Volume 406, Number 1, July IV 2003
|Page(s)||141 - 148|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
High resolution spectroscopy and emission line imaging of DEM L 71 with XMM-Newton
SRON National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
2 Columbia Astrophysics Laboratory, Columbia University, 550 West 1 20th Street, New York, NY 10027, USA
Corresponding author: K. J. van der Heyden, K.J.van.der.Heyden@sron.nl
Accepted: 15 April 2003
The X-ray emission from the supernova remnant DEM L 71 is measured and analysed using the high-resolution cameras and spectrometers on board XMM-Newton. The spectrum from the outer shell is reproduced very well by two plasma components of kTe = 0.3 and 0.8 keV. The abundance value from this shell is consistent with the average LMC values. More extreme temperature variations are possibly indicated by spatial variations in the forbidden/resonance line ratio, which could imply that in some regions the plasma is cooling dramatically and recombining. However, an alternative and equally interesting possibility is that the variation in forbidden/resonance ratios is due to resonant scattering, which would reduce resonance line emission along lines of sight with a high column density. The inner region is hotter ( keV) and shows enhanced Fe and Si abundances. We estimate the Fe and Si ejecta mass to be 0.7–1.1 and 0.1–0.15, respectively. The morphology, mass estimates and abundances strongly suggest that DEM L 71 is the result of a type Ia explosion, as indicated by previous measurements.
Key words: ISM: supernova remnants / ISM: individual objects: DEM L 71 / ISM: abundances / shock waves
© ESO, 2003
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