| Authors | Stanishev, V.; Goobar, A.; Benetti, S.; Kotak, R.; Pignata, G.; Navasardyan, H.; Mazzali, P.; Amanullah, R.; Garavini, G.; Nobili, S.; Qiu, Y.; Elias-Rosa, N.; Ruiz-Lapuente, P.; Mendez, J.; Meikle, P.; Patat, F.; Pastorello, A.; Altavilla, G.; Gustafsson, M.; Harutyunyan, A.; Iijima, T.; Jakobsson, P.; Kichizhieva, M. V.; Lundqvist, P.; Mattila, S.; Melinder, J.; Pavlenko, E. P.; Pavlyuk, N. N.; Sollerman, J.; Tsvetkov, D. Yu.; Turatto, M.; Hillebrandt, W. |
| 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 {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 ± 0.02 mag on JD2 452 766.38 ± 0.5. We derive a B-band stretch parameter of 0.988 ±0.003, which corresponds to ∆ m15=1.02 ±0.05, 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 {JHK} absolute magnitudes of SNe Ia, we find a distance modulus μ=32.79±0.15 mag to the host galaxy, UGC 9391. We measure a peak {uvoir} bolometric luminosity of 1.35(±0.20)×1043 erg s-1 and Arnett's rule implies that M56Ni≃0.68 ±0.14 M☉ of 56Ni was synthesized during the explosion. Modeling of the {uvoir} bolometric light curve also indicates M56Ni in the range 0.6-0.8 M☉. The spectral evolution of SN 2003du at both optical and NIR wavelengths also closely resembles normal SNe Ia. In particular, the Si II ratio at maximum R(Si II) = 0.22 ±0.02 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 Ca II H&K doublet and infrared triplet, and possibly in Si II λ6355, 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 Si II λ6355 line in many SNe Ia is due to the presence of two blended absorption components. Table 3 and Appendix are only available in electronic form at http://www.aanda.org |
