M83XMM - M 83 XMM-Newton X-Ray Point Source Catalog

Overview

This database table contains results obtained from the analysis of three XMM-Newton observations of the grand-design barred spiral galaxy M 83. The aims of this study were to study the X-ray source populations in M 83 and to calculate the X-ray luminosity functions of X-ray binaries for different regions of the galaxy.

The authors detected 189 sources in the XMM-Newton field of view in the energy range of 0.2-12 keV. They constrained their nature by means of spectral analysis, hardness ratios, studies of the X-ray variability, and cross-correlations with catalogs in X-ray, optical, infrared, and radio wavelengths.

The authors identified and classified 12 background objects, five foreground stars, two X-ray binaries, one supernova remnant candidate, one super-soft source candidate and one ultra-luminous X-ray source. Among these sources, they classified for the first time three active galactic nuclei (AGN) candidates. the authors derived X-ray luminosity functions for the X-ray sources in M 83 in the 2-10 keV energy range, within and outside the D₂₅ ellipse, correcting the total X-ray luminosity function for incompleteness and subtracting the AGN contribution. The X-ray luminosity function inside the D25 ellipse is consistent with that previously observed by Chandra. The Kolmogorov-Smirnov test shows that the X-ray luminosity function of the outer disc and the AGN luminosity distribution are uncorrelated with a probability of ~99.3%. The authors also found that the X-ray sources detected outside the D₂₅ ellipse and the uniform spatial distribution of AGNs are spatially uncorrelated with a significance of 99.5%. They interpret these results as an indication that part of the observed X-ray sources are X-ray binaries in the outer disc of M 83.

The authors analyzed the public archival XMM-Newton data of M 83 (PIs: Watson, Kuntz). Three observations were analyzed, one pointing at the center of the galaxy (obs.1) and two in the south, which covered the outer arms with a young population of stars discovered with GALEX. The details of these observations are given in Table 1 of the reference paper (summarized below):

                                                   EPIC   EPIC   EPIC
  No  ObsID      Date         RA           DE       PN    MOS1   MOS2   Mode
                                                  F Texp F Texp F Texp PN MOS

  1 0110910201 2003-01-27 13:37:05.16 -29:51:46.1 t 21.2 m 24.6 m 24.6 EFF FF
  2 0503230101 2008-01-16 13:37:01.09 -30:03:49.9 m 15.4 m 19.0 m 19.0 EFF FF
  3 0552080101 2008-08-16 13:36:50.87 -30:03:55.2 m 25.0 m 28.8 m 28.8 EFF FF

where F is the filter (t for thin, m for medium), T_exp is the exposure time in ks, EFF = extended full frame imaging mode, and FF = full frame imaging mode.

Catalog Bibcode

2013A&A...553A...7D

References

X-ray source population study of the starburst galaxy M 83 with XMM-Newton.
    Ducci L., Sasaki M., Haberl F., Pietsch and W.
    <Astron. Astrophys. 553, A7 (2013)>
    =2013A&A...553A...7D        (SIMBAD/NED BibCode)

Provenance

This table was created by the HEASARC in April 2013 based on CDS Catalog J/A+A/553/A7 files tableb1.dat and tableb2.dat.

Parameters

Source_Number
A unique identification number for each XMM-Newton X-ray source in this table in order of increasing J2000.0 Right Ascension.

Name
The X-ray source designation invented by the HEASARC, in the style recommended by the CDS Dictionary of Nomenclature of Celestial Objects, using the '[DSH2013]' prefix (for Ducci, Sasaki, Haberl 2013) and the source number.

RA
The Right Ascension of the XMM-Newton X-ray source in the selected equinox. This was given in J2000.0 sexagesimal coordinates to a precision of 0.01 seconds of time in the original table. These coordinates were astrometrically corrected by comparing the original X-ray positions with the USNO-B1 positions of 5 X-ray emitting foreground star candidates, resulting in a systematic correction Delta_RA of -2.02 +/- 0,43 arcseconds.

