Stephen P. Reynolds et al 2007 ApJ 668 L135 doi:10.1086/522830
Stephen P. Reynolds1, Kazimierz J. Borkowski1, Una Hwang2, John P. Hughes3, Carles Badenes3,4, J. M. Laming5 and J. M. Blondin1
Show affiliationsWe present initial results of a 750 ks Chandra observation of the remnant of Kepler's supernova of AD 1604. The strength and prominence of iron emission, together with the absence of O-rich ejecta, demonstrate that Kepler resulted from a thermonuclear supernova, even though evidence for circumstellar interaction is also strong. We have analyzed spectra of over 100 small regions, and find that they fall into three classes. (1) The vast majority show Fe L emission between 0.7 and 1 keV and Si and S Kα emission; we associate these with shocked ejecta. A few of these are found at or beyond the mean blast wave radius. (2) A very few regions show solar O/Fe abundance ratios; these we associate with shocked circumstellar medium (CSM). Otherwise O is scarce. (3) A few regions are dominated by continuum, probably synchrotron radiation. Finally, we find no central point source, with a limit ~100 times fainter than the central object in Cas A. The evidence that the blast wave is interacting with CSM may indicate a Ia explosion in a more massive progenitor.
ISM: individual (G4.5+6.8 (SN 1604)); supernova remnants; supernovae: general; X-rays: ISM
Issue 2 (2007 October 20)
Received 2007 April 25, accepted for publication 2007 August 28
Published 2007 October 2
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