Taubenberger 2006 SN 2004aw的观测

主要内容:
喷出物的质量在3.5-8M_sun之间，比1994I大，比1998bw小。没有强的和伽玛暴成协的依据。

精彩摘抄:


各个暴在不同时期的谱线

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Title:		SN 2004aw: confirming diversity of Type Ic supernovae
Authors:		Taubenberger, S.; Pastorello, A.; Mazzali, P. A.; Valenti, S.; Pignata, G.; Sauer, D. N.; Arbey, A.; Bärnbantner, O.; Benetti, S.; Della Valle, A.; Deng, J.; Elias-Rosa, N.; Filippenko, A. V.; Foley, R. J.; Goobar, A.; Kotak, R.; Li, W.; Meikle, P.; Mendez, J.; Patat, F.; Pian, E.; Ries, C.; Ruiz-Lapuente, P.; Salvo, M.; Stanishev, V.; Turatto, M.; Hillebrandt, W.
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 371, Issue 3, pp. 1459-1477. (MNRAS Homepage)
Publication Date:		09/2006
Origin:		MNRAS
MNRAS Keywords:		supernovae: general: supernovae: individual: SN 2004aw: supernovae: individual: SN 1994I: supernovae: individual: SN 2002ap: supernovae: individual: SN 2003jd: galaxies: individual: NGC 3997
Abstract Copyright:		(c) 2006 The Authors. Journal compilation © 2006 RAS
DOI:		10.1111/j.1365-2966.2006.10776.x
Bibliographic Code:		2006MNRAS.371.1459T

Abstract

Optical and near-infrared (near-IR) observations of the Type Ic supernova (SN Ic) 2004aw are presented, obtained from -3 to +413 d with respect to the B-band maximum. The photometric evolution is characterized by a comparatively slow post-maximum decline of the light curves. The peaks in redder bands are significantly delayed relative to the bluer bands, the I-band maximum occurring 8.4 d later than that in B. With an absolute peak magnitude of -18.02 in the V band the SN can be considered fairly bright, but not exceptional. This also holds for the U through I bolometric light curve, where SN 2004aw has a position intermediate between SNe 2002ap and 1998bw. Spectroscopically SN 2004aw provides a link between a normal SN Ic like SN 1994I and the group of broad-lined SNe Ic. The spectral evolution is rather slow, with a spectrum at day +64 being still predominantly photospheric. The shape of the nebular [OI] λλ6300, 6364 line indicates a highly aspherical explosion. Helium cannot be unambiguously identified in the spectra, even in the near-IR. Using an analytical description of the light-curve peak we find that the total mass of the ejecta in SN 2004aw is 3.5-8.0M_solar, significantly larger than that in SN 1994I, although not as large as in SN 1998bw. The same model suggests that about 0.3M_solar of ⁵⁶Ni has been synthesized in the explosion. No connection to a GRB can be firmly established.

Based on observations at ESO-Paranal, Prog. 074.D-0161(A).

E-mail: tauben@mpa-garching.mpg.de

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