XMM-Newton study of 30 Doradus C and a newly identified MCSNR J0536-6913 in the Large Magellanic Cloud
Kavanagh PJ, Sasaki M, Bozzetto LM, Filipovic MD, Points SD, Maggi P, Haberl F (2015)
Publication Status: Published
Publication Type: Journal article
Publication year: 2015
Journal
Publisher: EDP SCIENCES S A
Book Volume: 573
DOI: 10.1051/0004-6361/201424354
Abstract
Aims: 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.
Methods: All available XMM-Newton data
(flare-filtered exposure times of 420 ks EPIC-pn, 556 ks EPIC-MOS1, 614
ks 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.
Results: 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 0.3-10 keV X-ray luminosity of ~8 × 1034 erg s-1. Based on derived ejecta abundance ratios, we determined the mass of the stellar progenitor to be either ~18 M☉ or as high as ≳40 M☉,
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.
Conclusions: 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.
Authors with CRIS profile
Involved external institutions
Eberhard Karls Universität Tübingen
Germany (DE)
University of Western Sydney
Australia (AU)
Max-Planck-Institut für extraterrestrische Physik (MPE) / Max Planck Institute for Extraterrestrial Physics
Germany (DE)
National Optical Astronomy Observatory (NOAO)
United States (USA) (US)
Germany (DE)
University of Western Sydney
Australia (AU)
Max-Planck-Institut für extraterrestrische Physik (MPE) / Max Planck Institute for Extraterrestrial Physics
Germany (DE)
National Optical Astronomy Observatory (NOAO)
United States (USA) (US)
How to cite
APA:
Kavanagh, P.J., Sasaki, M., Bozzetto, L.M., Filipovic, M.D., Points, S.D., Maggi, P., & Haberl, F. (2015). XMM-Newton study of 30 Doradus C and a newly identified MCSNR J0536-6913 in the Large Magellanic Cloud. Astronomy & Astrophysics, 573. https://doi.org/10.1051/0004-6361/201424354
MLA:
Kavanagh, P. J., et al. "XMM-Newton study of 30 Doradus C and a newly identified MCSNR J0536-6913 in the Large Magellanic Cloud." Astronomy & Astrophysics 573 (2015).
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