SN 2004aw

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dc.contributor.authorTaubenberger, S.
dc.contributor.authorPastorello, A.
dc.contributor.authorMazzali, P. A.
dc.contributor.authorValenti, S.
dc.contributor.authorPignata, G.
dc.contributor.authorSauer, D. N.
dc.contributor.authorArbey, A.
dc.contributor.authorBaernbantner, O.
dc.contributor.authorBenetti, S.
dc.contributor.authorDella Valle, A.
dc.contributor.authorDeng, J.
dc.contributor.authorElias-Rosa, N.
dc.contributor.authorFilippenko, A. V.
dc.contributor.authorFoley, R. J.
dc.contributor.authorGoobar, A.
dc.contributor.authorKotak, R.
dc.contributor.authorLi, W.
dc.contributor.authorMeikle, P.
dc.contributor.authorMendez, J.
dc.contributor.authorPatat, F.
dc.contributor.authorPian, E.
dc.contributor.authorRies, C.
dc.contributor.authorRuiz-Lapuente, P.
dc.contributor.authorSalvo, M.
dc.contributor.authorStanishev, V.
dc.contributor.authorTuratto, M.
dc.contributor.authorHillebrandt, W.
dc.date.accessioned2025-01-21T01:05:56Z
dc.date.available2025-01-21T01:05:56Z
dc.date.issued2006
dc.description.abstractOptical 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 [O-I] lambda lambda 6300, 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-circle dot, significantly larger than that in SN 1994I, although not as large as in SN 1998bw. The same model suggests that about 0.3 M-circle dot of Ni-56 has been synthesized in the explosion. No connection to a GRB can be firmly established.
dc.fuente.origenWOS
dc.identifier.doi10.1111/j.1365-2966.2006.10776.x
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2006.10776.x
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/96049
dc.identifier.wosidWOS:000240350000039
dc.issue.numero3
dc.language.isoen
dc.pagina.final1477
dc.pagina.inicio1459
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectsupernovae : general
dc.subjectsupernovae : individual
dc.subjectSN 2004aw
dc.subjectsupernovae : individual : SN1994I
dc.subjectsupernovae : individual : SN 2002ap
dc.subjectsupernovae : individual : SN 2003jd
dc.subjectgalaxies : individual : NGC 3997
dc.titleSN 2004aw
dc.typeartículo
dc.volumen371
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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