M33SNRXMM - M 33 XMM-Newton Supernova Remnants Catalog

Overview

The authors of this catalog carried out a study of the X-ray properties of the supernova remnant (SNR) population in M 33 with XMM-Newton, comprising deep observations of eight fields in M 33 covering all of the area within the D₂₅ contours, and with a typical luminosity of 7.1 x 10³⁴ erg/s (0.2-2.0keV). With their deep observations and large field of view they have detected 105 SNRs at the 3-sigma level, of which 54 SNRs are newly detected in X-rays, and three are newly discovered SNRs. Combining XMM-Newton data with deep Chandra survey data allowed detailed spectral fitting of 15 SNRs, for which they have measured temperatures, ionization time-scales and individual abundances. This large sample of SNRs allowed the authors to construct an X-ray luminosity function, and compare its shape to luminosity functions from host galaxies of differing metallicities and star formation rates to look for environmental effects on SNR properties. They concluded that while metallicity may play a role in SNR population characteristics, differing star formation histories on short time-scales, and small-scale environmental effects appear to cause more significant differences between X-ray luminosity distributions. In addition, they analyze the X-ray detectability of SNRs, and find that in M 33 SNRs with higher [SII]/H-alpha ratios, as well as those with smaller galactocentric distances, are more detectable in X-rays.

This catalog utilized data from a deep survey of M 33 using an 8 field XMM-Newton mosaic that extends out to the D25 isophote. The point source catalog from this survey was published by W15 (Williams+2015, J/ApJS/218/9). In addition to the catalog of W15, the authors utilized high-resolution observations from the Chandra ACIS Survey of M 33 (ChASeM33, Tullmann+2011, J/ApJS/193/31) for the purposes of obtaining X-ray spectral fits.

Catalog Bibcode

2017MNRAS.472..308G

References

Supernova remnants in M33: X-ray properties as observed by XMM-Newton.
    Garofali K., Williams B.F., Plucinsky P.P., Gaetz T.J., Wold B., Haberl F.,
    Long K.S., Blair W.P., Pannuti T.G., Winkler P.F., Gross J.
   <Mon. Not. R. Astron. Soc., 472, 308-333 (2017)>
   =2017MNRAS.472..308G    (SIMBAD/NED BibCode)

Provenance

This table was ingested by the HEASARC in October 2019 based upon the CDS Catalog J/MNRAS/472/308 files table2.dat and table3.dat.

Parameters

Name
The catalog-based source designation which uses "[GWP2017] " as a prefix to the source_id.

Source_ID
The unique identifier from the catalog of M 33 supernova remnants, corresponding to 3-sigma detected sources only, based on the 0.2-2keV band.

Source_Flag
The source flag contains comments concerning the specified source, coded as follows, based on a by-eye evaluation:

      c = Flux is contaminated by nearby bright X-ray source, but source has a
          previous X-ray detection. Flux is an upper limit.
      e = Unrealistic source count errors from emldetect in at least one
          individual band. Source count errors pegged to total count values.
      n = Determined to be a non-detection via by-eye catalogue checking.
          Flux is an upper limit.
      t = Total counts in the full band are discrepant by a factor of two from
          the summation of counts in each individual band due an emldetect
          merging issue. Total counts in the 0.2-2.0keV band are reported as the
          sum of counts in the 0.2-0.5, 0.5-1.0 and 1.0-2.0keV band.
      x = Flux is contaminated by nearby bright X-ray source, but source does not
          have a previous X-ray detection. Flux is an upper limit.

RA
The Right Ascension of the XMM X-ray source in the selected equinox. This parameter was given in J2000.0 equatorial coordinates to a precision of 0.01 seconds of time in the original table. The positions for all sources come from the catalogue of Williams+2015 (J/ApJS/218/9).

Dec
The Declination of the XMM X-ray source in the selected equinox. This parameter was given in J2000.0 equatorial coordinates to a precision of 0.01 seconds of time in the original table. The positions for all sources come from the catalogue of Williams+2015 (J/ApJS/218/9).

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

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

B1_Counts
The source counts in the 0.2-2.0keV band, which are used to determine detections.

B1_Counts_Error
The uncertainty in the source counts in the 0.2-2.0keV band.

B2_Counts
The source counts in the 0.35-2keV band, which are used to compare with values in Long+ 2010 (J/ApJS/187/495).

B2_Counts_Error
The uncertainty in source counts in the 0.35-2keV band.

B3_Counts
The source counts in the 0.3-0.7keV (soft) band.

B3_Counts_Error
The uncertainty in source counts in the 0.3-0.7keV (soft) band.

B4_Counts
The source counts in the 0.7-1.1keV (medium) band.

B4_Counts_Error
The uncertainty in source counts in the 0.7-1.1keV (medium) band.

B5_Counts
The source counts in the 1.1-4.2keV (hard) band.

B5_Counts_Error
The uncertainty in source counts in the 1.1-4.2keV (hard) band.

HR1
The hardness ratio in the 0.3-0.7 (S), 0.7-1.1 (M) and 1.1-4.2 keV (H) bands: HR1=(M-S)/(H+M+S)

HR1_Error
The uncertainty in the hardness ratio, HR1.

HR2
The hardness ratio in the 0.3-0.7 (S), 0.7-1.1 (M) and 1.1-4.2keV (H) bands: HR2=(H-M)/(H+M+S).

HR2_Error
The uncertainty in the hardness ratio, HR2.

HR3
The hardness ratio from the 0.2-0.5 (S) , 0.5-1.0 (M) and 1.0-2.0keV (H) bands: HR3=(M-S)/(S+M)

HR3_Error
The uncertainty in the hardness ratio, HR3.

HR4
The hardness ratio from the 0.2-0.5 (S), 0.5-1.0 (M) and 1.0-2.0keV (H) Bands: HR4=(H-M)/(H+M)

HR4_Error
The uncertainty in hardness ratio, HR4.

Detect_Flag
The measurement level in Long+ 2010 (J/ApJS/187/495): 3-sigma, 2-sigma or upper limit (<).

Alt_Name_1
The identification number in Long+ 2010 (J/ApJS/187/495).

Alt_Name_2
The identification number in Lee & Lee 2014 (J/ApJ/793/134).

B1_Flux
The flux in the 0.2-2.0keV band, in erg/s/cm².

B2_Flux
The flux in the 0.35-2.0keV band, in erg/s/cm².

Size_1
The optical SNR size, in the unit of pc, taken from Long+ 2010 (J/ApJS/187/495).

Size_2
The optical SNR size, in the unit of pc, taken from Lee & Lee 2014 (J/ApJ/793/134).

SII_Ha_Ratio_1
The [SII]/H-alpha optical emission line ratio, taken from Long+ 2010 (J/ApJS/187/495).

SII_Ha_Ratio_2
The [SII]/H-alpha optical emission line ratio, taken from Lee & Lee 2014 (J/ApJ/793/134).

Log_LHa_1
The logarithm of the H-alpha luminosity, taken from Long+ 2010 (J/ApJS/187/495), given in erg/s.

Log_LHa_2
The logarithm of the H-alpha luminosity, taken from Lee & Lee 2014 (J/ApJ/793/134), given in erg/s.

Contact Person

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Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:30:38 EDT