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    XMM-Newton observation of SNR J0533–7202 in the Large Magellanic Cloud*

    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

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    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
    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
    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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