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
Publisher: EDP SCIENCES S A
Book Volume: 579
DOI: 10.1051/0004-6361/201526143
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.
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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