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TAURUSXMM - Taurus Molecular Cloud XMM-Newton X-Ray Source Catalog

HEASARC
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Overview

The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST) surveys the most populated ~5 square degrees of the Taurus Molecular Cloud, using the XMM-Newton X-ray observatory to study the thermal structure, variability, and long-term evolution of hot plasma, to investigate the magnetic dynamo, and to search for new potential members of the association. The authors present overall correlations with fundamental stellar parameters that were derived from the previous literature. The present overview paper introduces the project and provides the basic results from the X-ray analysis of all sources detected in the XEST survey. Comprehensive tables in the published paper summarize the stellar properties of all the targets surveyed. The survey goes deeper than previous X-ray surveys of Taurus by about an order of magnitude and for the first time systematically accesses very faint and strongly absorbed TMC objects. The authors find a detection rate of 85% and 98% for classical and weak-line T Tauri stars (CTTS and WTTS), respectively, and identify about half of the surveyed protostars and brown dwarfs. Overall, 136 out of 169 surveyed stellar systems were detected. The authors describe an X-ray luminosity vs. mass correlation, discuss the distribution of X-ray-to-bolometric luminosity ratios, and show evidence for lower X-ray luminosities in CTTS compared to WTTS.

The complete catalog of all X-ray sources (stellar and non-stellar) detected in the 28 XEST fields is presented in this table. The catalog provides X-ray coordinates, their uncertainties, X-ray count rates and their uncertainties, and X-ray hardness ratios for 2347 detected X-ray sources. If two XEST fields overlap, the same sources may have been identified twice, with different XEST IDs assigned, notice.


Catalog Bibcode

2007A&A...468..353G

References

The XMM-Newton Extended Survey of the Taurus Molecular Cloud.
    Guedel M., Briggs K.R., Arzner K., Audard M., Bouvier J., Feigelson E.D.,
    Franciosini E., Glauser A., Grosso N., Micela G., Monin J.-L.,
    Montmerle T., Padgett D.L., Palla F., Pillitteri I., Rebull L.,
    Scelsi L., Silva B., Skinner S.L., Stelzer B., Telleschi A.
    <Astron. Astrophys. 468, 353 (2007)>
    =2007A&A...468..353G        (SIMBAD/NED BibCode)

Provenance

This table was created by the HEASARC in July 2007 based on the CDS Catalog J/A+A/468/353 file table14.dat.

Parameters

Source_Number
A running X-ray source number in order of increasing J2000.0 Right Ascension for the entire XEST catalog.

Alt_Name
The alternate name for the X-ray source using the '[GBA2007]' prefix (for Guedel, Briggs, Arzner 2007) and the value of the source number parameter, as recommended by the CDS Dictionary of Nomenclature of Celestial Objects.

Xest_Field
The XEST field number in which the X-ray source was detected. This is also used as the first numerical field in the source name: e.g., the source 'XEST 27-020' was detected in XEST field number 27. The full details of the 28 fields (separate XMM-Newton pointings) are given in Table 1 of the reference paper.

Field_Source_Number
The XEST source number of the X-ray source within the field in which the source was detected. This is a running X-ray source number in order of increasing J2000.0 Right Ascension within the field. This parameter is also used as the second numerical field in the source name: e.g., the source 'XEST 27-020' is the 20th source in order of increasing RA in XEST field number 27.

Name
The preferred designation for the X-ray source using the 'XEST' prefix (for XMM-Newton Extended Survey of the Taurus molecular cloud), the XEST field number, and the running source number within the field, as registered with the CDS Dictionary of Nomenclature of Celestial Objects. Thus, the source 'XEST 27-020' is the 20th source in order of increasing RA in XEST field number 27.

RA
The Right Ascension of the X-ray source in the selected equinox corrected for boresight shift as discussed in Section 4.7 of the reference paper. The RA was given in J2000.0 coordinates to a precision of 0.01 seconds of time in the original table.

Dec
The Declination of the X-ray source in the selected equinox corrected for boresight shift as discussed in Section 4.7 of the reference paper. The Declination was given in J2000.0 coordinates to a precision of 0.1 arcseconds in the original table.

LII
The Galactic Longitude of the X-ray source.

BII
The Galactic Latitude of the X-ray source.

