2012A&A...546A.109M


Query : 2012A&A...546A.109M

2012A&A...546A.109M - Astronomy and Astrophysics, volume 546A, 109-109 (2012/10-1)

Multi-frequency study of supernova remnants in the Large Magellanic Cloud. Confirmation of the supernova remnant status of DEM L205.

MAGGI P., HABERL F., BOZZETTO L.M., FILIPOVIC M.D., POINTS S.D., CHU Y.-H., SASAKI M., PIETSCH W., GRUENDL R.A., DICKEL J., SMITH R.C., STURM R., CRAWFORD E.J. and DE HORTA A.Y.

Abstract (from CDS):

The Large Magellanic Cloud (LMC) is an ideal target for the study of an unbiased and complete sample of supernova remnants (SNRs). We started an X-ray survey of the LMC with XMM-Newton, which, in combination with observations at other wavelengths, will allow us to discover and study remnants that are either even fainter or more evolved (or both) than previously known. We present new X-ray and radio data of the LMC SNR candidate DEM L205, obtained by XMM-Newton and ATCA, along with archival optical and infrared observations. We use data at various wavelengths to study this object and its complex neighbourhood, in particular in the context of the star formation activity, past and present, around the source. We analyse the X-ray spectrum to derive some remnant's properties, such as age and explosion energy. Supernova remnant features are detected at all observed wavelengths: soft and extended X-ray emission is observed, arising from a thermal plasma with a temperature kT between 0.2keV and 0.3keV. Optical line emission is characterised by an enhanced [SII]-to-Hα ratio and a shell-like morphology, correlating with the X-ray emission. The source is not or only tentatively detected at near-infrared wavelengths (shorter than 10µm), but there is a detection of arc-like emission at mid and far-infrared wavelengths (24 and 70µm) that can be unambiguously associated with the remnant. We suggest that thermal emission from dust heated by stellar radiation and shock waves is the main contributor to the infrared emission. Finally, an extended and faint non-thermal radio emission correlates with the remnant at other wavelengths and we find a radio spectral index between -0.7 and -0.9, within the range for SNRs. The size of the remnant is ∼79x64pc and we estimate a dynamical age of about 35000 years. We definitely confirm DEM L205 as a new SNR. This object ranks amongst the largest remnants known in the LMC. The numerous massive stars and the recent outburst in star formation around the source strongly suggest that a core-collapse supernova is the progenitor of this remnant.

Abstract Copyright:

Journal keyword(s): Magellanic Clouds - ISM: supernova remnants - ISM: individual objects: MCSNR J0528-6727 - X-rays: ISM

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6408 1
2 SNR B0453-68.5 SNR 04 53 36.00 -68 29 30.0           ~ 73 1
3 SNR B0505-67.9 SNR 05 05 42.0 -67 52 29           ~ 133 0
4 SNR J050555-680150 SNR 05 05 55.00 -68 01 54.0           ~ 80 0
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16242 1
6 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 381 1
7 LHA 120-N 51D HII 05 25 17.3 -67 22 47           ~ 111 0
8 SNR B0525-66.0 SNR 05 25 27.1 -65 59 11           ~ 95 1
9 LHA 120-N 51 EmO 05 26 47 -67 31.1           ~ 43 0
10 NGC 1968 As* 05 27 23 -67 28.3   8.29 8.22     ~ 39 0
11 LHA 120-N 51C EmO 05 27 39 -67 27.3           ~ 13 0
12 LHA 120-N 51A HII 05 27 57 -67 25.4           ~ 24 1
13 LH 63 As* 05 27 58 -67 24.4           ~ 26 0
14 [FKM2008] LMC N J0528-6725 MoC 05 28 01.4 -67 25 41           ~ 5 0
15 MCSNR J0528-6727 HII 05 28 06.2 -67 26 50           ~ 21 0
16 [HP99] 534 X 05 28 19.6 -67 27 26           ~ 2 0
17 M 1 SNR 05 34 32 +22 00.8           ~ 5955 1
18 NAME LHB X 16 42.0 +02 19           ~ 299 0

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2022.09.25-04:11:02

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