Journal
ASTROPHYSICAL JOURNAL
Volume 792, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/792/1/7
Keywords
supernovae: general; supernovae: individual (SN 2010as)
Categories
Funding
- World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan
- Proyecto FONDECYT [11090421]
- Millennium Institute of Astrophysics (MAS) through the Programa Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo de Chile [IC120009]
- FONDECYT [3140326]
- Danish Agency for Science and Technology
- Instrument Center for Danish Astrophysics (IDA)
- GROND [23740141, 26800100]
- Leibniz-Prize to Prof. G. Hasinger, Deutsche Forschungsgemeinschaft (DFG) [HA 1850/28-1]
- National Aeronautics and Space Administration
- [23740175]
- [23224004]
- [23540262]
- [26400222]
- Grants-in-Aid for Scientific Research [26800100, 23224004] Funding Source: KAKEN
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We present extensive optical and near-infrared photometric and spectroscopic observations of the stripped-envelope supernova SN 2010as. Spectroscopic peculiarities such as initially weak helium features and low expansion velocities with a nearly flat evolution place this object in the small family of events previously identified as transitional Type Ib/c supernovae (SNe). There is ubiquitous evidence of hydrogen, albeit weak, in this family of SNe, indicating that they are in fact a peculiar kind of Type IIb SNe that we name flat-velocity Type IIb. The flat-velocity evolution-which occurs at different levels between 6000 and 8000 km s(-1) for different SNe-suggests the presence of a dense shell in the ejecta. Despite the spectroscopic similarities, these objects show surprisingly diverse luminosities. We discuss the possible physical or geometrical unification picture for such diversity. Using archival Hubble Space Telescope images, we associate SN 2010as with a massive cluster and derive a progenitor age of approximate to 6 Myr, assuming a single star-formation burst, which is compatible with a Wolf-Rayet progenitor. Our hydrodynamical modeling, on the contrary, indicates that the pre-explosion mass was relatively low, approximate to 4M(circle dot). The seeming contradiction between a young age and low pre-SN mass may be solved by a massive interacting binary progenitor.
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