Institut für Astronomie und Astrophysik Abteilung Astronomie Sand 1, D-72076 Tübingen, Germany

Preprint B/14

Multi-frequency study of a new Fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902

L. M. Bozzetto (1), P. J. Kavanagh (2), P. Maggi (3), M. D. Filipovic (1), M. Stupar (4,5), Q. A. Parker (4,5,6), W. A. Reid (4,5), M. Sasaki (2), F. Haberl (3), D. Urosevic (7,8), J. Dickel (9), R. Sturm (3), R. Williams (10), M. Ehle (11), R. Gruendl (12), Y.-H. Chu (12), S. Points (13), E. J. Crawford (1)

(1) University of Western Sydney, Locked Bag 1797, Penrith South DC, NSW 1797, Australia
(2) Institut für Astronomie und Astrophysik Tübingen, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
(3) Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany
(4) Department of Physics, Macquarie University, Sydney, NSW 2109, Australia
(5) Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia
(6) Research Centre for Astronomy, Astrophysics and Astrophotonics, Macquarie University, Sydney, NSW 2109 Australia
(7) Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia
(8) Isaac Newton Institute of Chile, Yugoslavia Branch
(9) Physics and Astronomy Department, University of New Mexico, MSC 07-4220, Albuquerque, NM 87131, USA
(10) Coca-Cola Space Science Center, 701 Front Avenue, Columbus, GA 31901
(11) XMM-Newton Science Operations Centre, ESAC, ESA, PO Box 78, 28691 Villanueva de la Can ̃ada, Madrid, Spain
(12) Department of Astronomy, University of Illinois, 1002 West Green Street, Urbana, IL 61801, USA
(13) Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile

To be published in: MNRAS

Abstract. We present a detailed radio, X-ray and optical study of a newly discovered Large Magellanic Cloud (LMC) supernova remnant (SNR) which we denote MCSNR J0508-6902. Observations from the Australian Telescope Compact Array (ATCA) and the XMM-Newton X-ray observatory are complemented by deep Hα images and Anglo Australian Telescope AAOmega spectroscopic data to study the SNR shell and its shock-ionisation. Archival data at other wavelengths are also examined. The remnant follows a filled-in shell type morphology in the radio-continuum and has a size of ∼74 pc × 57 pc at the LMC distance. The X-ray emission exhibits a faint soft shell morphology with Fe-rich gas in its interior − indicative of a Type Ia origin. The remnant appears to be mostly dissipated at higher radio-continuum frequencies leaving only the south-eastern limb fully detectable while in the optical it is the western side of the SNR shell that is clearly detected. The best-fit temperature to the shel l X-ray emission (kT=0.41+0.05−0.06 keV) is consistent with other large LMC SNRs. We determined an O/Fe ratio of <21 and an Fe mass of 0.5-1.8 M⊙ in the interior of the remnant, both of which are consistent with the Type Ia scenario. We find an equipartition magnetic field for the remnant of ∼28 μG, a value typical of older SNRs and consistent with other analyses which also infer an older remnant.
 
Key words: ISM: supernova remnants, (galaxies:) Magellanic Clouds, radio contin- uum: ISM, X-rays: ISM

Astrophysics (astro-ph): 1401.1868

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