Our results indicate that typical SNe IIn arise from progenitor stars that undergo luminous-blue-variable-like mass loss shortly before they explode.", We compile similar data for SNe IIn from the literature and discuss our results in the context of this larger sample. We measure the progenitor star wind velocities (600-1400kms-1) for the SNe in our sample and derive pre-explosion mass-loss rates (0.026-0.12 M ⊙ yr-1). Our light curves show a relatively long rise time (>20 days) followed by a slow decline stage (0.01-0.15magday-1), and a typical V-band peak magnitude of MV = -18.4☑.0mag. We find that a narrow P-Cygni profile in the hydrogen Balmer lines appears to be a ubiquitous feature of SNe IIn. Therefore, these events are representative of the observed population of SNe IIn. The CCCP SN sample is unbiased to the extent that object selection was not influenced by target SN properties. Here, we study the four SNe IIn observed by the Caltech Core-Collapse Project (CCCP). Our results indicate that typical SNe IIn arise from progenitor stars that undergo luminous-blue-variable-like mass loss shortly before they explode.Ībstract = "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. We measure the progenitor star wind velocities (600-1400kms -1) for the SNe in our sample and derive pre-explosion mass-loss rates (0.026-0.12 M ⊙ yr -1). Our light curves show a relatively long rise time (>20 days) followed by a slow decline stage (0.01-0.15magday -1), and a typical V-band peak magnitude of M V = -18.4☑.0mag. 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.
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