AAS 206th Meeting, 29 May - 2 June 2005
Session 45 Supernovae Observations and Theory
Poster, Wednesday, 10:00am-7:00pm, Thursday, 9:20am-2:00pm, June 1, 2005, Ballroom A

Previous   |   Session 45   |   Next

[45.07] Does Metallicity Affect the Fate of Massive Stars?

R. Covarrubias, J. Dalcanton (University of Washington), M. Hamuy (Las Campanas Observatory, Carnegie Institution of Washington)

It has been shown theoretically that the relative number of core collapse supernovae (CCSNe) subtypes should depend on the metallicity of the host galaxy (Maeder 1992; Mowlavi et al. 1998). Moreover, Prantzos (2003) has shown indirectly that the ratio of the number of type II to the number of type Ib,c depends strongly on metallicity using the well known Metallicity-Luminosity relationship for late type galaxies (Garnet 2002 and references therein). Supernovae properties will be derived for 57 nearby (z < 0.05) CCSNe with high-quality optical photometry and spectroscopy that the CTIO and Carnegie group have collected between 1986-2003, mostly since 2001 in the course of the Carnegie Type II Supernova Survey (CATS). For nearly 20 of these objects we have also obtained NIR photometry. The data reductions and analysis are underway. So far, we have derived observed and physical properties for 24 SNe such as the mass and initial radius of the ejected envelopes and the explosion energy.

Our primary objective is to investigate if there is a relation between the host galaxy abundance and the observables properties of CCSNe. We are in the process of directly measuring the host galaxy radial metallicity distribution. Whenever possible, the metallicity at the SN position is measured. This allows us to: 1) narrow down the progenitors of CCSNe types, and 2) probe the effects of metallicity on CCSNe's light curves and spectra.

The author(s) of this abstract have provided an email address for comments about the abstract: ricardo@astro.washington.edu

Previous   |   Session 45   |   Next

Bulletin of the American Astronomical Society, 37 #2
© 2005. The American Astronomical Soceity.