ACDS V10.0 - Detailed Description of J/A+A/585/A162

ACDS V10.0 - Sun Jan 19 01:56:25 CET 2025

| # Detailed Description of J/A+A/585/A162 : X-ray supernova remnants in LMC (Maggi+, 2016) |

Note : this is the description file of the original catalog. This HTML page corresponds well to the original description, but some minor changes in the format may have been introduced in the FITS output files in order to allow for arithmetic operations on quantities such as coordinates and times. h:m:s and d:m:s units are normally converted into degrees, and YYYY-MM-DD into julian days.
Similarly, some slight changes may have been introduced in the units; the value given in the HTML files supersedes the value indicated in the ReadMe file for this catalogue.

    J/A+A/585/A162      X-ray supernova remnants in LMC          (Maggi+, 2016)
    ================================================================================
    The population of X-ray supernova remnants in the Large Magellanic Cloud.
        Maggi P., Haberl F., Kavanagh P.J., Sasaki M., Bozzetto L.M.,
        Filipovic M.D., Vasilopoulos G., Pietsch W., Points S.D., Chu Y.-H.,
        Dickel J., Ehle M., Williams R., Greiner J.
       <Astron. Astrophys., 585, A162-162 (2016)>
       =2016A&A...585A.162M    (SIMBAD/NED BibCode)
    ================================================================================
    ADC_Keywords: Magellanic Clouds ; Supernova remnants ; X-ray sources

    Keywords: ISM: supernova remnants - Magellanic Clouds - ISM: abundances -
              supernovae: general - stars: formation - X-rays: ISM

    Abstract:
        We present a comprehensive X-ray study of the population of supernova
        remnants (SNRs) in the Large Magellanic Cloud (LMC). Using primarily
        XMM-Newton observations, we conduct a systematic spectral analysis of
        LMC SNRs to gain new insight into their evolution and the interplay
        with their host galaxy. We combined all the archival XMM-Newton
        observations of the LMC with those of our Very Large Programme LMC
        survey. We produced X-ray images and spectra of 51 SNRs, out of a list
        of 59 objects compiled from the literature and augmented with newly
        found objects. Using a careful modelling of the background, we
        consistently analysed all the X-ray spectra and measure temperatures,
        luminosities, and chemical compositions. The locations of SNRs are
        compared to the distributions of stars, cold gas, and warm gas in the
        LMC, and we investigated the connection between the SNRs and their
        local environment, characterised by various star formation histories.
        We tentatively typed all LMC SNRs, in order to constrain the ratio of
        core-collapse to type Ia SN rates in the LMC. We also compared the
        column densities derived from X-ray spectra to HI maps, thus probing
        the three-dimensional structure of the LMC. This work provides the
        first homogeneous catalogue of the X-ray spectral properties of SNRs
        in the LMC. It offers a complete census of LMC remnants whose X-ray
        emission exhibits Fe K lines (13% of the sample), or reveals the
        contribution from hot supernova ejecta (39%), which both give clues to
        the progenitor types. The abundances of O, Ne, Mg, Si, and Fe in the
        hot phase of the LMC interstellar medium are found to be between 0.2
        and 0.5 times the solar values with a lower abundance ratio
        [{alpha}/Fe] than in the Milky Way. The current ratio of core-collapse
        to type Ia SN rates in the LMC is constrained to
        NCC/NIa=1.35(-0.24+0.11), which is lower than in local SN
        surveys and galaxy clusters. Our comparison of the X-ray luminosity
        functions of SNRs in Local Group galaxies (LMC, SMC, M31, and M33)
        reveals an intriguing excess of bright objects in the LMC. Finally, we
        confirm that 30 Doradus and the LMC Bar are offset from the main disc
        of the LMC to the far and near sides, respectively.

    Description:
        The processing of all available XMM-Newton data in the LMC region, and
        those of the VLP survey in particular, was done with the data
        reduction pipeline developed in our research group over several years.
        Various non-X-ray data were used to supplement the XMM-Newton
        observations. They allow us to assess e.g. the relation between the
        population of SNRs and large scale structure of the LMC, or to
        evaluate doubtful candidates in the sample compilation.
        We compiled a sample of 59 definite SNRs, cleaned of misclassified
        objects and doubtful candidates.

    File Summary:

           FileName      Lrecl  Records   Explanations

    ×                   80        .   This file
    × ReadMe            80        .   This file
    × tablec1.dat      101       59   SNRs in the LMC
    × table4.dat        62       39   1T/2T SNRs with detected ejecta (D), and used
                                     for measurements of ISM composition (I)

    See also:
      B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2016)
      J/A+AS/143/391 : ROSAT HRI catalogue of LMC X-ray sources (Sasaki+, 2000)

