XMM-Newton observation of SNR J0533-7202 in the Large Magellanic Cloud
Kavanagh PJ, Sasaki M, Whelan ET, Maggi P, Haberl F, Bozzetto LM, Filipovic MD, Crawford EJ (2015)
Publication Status: Published
Publication Type: Journal article
Publication year: 2015
Journal
Publisher: EDP SCIENCES S A
Book Volume: 579
DOI: 10.1051/0004-6361/201526143
Abstract
Aims: We present an X-ray study of the supernova remnant SNR J0533-7202
in the Large Magellanic Cloud (LMC) and determine its physical
characteristics based on its X-ray emission.
Methods: We observed
SNR J0533-7202 with XMM-Newton (background flare-filtered exposure times
of 18 ks EPIC-pn and 31 ks EPIC-MOS1, EPIC-MOS2). We produced X-ray
images of the supernova remnant, performed an X-ray spectral analysis,
and compared the results to multi-wavelength studies.
Results: The
distribution of X-ray emission is highly non-uniform, with the
south-west region much brighter than the north-east. The detected X-ray
emission is correlated with the radio emission from the remnant. We
determine that this morphology is most likely due to the supernova
remnant expanding into a non-uniform ambient medium and not an
absorption effect. We estimate the remnant size to be 53.9 (±3.4) × 43.6
(±3.4) pc, with the major axis rotated ~64° east of north. We find no
spectral signatures of ejecta emission and infer that the X-ray plasma
is dominated by swept up interstellar medium. Using the spectral fit
results and the Sedov self-similar solution, we estimate the age of SNR
J0533-7202 to be ~17-27 kyr, with an initial explosion energy of
(0.09-0.83) × 1051 erg. We detected an X-ray source located
near the centre of the remnant, namely XMMU J053348.2-720233. The source
type could not be conclusively determined due to the lack of a
multi-wavelength counterpart and low X-ray counts. We found that it is
likely either a background active galactic nucleus or a low-mass X-ray
binary in the LMC.
Conclusions: We detected bright thermal X-ray
emission from SNR J0533-7202 and determined that the remnant is in the
Sedov phase of its evolution. The lack of ejecta emission prohibits us
from typing the remnant with the X-ray data. Therefore, the likely Type
Ia classification based on the local stellar population and star
formation history reported in the literature cannot be improved upon.
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)
Germany (DE)
University of Western Sydney
Australia (AU)
Max-Planck-Institut für extraterrestrische Physik (MPE) / Max Planck Institute for Extraterrestrial Physics
Germany (DE)
How to cite
APA:
Kavanagh, P.J., Sasaki, M., Whelan, E.T., Maggi, P., Haberl, F., Bozzetto, L.M.,... Crawford, E.J. (2015). XMM-Newton observation of SNR J0533-7202 in the Large Magellanic Cloud. Astronomy & Astrophysics, 579. https://doi.org/10.1051/0004-6361/201526143
MLA:
Kavanagh, P. J., et al. "XMM-Newton observation of SNR J0533-7202 in the Large Magellanic Cloud." Astronomy & Astrophysics 579 (2015).
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