We present the results of a detailed investigation of the Galactic supernova remnant RCW 86 using the XMM-Newton X-ray telescope. RCW 86 is the probable remnant of SN 185 A.D, a supernova that likely exploded inside a wind-blown cavity. We use the XM
M-Newton Reflection Grating Spectrometer (RGS) to derive precise temperatures and ionization ages of the plasma, which are an indication of the interaction history of the remnant with the presumed cavity. We find that the spectra are well fitted by two non-equilibrium ionization models, which enables us to constrain the properties of the ejecta and interstellar matter plasma. Furthermore, we performed a principal component analysis on EPIC MOS and pn data to find regions with particular spectral properties. We present evidence that the shocked ejecta, emitting Fe-K and Si line emission, are confined to a shell of approximately 2 pc width with an oblate spheroidal morphology. Using detailed hydrodynamical simulations, we show that general dynamical and emission properties at different portions of the remnant can be well-reproduced by a type Ia supernova that exploded in a non-spherically symmetric wind-blown cavity. We also show that this cavity can be created using general wind properties for a single degenerate system. Our data and simulations provide further evidence that RCW 86 is indeed the remnant of SN 185, and is the likely result of a type Ia explosion of single degenerate origin.
Aims: We want to probe the physics of fast collision-less shocks in supernova remnants. In particular, we are interested in the non-equilibration of temperatures and particle acceleration. Specifically, we aim to measure the oxygen temperature with r
egards to the electron temperature. In addition, we search for synchrotron emission in the northwestern thermal rim. Methods: This study is part of a dedicated deep observational project of SN 1006 using XMM-Newton, which provides us with currently the best resolution spectra of the bright northwestern oxygen knot. We aim to use the reflection grating spectrometer to measure the thermal broadening of the O vii line triplet by convolving the emission profile of the remnant with the response matrix. Results: The line broadening was measured to be {sigma}_e = 2.4 pm 0.3 eV, corresponding to an oxygen temperature of 275$^{+72}_{-63}$ keV. From the EPIC spectra we obtain an electron temperature of 1.35 pm 0.10 keV. The difference in temperature between the species provides further evidence of non-equilibration of temperatures in a shock. In addition, we find evidence for a bow shock that emits X-ray synchrotron radiation, which is at odds with the general idea that due to the magnetic field orientation only in the NE and SW region X-ray synchrotron radiation should be emitted. We find an unusual H{alpha} and X-ray synchrotron geometry, in that the H{alpha} emission peaks downstream of the synchrotron emission. This may be an indication for a peculiar H{alpha} shock, in which the density is lower and neutral fraction are higher than in other supernova remnants, resulting in a peak in H{alpha} emission further downstream of the shock.
Aims: We study the supernova remnant 0506-68 in order to obtain detailed information about, among other things, the ionisation state and age of the ionised plasma. Methods: Using the Reflection Grating Spectrometer (RGS) onboard the XMM-Newton satell
ite we are able to take detailed spectra of the remnant. In addition, we use the MOS data to obtain spectral information at higher energies. Results: The spectrum shows signs of recombination and we derive the conditions for which the remnant and SNR in general are able to cool rapidly enough to become over-ionised. The elemental abundances found are mostly in agreement with the mean LMC abundances. Our models and calculations favour the lower age estimate mentioned in the literature of $sim4000$ year.
