EDP Sciences
Free Access
Volume 406, Number 1, July IV 2003
Page(s) 141 - 148
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20030658

A&A 406, 141-148 (2003)
DOI: 10.1051/0004-6361:20030658

High resolution spectroscopy and emission line imaging of DEM L 71 with XMM-Newton

K. J. van der Heyden1, J. A. M. Bleeker1, J. S. Kaastra1 and J. Vink2, 3

1  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
3  Chandra fellow

(Received 5 February 2003 / 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 $kT_{\rm e}$ = 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 $\ion{O}{vii}$ 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 $\ion{O}{vii}$ column density. The inner region is hotter ( $kT_{\rm e} = 1.1$ keV) and shows enhanced Fe and Si abundances. We estimate the Fe and Si ejecta mass to be 0.7-1.1 $~M_{\odot}$ and 0.1-0.15 $~M_{\odot}$, 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

Offprint request: K. J. van der Heyden, K.J.van.der.Heyden@sron.nl

SIMBAD Objects

© ESO 2003

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