Статья

Models for the Type Ic Hypernova SN 2003lw associated with GRB 031203

Paolo A. MazzaliDepartment of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanJinsong DengDepartment of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanElena PianNational Institute for Astrophysics, Osservatorio Astronomico di Trieste, Via Tiepolo 11, I-34131 Trieste, ItalyDaniele MalesaniInternational School for Advanced Studies (SISSA), via Beirut 2-4, I-34014 Trieste, ItalyNozomu TominagaDepartment of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanKeiichi MaedaDepartment of Earth Science and Astronomy, Graduate School of Arts and Science, University of Tokyo, Meguro-ku, Tokyo 153-8902, JapanKen’ichi NomotoDepartment of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanGuido ChincariniNational Institute for Astrophysics, Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), ItalyStefano CovinoNational Institute for Astrophysics, Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), ItalyMassimo Della ValleEuropean Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, GermanyDino FugazzaNational Institute for Astrophysics, Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), ItalyGianpiero TagliaferriNational Institute for Astrophysics, Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), ItalyAvishay Gal‐YamDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125

2006en

ABI

Аннотация

The Gamma-Ray Burst 031203 at a redshift z=0.1055 revealed a highly reddened Type Ic Supernova, SN 2003lw, in its afterglow light. This is the third well established case of a link between a long-duration GRB and a type Ic SN. The SN light curve is obtained subtracting the galaxy contribution and is modelled together with two spectra at near-maximum epochs. A red VLT grism 150I spectrum of the SN near peak is used to extend the spectral coverage, and in particular to constrain the uncertain reddening, the most likely value for which is E_{G+H}(B-V) about 1.07 +/- 0.05. Accounting for reddening, SN 2003lw is about 0.3 mag brighter than the prototypical GRB-SN 1998bw. Light curve models yield a 56Ni mass of about 0.55 solar mass. The optimal explosion model is somewhat more massive (ejecta mass about 13 solar mass) and energetic (kinetic energy about 6 times 10^52 erg) than the model for SN 1998bw, implying a massive progenitor (40 - 50 solar mass). The mass at high velocity is not very large (1.4 solar mass above 30000 km/s, but only 0.1 solar mass above 60000 km/s), but is sufficient to cause the observed broad lines. The similarity of SNe 2003lw and 1998bw and the weakness of their related GRBs, GRB031203 and GRB980425, suggest that both GRBs may be normal events viewed slightly off-axis or a weaker but possibly more frequent type of GRB.

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Идентификаторы

DOI: 10.1086/504415

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