Dec
The Declination of the XMM-Newton X-ray source in the selected equinox. This was given in J2000.0 sexagesimal coordinates to a precision of 0.1 arcseconds in the original table. These coordinates were astrometrically corrected by comparing the original X-ray positions with the USNO-B1 positions of 5 X-ray emitting foreground star candidates, resulting in a systematic correction Delta_Dec of -0.44 +/- 0,43 arcseconds.

LII
The Galactic Longitude of the XMM-Newton X-ray source.

BII
The Galactic Latitude of the XMM-Newton X-ray source.

Error_Radius
The positional uncertainty of the XMM-Newton X-ray source position, in arcseconds.

Count_Rate_1
The combined (PN + MOS1 + MOS2) count rate of the XMM-Newton X-ray source in the first observation in the 0.2-12 keV band, in ct/s.

Count_Rate_1_Error
The uncertainty in the combined (PN + MOS1 + MOS2) count rate of the XMM-Newton X-ray source in the first observation, in the 0.2-12 keV band, in ct/s.

Count_Rate_2
The combined (PN + MOS1 + MOS2) count rate of the XMM-Newton X-ray source in the second observation, in the 0.2-12 keV band, in ct/s.

Count_Rate_2_Error
The uncertainty in the combined (PN + MOS1 + MOS2) count rate of the XMM-Newton X-ray source in the second observation, in the 0.2-12 keV band, in ct/s.

Count_Rate_3
The combined (PN + MOS1 + MOS2) count rate of the XMM-Newton X-ray source in the third observation, in the 0.2-12 keV band, in ct/s.

Count_Rate_3_Error
The uncertainty in the combined (PN + MOS1 + MOS2) count rate of the XMM-Newton X-ray source in the third observation, in the 0.2-12 keV band, in ct/s.

Detect_Likelihood_1
The detection likelihood L of the XMM-Newton X-ray source in the first observation, defined by the relationship L = - ln(p), where p is the probability that a Poissonian fluctuation in the background is detected as a spurious source.

Detect_Likelihood_2
The detection likelihood L of the XMM-Newton X-ray source in the second observation, defined by the relationship L = - ln(p), where p is the probability that a Poissonian fluctuation in the background is detected as a spurious source.

Detect_Likelihood_3
The detection likelihood L of the XMM-Newton X-ray source in the third observation, defined by the relationship L = - ln(p), where p is the probability that a Poissonian fluctuation in the background is detected as a spurious source.

Hardness_Ratio_1
The hardness ratio HR1 = (R2-R1)/(R2+R1) of the XMM-Newton X-ray source in the observation in which the highest number of counts was detected, where R1 is the combined (PN + MOS1 + MOS2) count rate in the 0.2-0.5 keV band and R2 is the combined (PN + MOS1 + MOS2) count rate in the 0.5-1.0 keV band.

Hardness_Ratio_1_Error
The uncertainty in the hardness ration HR1 of the XMM-Newton X-ray source.

Hardness_Ratio_2
The hardness ratio HR2 = (R3-R2)/(R3+R2) of the XMM-Newton X-ray source in the observation in which the highest number of counts was detected, where R2 is the combined (PN + MOS1 + MOS2) count rate in the 0.5-1.0 keV band and R3 is the combined (PN + MOS1 + MOS2) count rate in the 1.0-2.0 keV band.

Hardness_Ratio_2_Error
The uncertainty in the hardness ration HR2 of the XMM-Newton X-ray source.

Hardness_Ratio_3
The hardness ratio HR3 = (R4-R3)/(R4+R3) of the XMM-Newton X-ray source in the observation in which the highest number of counts was detected, where R3 is the combined (PN + MOS1 + MOS2) count rate in the 1.0-2.0 keV band and R4 is the combined (PN + MOS1 + MOS2) count rate in the 2.0-4.5 keV band.

Hardness_Ratio_3_Error
The uncertainty in the hardness ration HR3 of the XMM-Newton X-ray source.

