Journal Article

The bright Type IIP SN 2009bw, showing signs of interaction*

C. Inserra, M. Turatto, A. Pastorello, M. L. Pumo, E. Baron, S. Benetti, E. Cappellaro, S. Taubenberger, F. Bufano, N. Elias-Rosa, L. Zampieri, A. Harutyunyan, A. S. Moskvitin, M. Nissinen, V. Stanishev, D. Y. Tsvetkov, V. P. Hentunen, V. N. Komarova, N. N. Pavlyuk, V. V. Sokolov and T. N. Sokolova

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 422, issue 2, pages 1122-1139
Published in print May 2012 | ISSN: 0035-8711
Published online April 2012 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2012.20685.x
The bright Type IIP SN 2009bw, showing signs of interaction*

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We present photometry and spectroscopy of the Type IIP supernova (SN IIP) 2009bw in UGC 2890 from a few days after the outburst to 241 d. The light curve of SN 2009bw during the photospheric phase is similar to that of normal SNe IIP but with a brighter peak and plateau ( mag,  mag). The luminosity drop from the photospheric to the nebular phase is one of the fastest ever observed, ∼2.2 mag in about 13 d. The radioactive tail of the bolometric light curve indicates that the amount of ejected 56Ni is ≈0.022 M. The photospheric spectra reveal high-velocity lines of Hα and Hβ until about 105 d after the shock breakout, suggesting a possible early interaction between the SN ejecta and pre-existent circumstellar material, and the presence of CNO elements. By modelling the bolometric light curve, ejecta expansion velocity and photospheric temperature, we estimate a total ejected mass of ∼8–12 M, a kinetic energy of ∼0.3 foe and an initial radius of ∼3.6–7 × 1013 cm.

Keywords: supernovae: general; supernovae: individual: SN 2009bw; galaxies: individual: UGC 2890

Journal Article.  11033 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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