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2014 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 788, no 2, 154- p.Article in journal (Refereed) Published
Abstract [en]

Interaction of supernova (SN) ejecta with the optically thick circumstellar medium (CSM) of a progenitor star can result in a bright, long-lived shock-breakout event. Candidates for such SNe include Type IIn and superluminous SNe. If some of these SNe are powered by interaction, then there should be a specific relation between their peak luminosity, bolometric light-curve rise time, and shock-breakout velocity. Given that the shock velocity during shock breakout is not measured, we expect a correlation, with a significant spread, between the rise time and the peak luminosity of these SNe. Here, we present a sample of 15 SNe IIn for which we have good constraints on their rise time and peak luminosity from observations obtained using the Palomar Transient Factory. We report on a possible correlation between the R-band rise time and peak luminosity of these SNe, with a false-alarm probability of 3%. Assuming that these SNe are powered by interaction, combining these observables and theory allows us to deduce lower limits on the shock-breakout velocity. The lower limits on the shock velocity we find are consistent with what is expected for SNe (i.e., similar to 10(4) km s(-1)). This supports the suggestion that the early-time light curves of SNe IIn are caused by shock breakout in a dense CSM. We note that such a correlation can arise from other physical mechanisms. Performing such a test on other classes of SNe ( e. g., superluminous SNe) can be used to rule out the interaction model for a class of events.

Place, publisher, year, edition, pages
2014. Vol. 788, no 2, 154- p.
Keyword [en]
stars: massive, stars: mass-loss, supernovae: general
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:su:diva-106064DOI: 10.1088/0004-637X/788/2/154ISI: 000337466200057OAI: diva2:735755


Available from: 2014-07-31 Created: 2014-07-21 Last updated: 2014-07-31Bibliographically approved

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Fransson, Claes
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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