Issue A&A Volume 414, Number 2, February I 2004 Page(s) 545 - 558 Section Formation, structure and evolution of stars DOI http://dx.doi.org/10.1051/0004-6361:20031551

A&A 414, 545-558 (2004)
DOI: 10.1051/0004-6361:20031551

XMM-Newton observation of Kepler's supernova remnant

G. Cassam-Chenaï¹, A. Decourchelle¹, J. Ballet¹, U. Hwang², J. P. Hughes³ and R. Petre<sup>4

1</sup>  Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France
²  Department of Astronomy, University of Maryland, College Park, MD 20742
³  Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854-8109, USA
⁴  Laboratory for High Energy Astrophysics, Goddard Space Flight Center, Greenbelt, MD 20771

(Received 20 February 2003 / Accepted 30 September 2003)

Abstract
We present the first results coming from the observation of Kepler's supernova remnant obtained with the EPIC instruments on board the XMM-Newton satellite. We focus on the images and radial profiles of the emission lines (Si K, Fe L, Fe K) and of the high energy continuum. Chiefly, the Fe L and Si K emission-line images are generally consistent with each other and the radial profiles show that the Si K emission extends to a larger radius than the Fe L emission (distinctly in the southern part of the remnant). Therefore, in contrast to Cas A, no inversion of the Si- and Fe-rich ejecta layers is observed in Kepler. Moreover, the Fe K emission peaks at a smaller radius than the Fe L emission, which implies that the temperature increases inwards in the ejecta. The 4-6 keV high energy continuum map shows the same distribution as the asymmetric emission-line images except in the southeast where there is a strong additional emission. A two color image of the 4-6 keV and 8-10 keV high energy continuum illustrates that the hardness variations of the continuum are weak all along the remnant except in a few knots. The asymmetry in the Fe K emission-line is not associated with any asymmetry in the Fe K equivalent width map. The Si K maps lead to the same conclusions. Hence, abundance variations do not cause the north-south brightness asymmetry. The strong emission in the north may be due to overdensities in the circumstellar medium. In the southeastern region of the remnant, the lines have a very low equivalent width and the X-ray emission is largely nonthermal.

Key words: ISM: supernova remnants -- ISM: individual objects: Kepler, SN1604 -- X-rays: ISM

Offprint request: G. Cassam-Chenaï, gcc@discovery.saclay.cea.fr

SIMBAD Objects

© ESO 2004

What is OpenURL?