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Issue A&A
Volume 469, Number 2, July II 2007
Page(s) 645 - 661
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20066020



A&A 469, 645-661 (2007)
DOI: 10.1051/0004-6361:20066020

SN 2003du: 480 days in the life of a normal type Ia supernova

V. Stanishev1, A. Goobar1, S. Benetti2, R. Kotak3, 4, G. Pignata5, H. Navasardyan2, P. Mazzali6, 7, R. Amanullah1, G. Garavini1, S. Nobili1, Y. Qiu8, N. Elias-Rosa2, 9, P. Ruiz-Lapuente10, J. Mendez10, 11, P. Meikle12, F. Patat3, A. Pastorello6, 4, G. Altavilla10, M. Gustafsson13, A. Harutyunyan2, T. Iijima2, P. Jakobsson14, M. V. Kichizhieva15, P. Lundqvist16, S. Mattila4, J. Melinder16, E. P. Pavlenko17, N. N. Pavlyuk18, J. Sollerman16, 14, D. Yu. Tsvetkov18, M. Turatto2, and W. Hillebrandt7

1  Physics Department, Stockholm University, AlbaNova University Center, 106 91 Stockholm, Sweden
    e-mail: vall@physto.se
2  INAF, Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy
3  European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
4  Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast BT7 1NN, UK
5  Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Campus San Joaquín, Vicuña Mackenna 4860, Casilla 306, Santiago 22, Chile
6  INAF Osservatorio Astronomico di Trieste, via Tiepolo 11, 34131 Trieste, Italy
7  Max-Planck-Institut für Astrophysik, PO Box 1317, 85741 Garching, Germany
8  National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing, PR China
9  Universidad de La Laguna, Av. Astrofísico Fransisco Sánchez s/n, 38206 La Laguna, Tenerife, Spain
10  Department of Astronomy, University of Barcelona, Marti i Franques 1, 08028 Barcelona, Spain
11  Isaac Newton Group of Telescopes, Apartado de correos 321, 38700 Santa Cruz de La Palma, Canary Islands, Spain
12  Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK
13  Department of Physics and Astronomy, University of Aarhus, 8000 Aarhus C, Denmark
14  Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
15  Tavrida State University, Simferopol, Ukraine
16  Department of Astronomy, Stockholm University, AlbaNova University Center, 106 91 Stockholm, Sweden
17  Crimean Astrophysical Observatory, Ukraine
18  Sternberg Astronomical Institute, Moscow State University, Universitetskii pr. 13, Moscow 119992, Russia

(Received 12 July 2006 / Accepted 5 April 2007)

Abstract
Aims.We present a study of the optical and near-infrared (NIR) properties of the Type Ia Supernova (SN Ia) 2003du.
Methods. An extensive set of optical and NIR photometry and low-resolution long-slit spectra was obtained using a number of facilities. The observations started 13 days before B-band maximum light and continued for 480 days with exceptionally good time sampling. The optical photometry was calibrated through the S-correction technique.
Results. The ${\it UBVRIJHK}$ light curves and the color indices of SN 2003du closely resemble those of normal SNe Ia. SN 2003du reached a B-band maximum of 13.49 $\pm$ 0.02 mag on JD2 452 766.38 $\pm$ 0.5. We derive a B-band stretch parameter of $0.988 \pm0.003$, which corresponds to $\Delta m_{15}=1.02\,\pm0.05$, indicative of a SN Ia of standard luminosity. The reddening in the host galaxy was estimated by three methods, and was consistently found to be negligible. Using an updated calibration of the V and ${\it JHK}$ absolute magnitudes of SNe Ia, we find a distance modulus $\mu=32.79\pm0.15$ mag to the host galaxy, UGC 9391 . We measure a peak ${\it uvoir}$ bolometric luminosity of $1.35(\pm0.20)\times10^{43}$ erg s-1 and Arnett's rule implies that $M_{^{56}{\rm Ni}}\simeq0.68 \pm0.14\,M_{\odot}$ of $\element[][56]{Ni}$ was synthesized during the explosion. Modeling of the ${\it uvoir}$ bolometric light curve also indicates $M_{^{56}{\rm Ni}}$ in the range $0.6{-}0.8\,M_{\odot}$. The spectral evolution of SN 2003du at both optical and NIR wavelengths also closely resembles normal SNe Ia. In particular, the $\ion{Si}{ii}$ ratio at maximum $\mathcal{R}$( $\ion{Si}{ii}$) = $0.22\,\pm0.02$ and the time evolution of the blueshift velocities of the absorption line minima are typical. The pre-maximum spectra of SN 2003du showed conspicuous high-velocity features in the $\ion{Ca}{ii}$ H&K doublet and infrared triplet, and possibly in $\ion{Si}{ii}$ $\lambda$6355, lines. We compare the time evolution of the profiles of these lines with other well-observed SNe Ia and we suggest that the peculiar pre-maximum evolution of $\ion{Si}{ii}$ $\lambda$6355 line in many SNe Ia is due to the presence of two blended absorption components.


Key words: stars: supernovae: general -- stars: supernovae: individual: SN 2003du -- methods: observational -- techniques: photometric -- techniques: spectroscopic



© ESO 2007


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