XMM-Newton X-ray spectra of the SNR 0509-67.5: data and models

¹ Astronomical Institute Utrecht, University Utrecht, PO Box 80000, 3508TA Utrecht, The Netherlands e-mail: D.Kosenko@astro.uu.nl
² Sternberg Astronomical Institute, Russia
³ SRON, Utrecht, The Netherlands
⁴ Institute for Theoretical and Experimental Physics, 117218 Moscow, Russia
⁵ Stanford Linear Accelerator Center, Menlo Park, CA, USA

Received: 1 February 2008
Accepted: 26 June 2008

Abstract

Aims. We report on X-ray observations of the supernova remnant 0509-67.5 in the Large Magellanic Cloud acquired by the XMM-Newton X-ray observatory. We use the imaging spectroscopy (EPIC) and Reflective Grating Spectrometer (RGS) data to investigate properties of the remnant and its environment.

Methods. The X-ray spectra were analyzed with SPEX software package. In addition, we performed a numerical hydrodynamic simulation of the remnant.

Results. The EPIC data show prominent Fe K line emission, but the deduced overall amount of iron in the shocked ejecta is low. The data also show that the remnant has an asymmetric ejecta structure: the bright southwest region of the remnant shows an overabundance of metals. The analysis of the RGS spectrum shows that the remnant has a high line velocity broadening of 5000 km s^-1. We developed a hydrodynamical model for the remnant with basic hydrodynamical and spectral parameters that are similar to those observed.

Conclusions. The data analysis indicates that the reverse shock just recently reached iron layers of the ejecta. The brightness enhancement in the southwest region could be a sign of an asymmetric explosion or it could be the result of a density enhancement in the interstellar medium. We constructed numerical models that are in good agreement with the observations, with circumstellar density of , age of ~400 years, velocities of ~5000 km s^-1, and an electron-to-ion temperature ratio of 10^-2.