Supernova 1998bw – the final phases*
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
2 Stockholm Observatory, Department of Astronomy, SCFAB, 106 91 Stockholm, Sweden
3 Physics Department, University of Notre Dame, Notre Dame, IN, USA
4 Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, USA
5 Department of Astronomy, University of California, Berkeley, CA, USA
6 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, USA
7 Department of Astronomy, University of Texas, Austin, TX, USA
Corresponding author: J. Sollerman, firstname.lastname@example.org
Accepted: 28 February 2002
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 ~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 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.
Key words: supernovae: individual (SN 1998bw) / nuclear reactions, nucleosynthesis, abundances / Gamma rays: bursts
Based on observations collected at the European Southern Observatory, La Silla and Paranal, Chile and on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
© ESO, 2002