期刊
ASTRONOMY & ASTROPHYSICS
卷 583, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201526987
关键词
ISM: supernova remnants; Magellanic Clouds; X-rays: ISM
资金
- Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWi/DLR) [FKZ 50 OR 1309]
- Deutsche Forschungsgemeinschaft [SA2131/1-1]
- Centre National d'Etudes Spatiales (CNES)
- CTIO
- NSF [AST-9540747, AST-0307613]
- Dean B. McLaughlin Fund at the University of Michigan
- Commonwealth of Australia
Aims. We present a multi-frequency study of the supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud. Methods. We used new data from XMM-Newton to characterise the X-ray emission and data from the Australian Telescope Compact Array, the Magellanic Cloud Emission Line Survey, and Spitzer to gain a picture of the environment into which the remnant is expanding. We performed a morphological study, determined radio polarisation and magnetic field orientation, and performed an X-ray spectral analysis. Results. We estimated the remnant's size to be 24.9 (+/- 1.5) x 21.9 (+/- 1.5) pc, with the major axis rotated similar to 29 degrees east of north. Radio polarisation images at 3 cm and 6 cm indicate a higher degree of polarisation in the northwest and southeast tangentially oriented to the SNR shock front, indicative of an SNR compressing the magnetic field threading the interstellar medium. The X-ray spectrum is unusual as it requires a soft (similar to 0.2 keV) collisional ionisation equilibrium thermal plasma of interstellar medium abundance, in addition to a harder component. Using our fit results and the Sedov dynamical model, we showed that the thermal emission is not consistent with a Sedov remnant. We suggested that the thermal X-rays can be explained by MCSNR J0512-6707 having initially evolved into a wind-blown cavity and is now interacting with the surrounding dense shell. The origin of the hard component remains unclear. We could not determine the supernova type from the X-ray spectrum. Indirect evidence for the type is found in the study of the local stellar population and star formation history in the literature, which suggests a core-collapse origin. Conclusions. MCSNR J0512-6707 likely resulted from the core-collapse of high mass progenitor which carved a low density cavity into its surrounding medium, with the soft X-rays resulting from the impact of the blast wave with the surrounding shell. The unusual hard X-ray component requires deeper and higher spatial resolution radio and X-ray observations to confirm its origin.
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