    Byte-by-byte Description of file:  tablec1.dat

       Bytes Format Units   Label     Explanations

       1- 10  A10   ---     MCSNR     MCSNR identifier (JHHMM-DDMM)
      12- 13  I2    h       RAh       Right ascension of the remnant (J2000)
      15- 16  I2    min     RAm       Right ascension of the remnant (J2000)
      18- 19  I2    s       RAs       Right ascension of the remnant (J2000)
          21  A1    ---     DE-       Declination sign of the remnant (J2000)
      22- 23  I2    deg     DEd       Declination of the remnant (J2000)
      25- 26  I2    arcmin  DEm       Declination of the remnant (J2000)
      28- 29  I2    arcsec  DEs       Declination of the remnant (J2000)
      31- 48  A18   ---     OName     Old "common" name used in the literature
      50- 51  A2    ---     X-ray     Flag coding the type of X-ray data available
                                       and used in this work (1)
      53- 58  F6.2  10+28W  LX        ?=- X-ray luminosity in the 0.3-8keV band,
                                       in units of 1035erg/s, obtained as
                                       described in Sect. 7
      60- 65  F6.2  arcsec  XSize     X-ray size (2)
      67- 69  I3    deg     PA        ? Position angle of the maximal extent in the
                                       non-symmetric case (3)
          72  A1    ---     l_fNH     Limit flag on fNH
      73- 76  F4.2  ---     fNH       ?=- NH fraction, as defined in Sect. 8 (4)
      78- 80  I3    ---     NOB       Number of blue early-type stars within 100pc
                                       of the remnant (see Sect. 6.2)
      82- 86  F5.2  ---     r         Ratio of CC SNe to thermonuclear SNe expected
                                       from the observed distribution of stellar
                                       ages in the neighbourhood of the remnant, as
                                       obtained by Eq. (2) (see Sect. 6 for details)
      88- 90  F3.1  ---    Hint-spec  [1/5] Number attributed to SNRs as function of
                                       spectral results, as described in Sect. 6.3
                                       and Table 7 (5)
      92-101  A10   ---     Ref       Reference in which the SNR was first
                                       published (6)

    Note (1): Flag coding the type of X-ray data as follows:
         X = XMM-Newton data are present
        MX = multiple XMM-Newton observation of the remnant exist
         C = no XMM-Newton observations are available but Chandra observations
              were used
         R = no XMM-Newton observations are available but ROSAT observations
              were used
         N = no X-ray information was found
    Note (2): Only the maximal extent is given (corresponding to the diametre in a
         circularly symmetric case).
    Note (3): The PA is measured in degrees, eastwards of north. Size was measured
         from XMM-Newton images whenever applicable ("X" and "MX" flags).
         For "C" SNRs, the quoted value is taken from the entry in the Chandra SNR
         catalogue. For the ROSAT-only SNRs (J0448-6700 and J0455-6839), we used the
         value quoted in Badenes et al. (2010MNRAS.407.1301B) and Williams et al.
         (1999ApJS..123..467W), respectively.
    Note (4): The NH fraction is a measurement of how deep an SNR is with respect
         to the HI structure.
    Note (5): The numbers range from 1 meaning "strongly favours a type Ia SN
      origin", to 5 meaning "strongly favours a CC-SN origin".
    Note (6): References as follows:
         WM66   = Westerlund & Mathewson (1966MNRAS..131..371W)
         MC73   = Mathewson & Clarke (1973ApJ...180..725M)
         LHG81  = Long et al. (1981, Cat. J/ApJS/187/495)
         MFD83  = Mathewson et al. (1983ApJS...51..345M)
         TM84   = Turtle & Mills (1984PASAu...5..537T)
         MFD84  = Mathewson et al. (1984ApJS...55..189M)
         MFT85  = Mathewson et al. (1985ApJS...58..197M)
         CMG83  = Chu et al. (1993ApJ...414..213C)
         SCM94  = Smith et al. (1994AJ....108.1266S)
         CDS95  = Chu et al. (1995AJ....109.1729C)
         CKS97  = Chu et al. (1997PASP..109..554C)
         BGS06  = Blair et al. (2006ApJS..165..480B)
         KPS10  = Klimek et al. (2010ApJ...725.2281K)
         GSH12  = Grondin et al. (2012A&A...539A..15G)
         BFC12a = Bozzetto et al. (2012MNRAS.420.2588B)
         BFC12b = Bozzetto et al. (2012RMxAA..48...41B)
         DFB12  = de Horta et al. (2012A&A...540A..25D)
         MHB12  = Maggi et al. (2012A&A...546A.109M)
         KSP13  = Kavanagh et al. (2013A&A...549A..99K)
         BFC13  = Bozzetto et al. (2013MNRAS.432.2177B)
         MHK14  = Maggi et al. (2014A&A...561A..76M)
         BKM14  = Bozzetto et al. (2014MNRAS.439.1110B)
         KSB15a = Kavanagh et al. (2015A&A...573A..73K)
         KSB15b = Kavanagh et al. (2015A&A...579A..63K)

    Byte-by-byte Description of file:  table4.dat

       Bytes Format Units   Label     Explanations

           1  A1    ---     Case      [DI] D for 1T/2T SNRs with detected ejecta
                                       and I for ISM abundance
       3- 12  A10   ---     MCSNR     MCSNR identifier (JHHMM-DDMM)
      19- 37  A19   ---     OName     Old name
      38- 39  A2    ---     Type      SN type (1)
          46  A1    ---     HO        [Y-] High O/Fe flag (2)
          48  A1    ---     HO+Fe     [Y-] High O&Fe/Fe flag (for ISM abundance) (2)
          50  A1    ---     HNe       [Y-] High Ne/Fe flag (2)
          52  A1    ---     HMg       [Y-] High Mg/Fe flag (2)
          54  A1    ---     HSi       [Y-] High Si/Fe flag (2)
          56  A1    ---     LO        [Y-] Low O/Fe flag (2)
          58  A1    ---     LNe       [Y-] Low Ne/Fe flag (2)
          60  A1    ---     LMg       [Y-] Low Mg/Fe flag (2)
          62  A1    ---     LSi       [Y-] Low Si/Fe flag (2)

    Note (1): The classification given (type Ia or core-collapse) is described in
      Appendix B.
    Note (2): Y for detected.

    History:
        From electronic version of the journal
    ================================================================================
    (End)                                      Patricia Vannier [CDS]    11-Mar-2016