Supernova 1998bw - the final phases

被引：53

作者：

Sollerman, J

Holland, ST

Challis, P

Fransson, C

Garnavich, P

Kirshner, RP

Kozma, C

Leibundgut, B

Lundqvist, P

Patat, F

Filippenko, AV

Panagia, N

Wheeler, JC

机构：

[1] European So Observ, D-85748 Garching, Germany

[2] Stockholm Observ, Dept Astron, SCFAB, S-10691 Stockholm, Sweden

[3] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA

[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[5] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[6] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[7] Univ Texas, Dept Astron, Austin, TX 78712 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2002年 / 386卷 / 03期

关键词：

supernovae : individual (SN 1998bw); nuclear reactions; nucleosynthesis; abundances; Gamma rays : bursts;

D O I：

10.1051/0004-6361:20020326

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The probable association with GRB 980425 immediately put SN 1998bw at the forefront of supernova research. Here, we present revised late-time BVRI light curves of the supernova, based on template images taken at the VLT. To follow the supernova to the very last observable phases we have used HST/STIS. Deep images taken in June and November 2000 are compared to images taken in August 2001. The identification of the supernova is firmly established. This allows us to measure the light curve to similar to 1000 days past explosion. The main features are a rapid decline up to more than 500 days after explosion, with no sign of complete positron trapping from the Co-56 decay. Thereafter, the light curve flattens out significantly. One possible explanation is powering by more long lived radioactive isotopes, if they are abundantly formed in this energetic supernova.

引用

页码：944 / 956

页数：13

共 44 条

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