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 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
[α/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:
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FileName Lrecl Records Explanations
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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)
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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
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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)
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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 2010MNRAS.407.1301B) and Williams et al.
(1999ApJS..123..467W 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 1973ApJ...180..725M)
LHG81 = Long et al. (1981, Cat. J/ApJS/187/495)
MFD83 = Mathewson et al. (1983ApJS...51..345M 1983ApJS...51..345M)
TM84 = Turtle & Mills (1984PASAu...5..537T 1984PASAu...5..537T)
MFD84 = Mathewson et al. (1984ApJS...55..189M 1984ApJS...55..189M)
MFT85 = Mathewson et al. (1985ApJS...58..197M 1985ApJS...58..197M)
CMG83 = Chu et al. (1993ApJ...414..213C 1993ApJ...414..213C)
SCM94 = Smith et al. (1994AJ....108.1266S 1994AJ....108.1266S)
CDS95 = Chu et al. (1995AJ....109.1729C 1995AJ....109.1729C)
CKS97 = Chu et al. (1997PASP..109..554C 1997PASP..109..554C)
BGS06 = Blair et al. (2006ApJS..165..480B 2006ApJS..165..480B)
KPS10 = Klimek et al. (2010ApJ...725.2281K 2010ApJ...725.2281K)
GSH12 = Grondin et al. (2012A&A...539A..15G 2012A&A...539A..15G)
BFC12a = Bozzetto et al. (2012MNRAS.420.2588B 2012MNRAS.420.2588B)
BFC12b = Bozzetto et al. (2012RMxAA..48...41B 2012RMxAA..48...41B)
DFB12 = de Horta et al. (2012A&A...540A..25D 2012A&A...540A..25D)
MHB12 = Maggi et al. (2012A&A...546A.109M 2012A&A...546A.109M)
KSP13 = Kavanagh et al. (2013A&A...549A..99K 2013A&A...549A..99K)
BFC13 = Bozzetto et al. (2013MNRAS.432.2177B 2013MNRAS.432.2177B)
MHK14 = Maggi et al. (2014A&A...561A..76M 2014A&A...561A..76M)
BKM14 = Bozzetto et al. (2014MNRAS.439.1110B 2014MNRAS.439.1110B)
KSB15a = Kavanagh et al. (2015A&A...573A..73K 2015A&A...573A..73K)
KSB15b = Kavanagh et al. (2015A&A...579A..63K 2015A&A...579A..63K)
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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)
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Note (1): The classification given (type Ia or core-collapse) is described in
Appendix B.
Note (2): Y for detected.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 11-Mar-2016