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SN2003du: 480 days in the life of a normal type Ia supernova
Tekijät: 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 MV, Lundqvist P, Mattila S, Melinder J, Pavlenko EP, Pavlyuk NN, Sollerman J, Tsvetkov DY, Turatto M, Hillebrandt W
Kustantaja: EDP SCIENCES S A
Julkaisuvuosi: 2007
Journal: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: ASTRONOMY & ASTROPHYSICS
Lehden akronyymi: ASTRON ASTROPHYS
Vuosikerta: 469
Numero: 2
Aloitussivu: 645
Lopetussivu: U201
Sivujen määrä: 21
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361:20066020
Results. The UBVRIJHK light curves and the color indices of SN2003du closely resemble those of normal SNe Ia. SN2003du 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 Delta m(15) = 1.02 +/- 0.05, indicative of a SNIa 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 mu = 32.79 +/- 0.15 mag to the host galaxy, UGC 9391. We measure a peak uvoir bolometric luminosity of 1.35(+/- 0.20) x 10(43) erg s(-1) and Arnett's rule implies that M-56Ni similar or equal to 0.68 +/- 0.14 M-circle dot of Ni-56 was synthesized during the explosion. Modeling of the uvoir bolometric light curve also indicates M-56Ni in the range 0.6- 0.8 M-.. The spectral evolution of SN2003du 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 SN2003du showed conspicuous high-velocity features in the Ca II H& K doublet and infrared triplet, and possibly in 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 Si II lambda 6355 line in many SNe Ia is due to the presence of two blended absorption components.