Error_Radius
The one-sigma positional error of the X-ray source, in arcseconds, including the rms error in the boresight shift.

Detect_Likelihood
The maximum likelihood ML_F of the X-ray source detection in the mosaicked EPIC full-band (0.5 - 7.3 keV) image.

Counts
The number of detected source counts in the mosaicked EPIC full-band (0.5 - 7.3 keV) image. If the full-band maximum likelihood ML_F is less than 5, then the 95% upper limit to the counts is given.

Exposure
The total PN-equivalent effective exposure time, in seconds, at the position of the X-ray source in the mosaicked EPIC full-band (0.5 - 7.3 keV) image.

Count_Rate
The PN-equivalent source count rate CR_F, in counts per second, in the mosaicked EPIC full-band (0.5 - 7.3 keV) image. If the full-band maximum likelihood ML_F is less than 5, then the 95% upper limit to the count rate is given.

Count_Rate_Error
The one-sigma statistical error in the PN-equivalent source count rate in the mosaicked EPIC full-band (0.5 - 7.3 keV) image. Note that this does not include the uncertainty in the spectrally-dependent PN/MOS sensitivity ratio.

SB_Detect_Likelihood
The maximum likelihood ML_S of the X-ray source detection in the mosaicked EPIC soft-band (0.5 - 2.0 keV) image.

SB_Counts
The number of detected source counts in the mosaicked EPIC soft-band (0.5 - 2.0 keV) image. If the soft-band maximum likelihood ML_S is less than 5, then the 95% upper limit to the counts is given.

SB_Exposure
The total PN-equivalent effective exposure time, in seconds, at the position of the X-ray source in the mosaicked EPIC soft-band (0.5 - 2.0 keV) image.

SB_Count_Rate
The PN-equivalent source count rate CR_S, in counts per second, in the mosaicked EPIC soft-band (0.5 - 2.0 keV) image. If the soft-band maximum likelihood ML_S is less than 5, then the 95% upper limit to the count rate is given.

SB_Count_Rate_Error
The one-sigma statistical error in the PN-equivalent source count rate in the mosaicked EPIC soft-band (0.5 - 2.0 keV) image. Note that this does not include the uncertainty in the spectrally-dependent PN/MOS sensitivity ratio.

HB_Detect_Likelihood
The maximum likelihood ML_H of the X-ray source detection in the mosaicked EPIC hard-band (2.0 - 7.3 keV) image.

HB_Counts
The number of detected source counts in the mosaicked EPIC hard-band (2.0 - 7.3 keV) image. If the hard-band maximum likelihood ML_H is less than 5, then the 95% upper limit to the counts is given.

HB_Exposure
The total PN-equivalent effective exposure time, in seconds, at the position of the X-ray source in the mosaicked EPIC hard-band (2.0 - 7.3 keV) image.

HB_Count_Rate
The PN-equivalent source count rate CR_H, in counts per second, in the mosaicked EPIC hard-band (2.0 - 7.3 keV) image. If the hard-band maximum likelihood ML_H is less than 5, then the 95% upper limit to the count rate is given.

HB_Count_Rate_Error
The one-sigma statistical error in the PN-equivalent source count rate in the mosaicked EPIC hard-band (2.0 - 7.3 keV) image. Note that this does not include the uncertainty in the spectrally-dependent PN/MOS sensitivity ratio.

Hardness_Ratio
The hardness ratio HR defined in the standard way, viz., HR = (CR_H - CR_S)/(CR_F), where CR_H, CR_S and CR_F are the source count rates in the hard, soft and full bands, respectively. If an object was not detected in the soft (hard) band, then the quoted hardness ratio is an upper (lower) limit. If object is detected only in the full band, then HR was set to 0.

Hardness_Ratio_Min
The 1-sigma lower limit to the hardness ratio HR, i.e., HR - e_HR, where e_HR is the negative uncertainty.

Hardness_Ratio_Max
The 1-sigma upper limit to the hardness ratio HR, i.e., HR + e_HR, where e_HR is the positive uncertainty.

Comments
Comments concerning the by-eye verification of the X-ray source.


Contact Person

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

Page Author: Browse Software Development Team
Last Modified: 31-Jul-2007