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

Inserra, C. ORCID: https://orcid.org/0000-0002-3968-4409, Turatto, M., Pastorello, A., Pumo, M. L., Baron, E., Benetti, S., Cappellaro, E., Taubenberger, S., Bufano, F., Elias-Rosa, N., Zampieri, L., Harutyunyan, A., Moskvitin, A. S., Nissinen, M., Stanishev, V., Tsvetkov, D. Y., Hentunen, V. P., Komarova, V. N., Pavlyuk, N. N., Sokolov, V. V. and Sokolova, T. N. 2012. The bright Type IIP SN 2009bw, showing signs of interaction. Monthly Notices of the Royal Astronomical Society 422 (2) , pp. 1122-1139. 10.1111/j.1365-2966.2012.20685.x

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Abstract

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 (⁠forumla mag, forumla 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.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Publisher:	Oxford University Press
ISSN:	0035-8711
Date of First Compliant Deposit:	2 January 2019
Date of Acceptance:	2 February 2012
Last Modified:	06 May 2023 04:46
URI:	https://orca.cardiff.ac.uk/id/eprint/117983

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