Kavanagh, P.J. and Sasaki, M. and Whelan, Emma and Maggi, P. and Haber, F. and Bozzetto, L.M. and Filipović, M.D. and Crawford, E.J.
(2015)
XMM-Newton observation of SNR J0533–7202 in the Large Magellanic Cloud*.
Astronomy and Astrophysics, 579 (A63).
ISSN 0004-6361
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.
Item Type: |
Article
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Additional Information: |
*Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. |
Keywords: |
ISM: supernova remnants; Magellanic Clouds; X-rays: ISM; |
Academic Unit: |
Faculty of Science and Engineering > Experimental Physics |
Item ID: |
9882 |
Depositing User: |
Emma Whelan
|
Date Deposited: |
06 Sep 2018 15:13 |
Journal or Publication Title: |
Astronomy and Astrophysics |
Publisher: |
EDP Sciences |
Refereed: |
Yes |
URI: |
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Use Licence: |
This item is available under a Creative Commons Attribution Non Commercial Share Alike Licence (CC BY-NC-SA). Details of this licence are available
here |
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