Hardness_Ratio_4
The hardness ratio HR4 = (R5-R4)/(R5+R4) of the XMM-Newton X-ray source in the observation in which the highest number of counts was detected, where R4 is the combined (PN + MOS1 + MOS2) count rate in the 2.0-4.5 keV band and R5 is the combined (PN + MOS1 + MOS2) count rate in the 4.5-12 keV band.

Hardness_Ratio_4_Error
The uncertainty in the hardness ration HR4 of the XMM-Newton X-ray source.

USNOB1_Name
The proposed USNO-B1 identification for the XMM-Newton X-ray source.

USNOB1_Name_Match
This flag parameter indicates the grade (quality) for the USNO-B1 match to the X-ray source position. For each counterpart, the authors assigned a "grade" A, B, or C if the positions of the X-ray source and its counterpart are closer than 1 x, 2 x, or 3 x the combined statistical positional errors, respectively. The optical counterparts of several X-ray sources could not be determined uniquely. In such cases the authors assumed that the counterpart is the brightest optical object within the error circle.

TwoMASS_Name
The proposed 2MASS identification for the XMM-Newton X-ray source.

TwoMASS_Name_Match
This flag parameter indicates the grade (quality) for the 2MASS match to the X-ray source position. For each counterpart, the authors assigned a "grade" A, B, or C if the positions of the X-ray source and its counterpart are closer than 1 x, 2 x, or 3 x the combined statistical positional errors, respectively.

Optical_Name
The proposed optical identification for the XMM-Newton X-ray source. The CDS notes that the naming convention used for some of these names is different from that used in SIMBAD:

              [BL2004] 53 = [BL2004b] SNR 53 in SIMBAD,
              [BRK2009] 7 = [BRK2009] Background G 7 in SIMBAD
  	    [CRB1994] N = [CB85] N in SIMBAD

The optical counterparts of several X-ray sources could not be determined uniquely. In such cases the authors assumed that the counterpart is the brightest optical object within the error circle.

Optical_Name_Match
This flag parameter indicates the grade (quality) for the optical source match to the X-ray source position. For each counterpart, the authors assigned a "grade" A, B, or C if the positions of the X-ray source and its counterpart are closer than 1 x, 2 x, or 3 x the combined statistical positional errors, respectively.

Radio_Matches
The proposed radio identification(s) and their corresponding match grade(s) for the XMM-Newton X-ray source. For each counterpart, the authors assigned a "grade" A, B, or C if the positions of the X-ray source and its counterpart are closer than 1 x, 2 x, or 3 x the combined statistical positional errors, respectively.

Xray_Matches
Previous X-ray identification(s), the present authors' corresponding match grade(s) and (in some cases) the previously proposed classifications for the source. For each counterpart, the authors assigned a "grade" A, B, or C if the positions of the X-ray source and its counterpart are closer than 1 x, 2 x, or 3 x the combined statistical positional errors, respectively. Previous X-ray detections of some of these sources were reported by ROSAT (Ehle et al. 1998, A&A, 329, 39: [E1998] = [EPB98] NN in SIMBAD); Immler et al. (1999, A&A, 352, 415: [I1999] = [IVE99] HNN in SIMBAD), Einstein (Trinchieri et al. 1985, ApJ, 290, 96: [T1985] = [TFP85] HN in SIMBAD), and Chandra (Soria & Wu, 2003, A&A, 410, 53: [SW2003]). Some XMM-Newton X-ray sources have multiple previous X-ray matches, notice.

Broad_Type
The classification of the source. The authors used previous classifications in X-rays and other wavelengths, aw well as the methods of classification described in Sects. 4.1 (X-ray variability), 4.2 (spectral analysis), and 4.3 (hardness ratios) of the reference paper, to identify and classify sources as background objects, foreground stars, X-ray binaries (XRBs), SNRs, super-soft sources (SSSs), and ultra-luminous X-ray sources (ULXs).

Class
The HEASARC Browse object classification based on the value of the broad_type parameter.

Contact Person

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Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:30:47 EDT