The Type IIn SN 1995G: Interaction with the CSM

Details The Type IIn SN 1995G: Interaction with the CSM The Type IIn SN 1995G: Interaction with the CSM

2002-01-29

arxiv.org/abs/astro-ph/0201483v1

Mon.Not.Roy.Astron.Soc. 333 (2002) 27

Astronomy and Astrophysics

Astrophysics

14 pages, including 11 figures. Accepted by MNRAS

Scientific paper

10.1046/j.1365-8711.2002.05366.x

We present the photometric and spectroscopic evolution of the type IIn SN 1995G in NGC 1643, on the basis of 4 years of optical and infrared observations. This supernova shows very flat optical light curves similar to SN 1988Z, with a slow decline rate at all times. The spectra are characterized by strong Balmer lines with multiple components in emission and with a P-Cygni absorption component blueshifted by only 700 km/s. This feature indicates the presence of a slowly expanding shell above the SN ejecta as in the case of SNe 1994aj and 1996L. As in other SNe IIn the slow luminosity decline cannot be explained only with a radioactive energy input and an additional source of energy is required, most likely that produced by the interaction between supernova ejecta and a pre--existent circumstellar medium. It was estimated that the shell material has a density n(H) >> 10^8 cm^-3, consistent with the absence of forbidden lines in the spectra. About 2 years after the burst the low velocity shell is largely overtaken by the SN ejecta and the luminosity drops at a faster rate.

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