Low Luminosity Type II Supernovae: Spectroscopic and Photometric Evolution

Details Low Luminosity Type II Supernovae: Spectroscopic and Photometric Evolution Low Luminosity Type II Supernovae: Spectroscopic and Photometric Evolution

2003-09-09

arxiv.org/abs/astro-ph/0309264v1

Mon.Not.Roy.Astron.Soc.347:74,2004

Astronomy and Astrophysics

Astrophysics

23 pages, 26 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2004.07173.x

In this paper we present spectroscopic and photometric observations for four core collapse supernovae (SNe), namely SNe 1994N, 1999br, 1999eu and 2001dc. Together with SN 1997D, we show that they form a group of exceptionally low-luminosity events. These SNe have narrow spectral lines (indicating low expansion velocities) and low luminosities at every phase (significantly lower than those of typical core-collapse supernovae). The very low luminosity during the ^{56}Co radioactive decay tail indicates that the mass of ^{56}Ni ejected during the explosion is much smaller (M(Ni) ~ 2-8 x 10^{-3} Mo) than the average (M(Ni) ~ 6-10 x 10^{-2} Mo). Two supernovae of this group (SN 1999br and SN 2001dc) were discovered very close to the explosion epoch, allowing us to determine the lengths of their plateaux (~ 100 days) as well as establishiing the explosion epochs of the other, less-completely observed SNe. It is likely that this group of SNe represent the extreme low-luminosity tail of a single continuous distribution of SN II-P events. Their kinetic energy is also exceptionally low. Although an origin from low mass progenitors has also been proposed for low-luminosity core-collapse SNe, recent work provides evidence in favour of the high mass progenitor scenario. The incidence of these low--luminosity SNe could be as high as 4-5$ $ of all type II SNe.

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