TY - JOUR
T1 - SN 2004aw
T2 - Confirming diversity of Type Ic supernovae
AU - Taubenberger, S.
AU - Pastorello, A.
AU - Mazzali, P. A.
AU - Valenti, S.
AU - Pignata, G.
AU - Sauer, D. N.
AU - Arbey, A.
AU - Bärnbantner, O.
AU - Benetti, S.
AU - Della Valle, A.
AU - Deng, J.
AU - Elias-Rosa, N.
AU - Filippenko, A. V.
AU - Foley, R. J.
AU - Goobar, A.
AU - Kotak, R.
AU - Li, W.
AU - Meikle, P.
AU - Mendez, J.
AU - Patat, F.
AU - Pian, E.
AU - Ries, C.
AU - Ruiz-Lapuente, P.
AU - Salvo, M.
AU - Stanishev, V.
AU - Turatto, M.
AU - Hillebrandt, W.
PY - 2006/9
Y1 - 2006/9
N2 - 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 F band the SN can be considered fairly bright, but not exceptional. This also holds for the U through / 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 19941 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 [O I] 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 3.5-8.0 M⊙, significantly larger than that in SN 19941, although not as large as in SN 1998bw. The same model suggests that about 0.3 M⊙ of 56Ni has been synthesized in the explosion. No connection to a GRB can be firmly established.
AB - 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 F band the SN can be considered fairly bright, but not exceptional. This also holds for the U through / 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 19941 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 [O I] 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 3.5-8.0 M⊙, significantly larger than that in SN 19941, although not as large as in SN 1998bw. The same model suggests that about 0.3 M⊙ of 56Ni has been synthesized in the explosion. No connection to a GRB can be firmly established.
KW - Galaxies: individual: NGC 3997
KW - Supernovae: general
KW - Supernovae: individual: SN 1994I
KW - Supernovae: individual: SN 2002ap
KW - Supernovae: individual: SN 2003jd
KW - Supernovae: individual: SN 2004aw
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U2 - 10.1111/j.1365-2966.2006.10776.x
DO - 10.1111/j.1365-2966.2006.10776.x
M3 - Article
AN - SCOPUS:33748287111
SN - 0035-8711
VL - 371
SP - 1459
EP - 1477
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -