Reddening, Abundances, and Line Formation in SNe II

Abstract

We present detailed NLTE spectral synthesis models of the Type II supernova 2005cs, which occurred in M51 and for which the explosion time is well determined. We show that previous estimates for the reddening were significantly too high and briefly discuss how this will effect the inferred progenitor mass. We also show that standard CNO-burning enhanced abundances require far too large an oxygen depletion, although there is evidence for a single optical N II line and the sodium abundance shows clear evidence for enhancement over solar both as expected from CNO processing. Finally we calculate a distance using the SEAM method. Given the broad range of distances to M51 in the literature, the determination of a distance using Cepheid variables would be quite valuable.

31 pages, 12 figures, ApJ (2007), in press

References in corpus (14)

• Comparative Direct Analysis of Type Ia Supernova Spectra. II. Maximum Light
• Abundance stratification in Type Ia supernovae - I. The case of SN 2002bo
• A non-spherical core in the explosion of supernova SN 2004dj
• SN 2005cs in M51 I. The first month of evolution of a subluminous SN II plateau
• The Progenitor of SN 2005cs in the Whirlpool Galaxy
• Identification of the Red Supergiant Progenitor of Supernova 2005cs: Do the Progenitors of Type II-P Supernovae Have Low Mass?
• Towards a Cosmological Hubble Diagram for Type II-P Supernovae
• Quantitative Spectroscopy of Photospheric-Phase Type II Supernovae
• Type IIP Supernovae as Cosmological Probes: A SEAM Distance to SN 1999em
• Quantitative spectroscopic analysis of and distance to SN1999em
• Comparative Direct Analysis of Spectra of Type Ia Supernovae. I. SN 1994D
• Strong effects of time-dependent ionization in early SN 1987A
• Distance estimate and progenitor characteristics of SN 2005cs in M51
• SN 1998A: Explosion of a Blue Supergiant

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