{
  "id": "1505.06458",
  "version": "v1",
  "published": "2015-05-24T17:14:30.000Z",
  "updated": "2015-05-24T17:14:30.000Z",
  "title": "XMM-Newton observation of SNR J0533-7202 in the Large Magellanic Cloud",
  "authors": [
    "P. J. Kavanagh",
    "M. Sasaki",
    "E. T. Whelan",
    "P. Maggi",
    "F. Haberl",
    "L. M. Bozzetto",
    "M. D. Filipovic",
    "E. J. Crawford"
  ],
  "comment": "7 pages, 4 figures, accepted for publication in Astronomy and Astrophysics",
  "categories": [
    "astro-ph.HE"
  ],
  "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 (flare-filtered exposure times of 18 ks EPIC-pn and 31 ks EPIC-MOS1/MOS2). We produced X-ray images of the SNR, 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 brighter than the north-east. The X-ray emission is correlated with the radio emission from the remnant. We determine that this morphology is likely due to the SNR expanding into a non-uniform ambient medium and not an absorption effect. We estimate the size to be 53.9 (\\pm 3.4) x 43.6 (\\pm 3.4) pc, with the major axis rotated ~64 degrees east of north. We find no spectral signatures of ejecta 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 an age of ~17-27 kyr, with an initial explosion energy of (0.09-0.83) x 10^51 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 find 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.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-05-24T17:14:30.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "large magellanic cloud",
      "xmm-newton observation",
      "detected bright thermal x-ray emission",
      "initial explosion energy",
      "south-west region brighter"
    ],
    "publication": {
      "doi": "10.1051/0004-6361/201526143"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 7,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1372692
    }
  }
}