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Title:
SN 2004aw: confirming diversity of Type Ic supernovae
Authors:
Taubenberger, S.; Pastorello, A.; Mazzali, P. A.; Valenti, S.; Pignata, G.; Sauer, D. N.; Arbey, A.; Bärnbantner, O.; Benetti, S.; Della Valle, A.; Deng, J.; Elias-Rosa, N.; Filippenko, A. V.; Foley, R. J.; Goobar, A.; Kotak, R.; Li, W.; Meikle, P.; Mendez, J.; Patat, F.; Pian, E.; Ries, C.; Ruiz-Lapuente, P.; Salvo, M.; Stanishev, V.; Turatto, M.; Hillebrandt, W.
Affiliation:
AA(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), AB(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), AC(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany; INAF Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34131 Trieste, Italy; Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0099, Japan; Research Center for the Early Universe, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0099, Japan), AD(European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany; Physics Department, University of Ferrara, 44100 Ferrara, Italy), AE(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile), AF(INAF Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34131 Trieste, Italy), AG(Université de Lyon 1, Centre de Recherche Astronomique de Lyon, 9 Avenue Charles André, F-69230 Saint-Genis Laval, France; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), AH(Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany), AI(INAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy), AJ(INAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy), AK(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China; Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0099, Japan; Research Center for the Early Universe, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0099, Japan), AL(INAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy; Universidad de La Laguna, Av. Astrofísico Francisco Sánchez s/n, E-38206 La Laguna, Tenerife, Spain), AM(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA), AN(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA), AO(Department of Physics, Stockholm University, AlbaNova University Center, SE-10691 Stockholm, Sweden), AP(European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany; Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ), AQ(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA), AR(Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ), AS(Department of Astronomy, University of Barcelona, Martí i Franques 1, E-08028 Barcelona, Spain; Isaac Newton Group of Telescopes, 38700 Santa Cruz de La Palma, Islas Canarias, Spain), AT(European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany), AU(INAF Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34131 Trieste, Italy), AV(Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany), AW(Department of Astronomy, University of Barcelona, Martí i Franques 1, E-08028 Barcelona, Spain; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany), AX(RSAA, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia), AY(Department of Physics, Stockholm University, AlbaNova University Center, SE-10691 Stockholm, Sweden), AZ(INAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy), BA(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 371, Issue 3, pp. 1459-1477. (MNRAS Homepage)
Publication Date:
09/2006
Origin:
MNRAS
MNRAS Keywords:
supernovae: general: supernovae: individual: SN 2004aw: supernovae: individual: SN 1994I: supernovae: individual: SN 2002ap: supernovae: individual: SN 2003jd: galaxies: individual: NGC 3997, supernovae: general, supernovae: individual: SN 2004aw, supernovae: individual: SN 1994I, supernovae: individual: SN 2002ap, supernovae: individual: SN 2003jd, galaxies: individual: NGC 3997
Abstract Copyright:
(c) 2006 The Authors. Journal compilation © 2006 RAS
DOI:
10.1111/j.1365-2966.2006.10776.x
Bibliographic Code:
2006MNRAS.371.1459T

Abstract

Optical and near-infrared (near-IR) observations of the Type Ic supernova (SN Ic) 2004aw are presented, obtained from -3 to +413 d with respect to the B-band maximum. The photometric evolution is characterized by a comparatively slow post-maximum decline of the light curves. The peaks in redder bands are significantly delayed relative to the bluer bands, the I-band maximum occurring 8.4 d later than that in B. With an absolute peak magnitude of -18.02 in the V band the SN can be considered fairly bright, but not exceptional. This also holds for the U through I bolometric light curve, where SN 2004aw has a position intermediate between SNe 2002ap and 1998bw. Spectroscopically SN 2004aw provides a link between a normal SN Ic like SN 1994I and the group of broad-lined SNe Ic. The spectral evolution is rather slow, with a spectrum at day +64 being still predominantly photospheric. The shape of the nebular [OI] λλ6300, 6364 line indicates a highly aspherical explosion. Helium cannot be unambiguously identified in the spectra, even in the near-IR. Using an analytical description of the light-curve peak we find that the total mass of the ejecta in SN 2004aw is 3.5-8.0Msolar, significantly larger than that in SN 1994I, although not as large as in SN 1998bw. The same model suggests that about 0.3Msolar of 56Ni has been synthesized in the explosion. No connection to a GRB can be firmly established.

Based on observations at ESO-Paranal, Prog. 074.D-0161(A).

E-mail: tauben@mpa-garching.mpg.de


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