ISOCAM observations of young supernova remnants

Details ISOCAM observations of young supernova remnants ISOCAM observations of young supernova remnants

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..301d&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 301

Physics

3

Isocam, Supernova Remnants, Dust, Mixing

Scientific paper

In this paper, we present results from the CAMSNR program dedicated to observations of three young supernova remnants in our galaxy (Cassiopeia-A, Kepler and the Crab nebula). Most of the observations were spectro-imaging observations performed with the CVF (Circular Variable Filter) scan mode of ISOCAM ( te{cesarsky}). The origin of the bulk of the observed radiation is quite different in each remnant. The emission from Cassiopeia-A arises mainly from ``hot'' (about 220 K) thermal emission of newly formed dust in the so-called fast moving knots; in Kepler, the emission arises from thermal radiation of pre-supernova ``cold'' (about 120 K) dust; the emission from the Crab nebula is dominated by synchrotron emission. In addition to the above emission, ionic lines emission (especially neon lines) are detected in the three remnants. Information on the element mixing during the supernova explosion can be derived from the Cas-A observations.

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