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

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 3×10^-25 g/cm^3, age of ~400 years, velocities of ~5000 km s^-1, and an electron-to-ion temperature ratio of 10^-2.