ACDS V10.0 - Wed Jul 17 18:12:23 CEST 2019
 |
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