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On the Light Curve and Spectrum of SN 2003dh Separated from the Optical Afterglow of GRB 030329

J. DengResearch Center for the Early Universe, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, JapanNozomu TominagaDepartment of Astronomy, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, JapanP. A. MazzaliResearch Center for the Early Universe, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, JapanKeiichi MaedaDepartment of Astronomy, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, JapanKen’ichi NomotoResearch Center for the Early Universe, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, Japan

2005en

ABI

Annotatsiya

Accepted for publication in the Astrophysical Journal, Vol. ** * (2005) The net optical light curves and spectra of the supernova SN 2003dh are obtained from the published spectra of GRB 030329, covering about 6 days before SN maximum to about 60 days after. The bulk of the U-band flux is subtracted from the observed spectra using early-time afterglow templates, because strong line blanketing greatly depresses the UV and U-band SN flux in a metal-rich, fast-moving SN atmosphere. The blue-end spectra of the GRB-connected “hypernova ” SN 1998bw is used to determine the amount of subtraction. The substraction of a host galaxy template affects the late-time results. The derived SN 2003dh light curves are narrower than those of SN 1998bw, rising as fast before maximum, reaching a possibly fainter maximum and then declining ∼ 1.2 −1.4 times faster. The UV OIR bolometric SN light curve is built. Allowing for uncertainties, it can be reproduced with a spherical ejecta model of Mej ∼ 7±3 M⊙, EK ∼ 3.5 ± 1.5 × 10 52 ergs, with EK/Mej ∼ 5 following previous spectrum modelling, and M ( 56 Ni) ∼ 0.4 +0.15 −0.1 M⊙. This suggests a progenitor main-sequence mass of ∼ 25 − 40 M⊙,

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Identifikatorlar

DOI: 10.1086/429284

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