ESC and KAIT observations of the transitional Type Ia SN 2004eo
A. PastorelloAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NNP. A. MazzaliINAF Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34131 Trieste, ItalyG. PignataPontificia Universidad Catlica de Chile, Departamento de Astronoma y Astrofsica, Campus San Joaqun, Vicua Mackenna 4860, Casilla 306, Santiago 22, ChileS. BenettiINAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 3512 2 Padova, ItalyE. CappellaroINAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 3512 2 Padova, ItalyA. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAWenyu LiDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAW. P. S. MeikleAstrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZA. A. ArkharovCentral Astronomical Observatory of Pulkovo, 196140 St Petersburg, RussiaGuillermo A. BlancAPC, UMR 7164 (CNRS, Universit Paris 7, CEA, Observatoire de Paris), 10, rue Alice Domon et Lie Duquet, F-75205 Paris Cedex 13, FranceF. BufanoDipartimento di Astronomia, Universit di Padova, Vicolo dell'Osservatorio, 2, I-35122 Padova, ItalyA. DerekasSchool of Physics A28, University of Sydney, NSW 2006, AustraliaM. DolciINAF Osservatorio Astronomico di Collurania, via M. Maggini, 64100 Teramo, ItalyN. Elias–RosaINAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 3512 2 Padova, ItalyR. J. FoleyDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAM. GaneshalingamDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAA. HarutyunyanDipartimento di Astronomia, Universit di Padova, Vicolo dell'Osservatorio, 2, I-35122 Padova, ItalyL. L. KissSchool of Physics A28, University of Sydney, NSW 2006, AustraliaR. KotakAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NNV. M. LarionovAstronomical Institute of St Petersburg University, St Petersburg, Petrodvorets, Universitetsky pr. 28, 198504 St Petersburg, RussiaJ. R. LuceyDepartment of Physics, University of Durham, South Road, Durham DH1 3LEN. NapoleoneINAF Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040 Monte Porzio Catone, ItalyH. NavasardyanINAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 3512 2 Padova, ItalyF. PatatEuropean Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748, Garching bei Mnchen, GermanyJ. RichResearch School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories Cotter Road, Weston Creek, ACT 2611, AustraliaS. D. RyderAnglo-Australian Observatory, PO Box 296, Epping, NSW 1710, AustraliaM. SalvoResearch School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories Cotter Road, Weston Creek, ACT 2611, AustraliaB. SchmidtResearch School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories Cotter Road, Weston Creek, ACT 2611, AustraliaV. StanishevDepartment of Physics, Stockholm University, AlbaNova University Centre, SE-10691 Stockholm, SwedenP. SzékelyDepartment of Experimental Physics & Astronomical Observatory, University of Szeged, H-6720 Szeged, Dóm tér 9, HungaryS. TaubenbergerMax-Planck-Institut fr Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei Mnchen, GermanyS. TemporinCEA/DSM/DAPNIA, Service d'Astrophysique, Saclay, F-91191 Gif-sur-Yvette Cedex, FranceM. TurattoINAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 3512 2 Padova, ItalyW. HillebrandtMax-Planck-Institut fr Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei Mnchen, Germany
2007en
ABI
Abstract
We present optical and infrared observations of the unusual Type Ia supernova (SN) 2004eo. The light curves and spectra closely resemble those of the prototypical SN 1992A, and the luminosity at maximum (M B = -19.08) is close to the average for a Type Ia supernova (SN Ia). However, the ejected 56 Ni mass derived by modelling the bolometric light curve (about 0.45 M ) lies near the lower limit of the 56 Ni mass distribution observed in normal SNe Ia. Accordingly, SN 2004eo shows a relatively rapid post-maximum decline in the light curve [ m 15 (B) true = 1.46], small expansion velocities in the ejecta and a depth ratio Si II 5972/Si II 6355 similar to that of SN 1992A. The physical properties of SN 2004eo cause it to fall very close to the boundary between the faint, low-velocity gradient and high-velocity gradient subgroups proposed by Benetti et al.
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