Deng 2005 SN 2003dh的光变和谱

主要内容:
从GRB 030329的余辉中分离出来的

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Title:		On the Light Curve and Spectrum of SN 2003dh Separated from the Optical Afterglow of GRB 030329
Authors:		Deng, J.; Tominaga, N.; Mazzali, P. A.; Maeda, K.; Nomoto, K.
Publication:		The Astrophysical Journal, Volume 624, Issue 2, pp. 898-905. (ApJ Homepage)
Publication Date:		05/2005
Origin:		UCP
ApJ Keywords:		Gamma Rays: Bursts, Stars: Supernovae: General, Stars: Supernovae: Individual: Alphanumeric: SN 2003dh
Abstract Copyright:		(c) 2005: The American Astronomical Society
DOI:		10.1086/429284
Bibliographic Code:		2005ApJ...624..898D

Abstract

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 gamma-ray burst (GRB) connected hypernova SN 1998bw is used to determine the amount of subtraction. The subtraction 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. We then build UVOIR bolometric SN light curve. Allowing for uncertainties, it can be reproduced with a spherical ejecta model of M_ej~7+/-3 M_solar, E_K~3.5+/-1.5×10⁵² ergs, with E_K/M_ej~5 following previous spectrum modeling, and M(⁵⁶Ni)~0.4^+0.15_-0.1 M_solar. This suggests a progenitor main-sequence mass of ~25-40 M_solar, lower than SN 1998bw but significantly higher than normal Type Ic SNe and the GRB-unrelated hypernova SN 2002ap.

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