Analyzing SN 2003Z with PHOENIX ^*

¹ Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [sknop;yeti]@hs.uni-hamburg.de
² University of Oklahoma, 440 West Brooks St, Rm 100, Norman, OK 73019, USA e-mail: baron@nhn.ou.edu
³ Computational Research Division, Lawrence Berkeley National Laboratory, MS 50F-1650, 1 Cyclotron Rd, Berkeley, CA 94720-8139, USA
⁴ Institut für Astrophysik, University of Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany e-mail: dreizler@astro.physik.uni-goettingen.de

Received: 9 November 2006
Accepted: 22 April 2007

Abstract

Aims.We present synthetic spectra around maximum for the type II supernova SN 2003Z, which was first detected on January 29.7 2003. Comparison with observed spectra aim at the determination of physical parameters for SN 2003Z.

Methods.Synthetic spectra are calculated with our stellar atmosphere code PHOENIX. It solves the special relativistic equation of radiative transfer, including large NLTE-calculations and line blanketing by design, in 1-dimensional spherical symmetry. The observed spectra were obtained at the 3.5 m telescope at Calar Alto. The TWIN instrument was used so that a spectral range from about 3600 to 7500 Å was covered. The spectra were taken on Feb. 4, 5, 9, and 11, 2003.

Results.The physical parameters of the models give the luminosities, a range of possible velocity profiles for the SN, an estimate of the colour excess, and the observed metalicity.