A&A 365, L237-L241 (2001)
XMM-Newton EPIC observation of SMC SNR 0102-72.3M. Sasaki1, T. F. X. Stadlbauer1, F. Haberl1, M. D. Filipovic1,2,3 and P. J. Bennie4.
1 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, Postfach 1312, 85741 Garching, Germany
2 University of Western Sydney Nepean, PO Box 10, Kingswood, NSW 2747, Australia
3 Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 2121, Australia
4 University of Leicester, Leicester, LE1 7RH, UK
(Received 2 October 2000 / Accepted 2 November 2000)
Results from observations of the young oxygen-rich supernova remnant SNR 0102-72.3 in the Small Magellanic Cloud during the calibration phase of the XMM-Newton Observatory are presented. Both EPIC-PN and MOS observations show a ringlike structure with a radius of already known from Einstein, ROSAT and Chandra observations. Spectra of the entire SNR as well as parts in the eastern half were analyzed confirming shocked hot plasma in non-uniform ionization stages as the origin of the X-ray emission. The spectra differ in the northeastern and the southeastern part of the X-ray ring, showing emission line features of different strength. The temperature in the northeastern part is significantly higher than in the southeast, reflected by the lines of higher ionization stages and the harder continuum. Comparison to radio data shows the forward shock of the blast wave dominating in the northern part of the SNR, while the southern emission is most likely produced by the recently formed reverse shock in the ejecta. In the case of the overall spectrum of SNR 0102-72.3, the two-temperature non-equilibrium ionization model is more consistent with the data in comparison to the single plane-parallel shock model. The structure of SNR 0102-72.3 is complex due to variations in shock propagation leading to spatially differing X-ray spectra.
Key words: shock waves -ISM: supernova remnants -galaxies: Magellanic Clouds -X-rays: ISM
Offprint request: M. Sasaki, firstname.lastname@example.org
© ESO 2001