson's approximation to chi2 for Poissonian data was used, in which the model is used as the estimator of its own variance (see the documentation of ekstest for a more detailed description). If more than one exposure (that is, time series) is available for this source the smallest value of probability was used. See Sec. 3.1.4 of the UG for more details.

M1_Chi2prob
The chi2 probability (based on the null hypothesis) that the source as detected by the M1 camera is constant. The Pearson's approximation to chi2 for Poissonian data was used, in which the model is used as the estimator of its own variance (see the documentation of ekstest for a more detailed description). If more than one exposure (that is, time series) is available for this source the smallest value of probability was used. See Sec. 3.1.4 of the UG for more details.

M2_Chi2prob
The chi2 probability (based on the null hypothesis) that the source as detected by the M2 camera is constant. The Pearson's approximation to chi2 for Poissonian data was used, in which the model is used as the estimator of its own variance (see the documentation of ekstest for a more detailed description). If more than one exposure (that is, time series) is available for this source the smallest value of probability was used. See Sec. 3.1.4 of the UG for more details.

PN_Fvar
The fractional excess variance measured in the PN timeseries of the detection. Where multiple PN exposures exist, it is for the one giving the largest probability of variability (PN_CHI2PROB). This quantity provides a measure of the amplitude of variability in the timeseries, above purely statistical fluctuations. See Sec. 3.9 of the UG for more details.

PN_Fvar_Error
The error on the fractional excess variance for the PN timeseries of the detection (PN_FVAR). See Sec. 3.9 of the UG for more details.

M1_Fvar
The fractional excess variance measured in the MOS1 timeseries of the detection. Where multiple MOS1 exposures exist, it is for the one giving the largest probability of variability (M1_CHI2PROB). This quantity provides a measure of the amplitude of variability in the timeseries, above purely statistical fluctuations. See Sec. 3.9 of the UG for more details.

M1_Fvar_Error
The error on the fractional excess variance for the MOS1 timeseries of the detection (M1_FVAR). See Sec. 3.9 of the UG for more details.

M2_Fvar
The fractional excess variance measured in the MOS2 timeseries of the detection. Where multiple MOS2 exposures exist, it is for the one giving the largest probability of variability (M2_CHI2PROB). This quantity provides a measure of the amplitude of variability in the timeseries, above purely statistical fluctuations. See Sec. 3.9 of the UG for more details.

M2_Fvar_Error
The error on the fractional excess variance for the MOS2 timeseries of the detection (M2_FVAR). See Sec. 3.9 of the UG for more details.

Var_Flag
This flag is set to T(rue) if the source was detected as variable (chi2 probability < 1E-5, see PN_CHI2PROB, M1_CHI2PROB, M2_CHI2PROB) in at least one exposure, to F(alse) if the source was tested for variability but did not qualify as such, or to N(ull) if there was no timeseries file for the given detection. See Sec. 3.2.8 of the UG for more details.

Var_Exp_ID
If the source is detected as variable (that is, if VAR_FLAG is set to T(rue)), the exposure ID ('S' or 'U' followed by a three-digit number) of the exposure with the smallest chi2 probability is given here.

Var_Inst_ID
If the source is detected as variable (that is, if VAR_FLAG is set to T(rue)), the instrument ID (PN, M1, M2) of the exposure given in VAR_EXP_ID is listed here.

SC_RA
The mean Right Ascension in the selected equinox of all detections of the source SRCID, weighted by the positional errors POSERR (called error_radius in this table) values. This was given in J2000.0 decimal degrees in the original table.

SC_Dec
The mean Declination in the selected equinox of all detections of the source SRCID, weighted by the positional errors POSERR (called error_radius in this table) values. This was given in J2000.0 decimal degrees in the original table.

SC_Poserr
The error of the weighted mean position given in SC_RA and SC_DEC, in arcseconds.

SC_Det_ML
The total band detection likelihood of the source SRCID, i.e., the maximum of the likelihoods of all detections of this source (EP_8_DET_ML).

SC_Ep_1_Flux
The mean band 1 flux (0.2 - 0.5 keV) of all the detections of the source SRCID (see EP_1_FLUX) weighted by the errors (EP_1_FLUX_ERROR), in erg/cm2/s.

SC_Ep_1_Flux_Error
The error in the weighted mean band 1 flux, in erg/cm2/s

SC_Ep_2_Flux
The mean band 2 flux (0.5 - 1.0 keV) of all the detections of the source SRCID (see EP_2_FLUX) weighted by the errors (EP_2_FLUX_ERROR), in erg/cm2/s.

SC_Ep_2_Flux_Error
The error in the weighted mean band 2 flux, in erg/cm2/s

SC_Ep_3_Flux
The mean band 3 flux (1.0 - 2.0 keV) of all the detections of the source SRCID (see EP_3_FLUX) weighted by the errors (EP_3_FLUX_ERROR), in erg/cm2/s.

SC_Ep_3_Flux_Error
The error in the weighted mean band 3 flux, in erg/cm2/s

SC_Ep_4_Flux
The mean band 4 flux (2.0 - 4.5 keV) of all the detections of the source SRCID (see EP_4_FLUX) weighted by the errors (EP_4_FLUX_ERROR), in erg/cm2/s.

