Other
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0502i&link_type=abstract
American Astronomical Society, HEAD meeting #9, #5.02; Bulletin of the American Astronomical Society, Vol. 38, p.348
Other
Scientific paper
The Swift observatory is uniquely suited to probe the early emission of supernovae (SNe) due to its fast response and large wavelength band coverage. We present a study of the early (days to weeks) X-ray and UV properties of eight type-Ia SNe which have been extensively observed with the X-Ray Telescope (XRT) and UV/Optical Telescope (UVOT) onboard Swift, ranging from 5-132 days after the outburst. The type-Ia SN 2005ke is detected in X-rays based on deep monitoring with the XRT ranging from 8 to 120 days after the outburst. The X-ray emission is likely due to the interaction of the SN shock with circumstellar material (CSM), deposited by a stellar wind from the progenitor's companion star. Evidence of CSM interaction in X-rays is independently confirmed by an excess of UV emission. The type-IIP SN 2006bp is detected in X-rays with Swift 1-12 days after the explosion. Since no other SN has been detected in X-rays at such an early age, we discuss the importance of inverse Compton-scattering of optical photons on relativistic electrons as possible origin of the X-ray emission.
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