2015A&A...573A..73K


C.D.S. - SIMBAD4 rel 1.7 - 2019.07.20CEST18:58:01

2015A&A...573A..73K - Astronomy and Astrophysics, volume 573A, 73-73 (2015/1-1)

XMM-Newton study of 30 Doradus C and a newly identified MCSNR J0536-6913 in the Large Magellanic Cloud.

KAVANAGH P.J., SASAKI M., BOZZETTO L.M., FILIPOVIC M.D., POINTS S.D., MAGGI P. and HABERL F.

Abstract (from CDS):

We present a detailed study of the superbubble 30 Dor C and the newly identified supernova remnant MCSNR J0536-6913 in the Large Magellanic Cloud. All available XMM-Newton data (flare-filtered exposure times of 420ks EPIC-pn, 556ks EPIC-MOS1, 614ks EPIC-MOS2) were used to characterise the thermal X-ray emission in the region. An analysis of the non-thermal X-ray emission is also presented and discussed in the context of emission mechanisms previously suggested in the literature. These data are supplemented by X-ray data from Chandra, optical data from the Magellanic Cloud Emission Line Survey, and radio data from the Australia Telescope Compact Array and the Molonglo Observatory Synthesis Telescope.The brightest thermal emission towards 30 Dor C was found to be associated with a new supernova remnant, MCSNR J0536-6913. X-ray spectral analysis of MCSNR J0536-6913 suggested an ejecta-dominated remnant with lines of O, Ne, Mg, and Si, and a total 0.3-10keV X-ray luminosity of ∼8x1034erg/s. Based on derived ejecta abundance ratios, we determined the mass of the stellar progenitor to be either ∼18M or as high as >40M, though the spectral fits were subject to simplifying assumptions (e.g., uniform temperature and well-mixed ejecta). The thermal emission from the superbubble exhibited enrichment by α-process elements, evidence for a recent core-collapse SNR interaction with the superbubble shell. We detected non-thermal X-ray emission throughout 30 Dor C, with the brightest regions being highly correlated with the Hα and radio shells. We created a non-thermal spectral energy distribution for the north-eastern shell of 30 Dor C which was best-fit with an exponentially cut-off synchrotron model.Thermal X-ray emission from 30 Dor C is very complex, consisting of a large scale superbubble emission at the eastern shell wall with the brightest emission due to MCSNR J0536-6913. The fact that the non-thermal spectral energy distribution of the superbubble shell was observed to roll-off is further evidence that the non-thermal X-ray emission from 30 Dor C is synchrotron in origin.

Abstract Copyright:

Journal keyword(s): ISM: supernova remnants - ISM: bubbles - Magellanic Clouds - X-rays: ISM

Simbad objects: 36

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Number of rows : 36

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 8999 1
2 SNR B0102-72.3 SNR 01 04 01.2 -72 01 52           ~ 336 1
3 SNR B0103-72.6 SNR 01 05 05.6 -72 23 20           ~ 72 1
4 IC 131 HII 01 33 15.0 +30 45 09   12.52       ~ 58 0
5 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 4992 1
6 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5301 1
7 NGC 1761 As* 04 56 39 -66 29.0     9.94     ~ 95 0
8 LHA 120-N 11 HII 04 56 51.4 -66 24 24           ~ 225 0
9 LHA 120-N 186 EmO 04 59 45.5 -70 09 45           ~ 34 0
10 LHA 120-N 44 EmO 05 22 06.9 -67 56 46           ~ 160 1
11 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14185 1
12 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 338 1
13 LHA 120-N 51D HII 05 25 17.3 -67 22 47           ~ 104 0
14 LHA 120-N 206A HII 05 31 15.2 -71 03 58           ~ 94 2
15 SN 1987A SN* 05 35 28.020 -69 16 11.07   4.75 4.81     SN.IIPec 4351 2
16 [BUN2004] Shell D X 05 35.7 -69 13           ~ 2 0
17 [BUN2004] Shell C X 05 35.7 -69 10           ~ 2 0
18 NAME 30 Dor C Superbubble Rad 05 35 50.8 -69 12 22           ~ 40 1
19 NGC 2044 As* 05 36 11 -69 11.8   10.69 10.59     ~ 80 0
20 MCSNR J0536-6913 SNR 05 36 17.0 -69 13 28           ~ 7 0
21 [BUN2004] Shell A X 05 36.5 -69 13           ~ 2 0
22 CXOU J053633.3-691140 X 05 36 33.3 -69 11 40           ~ 2 0
23 [BUN2004] Shell B X 05 36.7 -69 10           ~ 2 0
24 PSR J0537-6909 Psr 05 37.0 -69 09           ~ 2 0
25 RMC 136 Cl* 05 38 42.396 -69 06 03.36   9.63 9.50     ~ 1661 2
26 LHA 120-N 158 HII 05 39 11.220 -69 30 13.65           ~ 79 0
27 X LMC X-1 HXB 05 39 38.8285930597 -69 44 35.533031148   14.8 14.5     O8(f)p 553 2
28 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 781 2
29 LHA 120-N 70 HII 05 43 17.5 -67 50 48           ~ 78 0
30 RCW 38 SFR 08 59 05.50 -47 30 39.4           ~ 256 2
31 NAME Lupus SN SNR 15 02 22.1 -42 05 49           SNIa 1172 1
32 NAME LHB X 16 42.0 +02 19           ~ 234 0
33 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 435 0
34 NAME Cyg Superbubble PoC 20 47 +41.2           ~ 72 1
35 NAME Cas A SNR 23 23 24.000 +58 48 54.00           ~ 2314 1
36 NAME Local Bubble ISM ~ ~           ~ 649 0

    Equat.    Gal    SGal    Ecl

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2019.07.20-18:58:01

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