SC_Ep_4_Flux_Error
The error in the weighted mean band 4 flux, in erg/cm2/s

SC_Ep_5_Flux
The mean band 5 flux (4.5 - 12.0 keV) of all the detections of the source SRCID (see EP_5_FLUX) weighted by the errors (EP_5_FLUX_ERROR), in erg/cm2/s.

SC_Ep_5_Flux_Error
The error in the weighted mean band 5 flux, in erg/cm2/s

SC_Ep_8_Flux
The mean combined band flux (0.2 - 12.0 keV) of all the detections of the source SRCID (see EP_1_FLUX) weighted by the errors (EP_8_FLUX_ERROR), in erg/cm2/s.

SC_Ep_8_Flux_Error
The error in the weighted mean band 8 flux, in erg/cm2/s

SC_Ep_9_Flux
The mean band 9 flux (0.5 - 4.5keV) of all the detections of the source SRCID (see EP_9_FLUX) weighted by the errors (EP_9_FLUX_ERROR), in erg/cm2/s.

SC_Ep_9_Flux_Error
The error in the weighted mean band 9 flux, in erg/cm2/s

SC_HR1
The mean hardness ratio of the bands 1 and 2 of all the detections of the Source SRCID (EP_HR1) weighted by the errors.

SC_HR1_Error
The error in the weighted mean hardness ratio of bands 1 and 2 of all the detections.

SC_HR2
The mean hardness ratio of the bands 2 and 3 of all the detections of the source SRCID (EP_HR2) weighted by the errors.

SC_HR2_Error
The error in the weighted mean hardness ratio of bands 2 and 3 of all the detections.

SC_HR3
The mean hardness ratio of the bands 3 and 4 of all the detections of the source SRCID (EP_HR3) weighted by the errors.

SC_HR3_Error
The error in the weighted mean hardness ratio of bands 3 and 4 of all the detections.

SC_HR4
The mean hardness ratio of the bands 4 and 5 of all the detections of the source SRCID (EP_HR4) weighted by the errors.

SC_HR4_Error
The error in the weighted mean hardness ratio of bands 4 and 5 of all the detections.

SC_Extent
The total band extent, i.e., the weighted average of the EPIC extents in the total band of all the detections of the source, in arcseconds.

SC_Ext_ML
The total band detection likelihood of the extended source SRCID, i.e., the largest of the extent likelihoods of all detections of this source.

SC_Chi2prob
The chi2 probability (based on the null hypothesis) that the unique source SRCID as detected by any of the observations is constant, that is, the minimum value of the EPIC probabilities in each detection, EP_CHI2PROB, is given.

SC_Fvar
The fractional excess variance of the unique source. It is the value corresponding to the exposure and instrument that shows the lowest probability of being constant (i.e. it is the PN_FVAR, M1_FVAR or M2_FVAR value corresponding to EP_CHI2PROB, SC_CHI2PROB.

SC_Fvar_Error
The error on the fractional excess variance of the unique source. It is the value corresponding to the exposure and instrument that shows the lowest probability of being constant (i.e. it is the PN_FVARERR, M1_FVARERR or M2_FVARERR value corresponding to EP_CHI2PROB, SC_CHI2PROB.

SC_Var_Flag
The variability flag for the unique source SRCID which is set to the value of VAR_FLAG for the most variable detection of this source.

SC_Sum_Flag
The summary flag for the unique source SRCID is taken to be the worst flag of all detections of this source (SUM_FLAG).

SC_Ep_8_Fmin
The minimum EPIC band 8 flux (EP_8_FLUX), in erg/cm2/s, among any of the constituent detections of the unique source.

SC_Ep_8_Fmin_Error
The error on the minimum EPIC band 8 flux (EP_8_FLUX_ERR), in erg/cm2/s, among any of the constituent detections of the unique source.

SC_Ep_8_Fmax
The maximum EPIC band 8 flux (EP_8_FLUX), in erg/cm2/s, among any of the constituent detections of the unique source.

SC_Ep_8_Fmax_Error
The error on the maximum EPIC band 8 flux (EP_8_FLUX_ERR), in erg/cm2/s, among any of the constituent detections of the unique source.

Obs_First
The start date of the earliest observation of any constituent detection of the unique source.

Obs_Last
The end date of the last observation of any constituent detection of the unique source.

N_Detections
The number of detections of the unique source SRCID used to derive the combined values.

Confused_Flag
This flag parameter is normally set to (F)alse, but is set to (T)rue when a given detection has a probability above zero of being associated with two or more distinct sources. The SRCID is that of the match with the highest probability, but there remains some uncertainty about which source is the correct match for the detection.

High_Background_Flag
This flag parameter is set to T(rue) if this detection comes from a field which, during manual screening, was considered to have a high background level which notably impacted on source detection (see Sec. 6.1.2 of the UG).


Contact Person

Questions regarding the XMMSSC database table can be addressed to the HEASARC User Hotline.

Page Author: Browse Software Development Team
Last Modified: 4-Sep-2013