SN 2004aw: Confirming Diversity of Type Ic Supernovae

Details SN 2004aw: Confirming Diversity of Type Ic Supernovae SN 2004aw: Confirming Diversity of Type Ic Supernovae

2006-07-05

arxiv.org/abs/astro-ph/0607078v2

Mon.Not.Roy.Astron.Soc.371:1459-1477,2006

Astronomy and Astrophysics

Astrophysics

22 pages, 15 figures, 6tables, LaTeX, MNRAS online-early, references and affiliations updated, style corrections

Scientific paper

10.1111/j.1365-2966.2006.10776.x

Optical and near-infrared observations of the Type Ic supernova (SN) 2004aw are presented, obtained from day -3 to day +413 with respect to the B-band maximum. The photometric evolution is characterised by a comparatively slow post-maximum decline of the light curves. The peaks in redder bands are significantly delayed relative to the bluer bands, the I-band maximum occurring 8.4 days later than that in B. With an absolute peak magnitude of -18.02 in the V band the SN can be considered fairly bright, but not exceptional. This also holds for the U through I bolometric light curve, where SN 2004aw has a position intermediate between SNe 2002ap and 1998bw. Spectroscopically SN 2004aw provides a link between a normal Type Ic supernova like SN 1994I and the group of broad-lined SNe Ic. The spectral evolution is rather slow, with a spectrum at day +64 being still predominantly photospheric. The shape of the nebular [O I] 6300,6364 line indicates a highly aspherical explosion. Helium cannot be unambiguously identified in the spectra, even in the near-infrared. Using an analytical description of the light curve peak we find that the total mass of the ejecta in SN 2004aw is 3.5-8.0 M_Sun, significantly larger than in SN 1994I, although not as large as in SN 1998bw. The same model suggests that about 0.3 M_Sun of {56}Ni has been synthesised in the explosion. No connection to a GRB can be firmly established.

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