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 \pm 0.3 pc and a reverse shock radius of 2.7 \pm 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 multi-component 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 _ { \mathrm { O } } \approx 32 % , M _ { \mathrm { Si / S } } \approx 7 \% / 5 \% , M _ { \mathrm { Ar + Ca } } \approx 1 % and M _ { \mathrm { Fe } } \approx 55 % .
From the continuum component we derive a circumstellar density of n _ { H } = 2.4 \pm 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 \pm 200 yr , somewhat lower than , but consistent with the age estimate based on the extent of the light echo ( 600 \pm 200 yr ) .

Finally , from the high resolution RGS spectra we measured a Doppler broadening of \sigma = 1873 \pm 50 km s ^ { -1 } , from which we derive a forward shock velocity of v _ { FS } = 2770 \pm 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 .