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CALTECH CORE-COLLAPSE PROJECT (CCCP) OBSERVATIONS OF TYPE IIn SUPERNOVAE: TYPICAL PROPERTIES AND IMPLICATIONS FOR THEIR PROGENITOR STARS

M. KieweBenoziyo Center for Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelA. Gal‐YamBenoziyo Center for Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelIair ArcaviBenoziyo Center for Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelDouglas C. LeonardDepartment of Astronomy, San Diego State University, San Diego CA 92182, USAJ. Emilio EnriquezDepartment of Astronomy, San Diego State University, San Diego CA 92182, USAS. B. CenkoDepartment of Astronomy, University of California, Berkeley, CA, 94720-3411, USAD. B. FoxDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA, 16802, USADae‐Sik MoonDepartment of Astronomy and Astrophysics, University of Toronto, Toronto, ON, M5S 3H4, CanadaDavid SandHarvard–Smithsonian Center for Astrophysics, 60 Garden#N# Street, Cambridge, MA 02138, USAAlicia SoderbergHarvard–Smithsonian Center for Astrophysics, 60 Garden#N# Street, Cambridge, MA 02138, USA(The CCCP)

2011en

ABI

Annotatsiya

Type IIn Supernovae (SNe IIn) are rare events, constituting only a few percent of all core-collapse SNe, and the current sample of well observed SNe IIn is small. Here, we study the four SNe IIn observed by the Caltech Core-Collapse Project (CCCP). The CCCP SN sample is unbiased to the extent that object selection was not influenced by target SN properties. Therefore, these events are representative of the observed population of SNe IIn. We find that a narrow P-Cygni profile in the hydrogen Balmer lines appears to be a ubiquitous feature of SNe IIn. Our light curves show a relatively long rise time (>20 days) followed by a slow decline stage (0.01 to 0.15 mag/day), and a typical V-band peak magnitude of M_V=-18.4 +/- 1.0 mag. We measure the progenitor star wind velocities (600 - 1400 km/s) for the SNe in our sample and derive pre-explosion mass loss rates (0.026 - 0.12 solar masses per year). We compile similar data for SNe IIn from the literature, and discuss our results in the context of this larger sample. Our results indicate that typical SNe IIn arise from progenitor stars that undergo LBV-like mass-loss shortly before they explode.

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DOI: 10.1088/0004-637x/744/1/10

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