Coronal Lines And Dust In Sn 2005ip: Not The Brightest, But The Hottest Type Iin Supernova

Details Coronal Lines And Dust In Sn 2005ip: Not The Brightest, But The Hottest Type Iin Supernova Coronal Lines And Dust In Sn 2005ip: Not The Brightest, But The Hottest Type Iin Supernova

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21349003s&link_type=abstract

American Astronomical Society, AAS Meeting #213, #490.03; Bulletin of the American Astronomical Society, Vol. 41, p.465

Astronomy and Astrophysics

Astronomy

Scientific paper

We present optical photometry and spectroscopy of SN2005ip for the first 3yr after discovery, showing an underlying Type II-L SN interacting with a steady wind to yield an unusual Type IIn spectrum. For the first 160d, it had a fast linear decline from a modest peak absolute magnitude of about -17.4 (unfiltered), followed by a plateau at roughly -14.8 mag for more than 2yr. Initially having a normal broad-lined spectrum superposed with sparse narrow lines from the photoionized circumstellar medium (CSM), it quickly developed signs of strong CSM interaction with a spectrum similar to that of SN1988Z. As the underlying SN II-L faded, SN2005ip exhibited a rich high-ionization spectrum with a dense forest of narrow coronal lines, unprecedented among SNe but reminiscent of some AGN. The line-profile evolution of SN2005ip confirms that dust formation caused its recently reported infrared excess, but these lines reveal that it is the first SN to show clear evidence for dust in both the fast SN ejecta and the slower post-shock gas. SN 2005ip's complex spectrum confirms the origin of the strange blue continuum in SN 2006jc, which also had post-shock dust formation. We suggest that SN 2005ip's late-time plateau and coronal spectrum result from rejuvenated CSM interaction between a sustained fast shock and a clumpy stellar wind, where X-rays escape through the optically thin interclump regions to heat the pre-shock CSM to coronal temperatures.

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