Volume 561, January 2014
|Number of page(s)||22|
|Published online||27 January 2014|
Department of Physics and AstronomyAarhus University,
Ny Munkegade 120, 8000
Aarhus C, Denmark
2 Carnegie Observatories, Las Campanas Observatory, 601 Casilla, La Serena, Chile
3 Las Cumbres Observatory Global Telescope Network Inc., Santa Barbara CA 93117, USA
4 The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden
5 The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, 10691 Stockholm, Sweden
6 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
7 Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, 606-8502 Kyoto, Japan
8 Kavli Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, 277-8583 Chiba, Japan
9 INAF-Osservatorio Astronomico di Padova, vicolo dell Osservatorio 5, 35122 Padova, Italy
10 Departamento Ciencias Fõsicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile
11 Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks, Rm 100, Norman OK 73019-2061, USA
12 Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena CA 91101, USA
13 Departamento de Astronomia, Universidad de Chile, 36D Casilla, Santiago, Chile
14 Department of Physics, Florida State University, Tallahassee FL 32306, USA
15 Department of Astrophysical Sciences, Princeton University, NJ 08544, USA
16 University of North Carolina at Chapel Hill, Campus Box 3255, Chapel Hill, 27599-3255, USA
Received: 22 October 2013
Accepted: 18 November 2013
A comprehensive set of optical and near-infrared (NIR) photometry and spectroscopy is presented for the faint and fast 2008ha-like supernova (SN) 2010ae. Contingent on the adopted value of host extinction, SN 2010ae reached a peak brightness of −13.8 > MV > −15.3 mag, while modeling of the UVOIR light curve suggests it produced 0.003–0.007 M⊙ of 56Ni, ejected 0.30−0.60 M⊙ of material, and had an explosion energy of 0.04–0.30 × 1051 erg. The values of these explosion parameters are similar to the peculiar SN 2008ha –for which we also present previously unpublished early phase optical and NIR light curves – and places these two transients at the faint end of the 2002cx-like SN population. Detailed inspection of the post-maximum NIR spectroscopic sequence indicates the presence of a multitude of spectral features, which are identified through SYNAPPS modeling to be mainly attributed to Co ii. Comparison with a collection of published and unpublished NIR spectra of other 2002cx-like SNe, reveals that a Co ii footprint is ubiquitous to this subclass of transients, providing a link to Type Ia SNe. A visual-wavelength spectrum of SN 2010ae obtained at +252 days past maximum shows a striking resemblance to a similar epoch spectrum of SN 2002cx. However, subtle differences in the strength and ratio of calcium emission features, as well as diversity among similar epoch spectra of other 2002cx-like SNe indicates a range of physical conditions of the ejecta, highlighting the heterogeneous nature of thispeculiar class of transients.
Key words: supernovae: general / supernovae: individual: SN 2008ha / supernovae: individual: SN 2010ae
Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere, Chile (ESO Programs 082.A-0526, 084.D-0719, 088.D-0222, 184.D-1140, and 386.D-0966); the Gemini Observatory, Cerro Pachon, Chile (Gemini Programs GS-2010A-Q-14 and GS-2010A-Q-38); the Magellan 6.5 m telescopes at Las Campanas Observatory; and the SOAR telescope.
Tables 1−5 and Appendix A are available in electronic form at http://www.aanda.org
Reduced spectra are available as FITS files at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/561/A146
© ESO, 2014
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