The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0

Abstract

We present a detailed analysis of the XMM-Newton and Chandra X-ray data of the young type Ia supernova remnant SNR 0519-69.0, which is situated in the Large Magellanic Cloud. We used data from both the Chandra ACIS and XMM-Newton EPIC MOS instruments, and high resolution X-ray spectra obtained with the XMM-Newton reflection grating spectrometer (RGS). Our analysis of the spatial distribution of X-ray line emission using the Chandra data shows that there is a radial stratification of oxygen, intermediate mass elements (IME) and iron, with the emission from more massive elements peaking more toward the center. Using a deprojection technique we measure a forward shock radius of 4.0 ± 0.3 pc and a reverse shock radius of 2.7 ± 0.4 pc. We took the observed stratification of the shocked ejecta into account in the modeling of the X-ray spectra, for which we used multicomponent non-equilibrium ionization models, with the components corresponding to layers dominated by one or two elements. An additional component was added in order to represent the shocked interstellar medium, which mostly contributed to the continuum emission. This multicomponent model fits the data adequately, and was also employed to characterize the spectra of distinct regions extracted from the Chandra data. From our spectral analysis we find that the approximate fractional masses of shocked ejecta for the most abundant elements are: M O ≈ 32%, M Si/S ≈ 7%/5%, M Ar+Ca ≈ 1% and M Fe ≈ 55%. From the continuum component we derive a circumstellar density of n H = 2.4 ± 0.2 cm −3 . This density, together with the measurements of the forward and reverse shock radii suggest an age of 0519-69.0 of 450 ± 200 yr, somewhat lower than, but consistent with the age estimate based on the extent of the light echo (600 ± 200 yr). Finally, from the high resolution RGS spectra we measured a Doppler broadening of σ = 1873 ± 50 km s −1 , from which we derive a forward shock velocity of v FS = 2770 ± 500 km s −1 . We discuss our results in the context of single degenerate explosion models, using semi-analytical and numerical modeling, and compare the characteristics of 0519-69.0 with those of other type Ia supernova remnants.

Modeling supernova remnants: effects of diffusive cosmic-ray acceleration on the evolution and application to observations

“…The observed ratios of the SNR reverse shock, the contact discontinuity, and the forward shock radii may depend on a number of yet unknown factors, such as the structure of the CSM (potential presupernova wind and density enhancement, see discussion in Kosenko et al 2010;Xu et al 2011), the CR acceleration, and the diffusion efficiency. Thus the results, presented in this study do not claim to be exhaustive, but rather describe a scenario that is capable of explaining the observations within the cosmic-ray acceleration paradigm.…”

The population of X-ray supernova remnants in the Large Magellanic Cloud

“…0519−69.0 exhibits strong lines of Si, S, Ar, and Ca, as well as prominent Fe L and K blends. To reproduce the spectra we used the multi-component approach of Kosenko et al (2010), who extensively studied the XMM-Newton and Chandra data.…”

Four new X-ray-selected supernova remnants in the Large Magellanic Cloud

“…This approach has been used in the past and allows, under some assumptions, to calculate the mass of the supernova nucleosynthesis products (e.g. Hughes et al 2003;Kosenko et al 2010;Bozzetto et al 2013b). …”