Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud
Kavanagh PJ, Sasaki M, Bozzetto LM, Points SD, Filipovic MD, Maggi P, Haberl F, Crawford EJ (2015)
Publication Status: Published
Publication Type: Journal article
Publication year: 2015
Journal
Publisher: EDP SCIENCES S A
Book Volume: 583
DOI: 10.1051/0004-6361/201526987
Abstract
Aims: We present a multi-frequency study of the supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud.
Methods: We used new data from XMM-Newton to characterise the X-ray
emission and data from the Australian Telescope Compact Array, the
Magellanic Cloud Emission Line Survey, and Spitzer to gain a picture of
the environment into which the remnant is expanding. We performed a
morphological study, determined radio polarisation and magnetic field
orientation, and performed an X-ray spectral analysis.
Results: We
estimated the remnant's size to be 24.9 ( ± 1.5) × 21.9 ( ± 1.5) pc,
with the major axis rotated ~29° east of north. Radio polarisation
images at 3 cm and 6 cm indicate a higher degree of polarisation in the
northwest and southeast tangentially oriented to the SNR shock front,
indicative of an SNR compressing the magnetic field threading the
interstellar medium. The X-ray spectrum is unusual as it requires a soft
(~0.2 keV) collisional ionisation equilibrium thermal plasma of
interstellar medium abundance, in addition to a harder component. Using
our fit results and the Sedov dynamical model, we showed that the
thermal emission is not consistent with a Sedov remnant. We suggested
that the thermal X-rays can be explained by MCSNR J0512-6707 having
initially evolved into a wind-blown cavity and is now interacting with
the surrounding dense shell. The origin of the hard component remains
unclear. We could not determine the supernova type from the X-ray
spectrum. Indirect evidence for the type is found in the study of the
local stellar population and star formation history in the literature,
which suggests a core-collapse origin.
Conclusions: MCSNR
J0512-6707 likely resulted from the core-collapse of high mass
progenitor which carved a low density cavity into its surrounding
medium, with the soft X-rays resulting from the impact of the blast wave
with the surrounding shell. The unusual hard X-ray component requires
deeper and higher spatial resolution radio and X-ray observations to
confirm its origin.
Authors with CRIS profile
Involved external institutions
Cerro Tololo Inter-American Observatory (CTIO)
Chile (CL)
Max-Planck-Institut für extraterrestrische Physik (MPE) / Max Planck Institute for Extraterrestrial Physics
Germany (DE)
University of Paris 7 - Denis Diderot / Université Paris VII Denis Diderot
France (FR)
Eberhard Karls Universität Tübingen
Germany (DE)
University of Western Sydney
Australia (AU)
Chile (CL)
Max-Planck-Institut für extraterrestrische Physik (MPE) / Max Planck Institute for Extraterrestrial Physics
Germany (DE)
University of Paris 7 - Denis Diderot / Université Paris VII Denis Diderot
France (FR)
Eberhard Karls Universität Tübingen
Germany (DE)
University of Western Sydney
Australia (AU)
How to cite
APA:
Kavanagh, P.J., Sasaki, M., Bozzetto, L.M., Points, S.D., Filipovic, M.D., Maggi, P.,... Crawford, E.J. (2015). Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud. Astronomy & Astrophysics, 583. https://doi.org/10.1051/0004-6361/201526987
MLA:
Kavanagh, P. J., et al. "Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud." Astronomy & Astrophysics 583 (2015).
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