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Post Info TOPIC: Supernova 2009bw


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Title: The bright Type IIP SN 2009bw, showing signs of interaction
Authors: 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, T.N. Sokolova

We present photometry and spectroscopy of the type IIP supernova 2009bw in UGC 2890 from few days after the outburst to 241 days. The light curve of SN 2009bw during the photospheric phase is similar to that of normal SNe IIP but with brighter peak and plateau (Mmax R = -17.82 mag, Mplateau R = -17.37 mag). The luminosity drop from the photospheric to the nebular phase is one of the fastest ever observed, ~2.2 mag in about 13 days. The radioactive tail of the bolometric light curve indicates that the amount of ejected 56 Ni is ~ 0.022 solar masses. The photospheric spectra reveal high velocity lines of H{\alpha} and H{\beta} until about 105 days 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 solar masses, a kinetic energy of ~0.3 foe and an initial radius of ~ 3.6 - 7 x 10^13 cm.

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A magnitude 15 Type II supernova, 2009bw, was discovered by Nissinen, Heikkinen, Hentunen (Taurus Hill observatory) on the 27th March, 2009, in the galaxy UGC 2890 in the constellation Camelopardalis.
The supernova is located 11" east and 22" north from the center of the galaxy.

Position(2000): RA = 03h56m06s.92, Dec. = +7255'40".9
z = 0.003853

CBET 1743 (Subscription)

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