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SN 2012au: A GOLDEN LINK BETWEEN SUPERLUMINOUS SUPERNOVAE AND THEIR LOWER-LUMINOSITY COUNTERPARTS

Dan MilisavljevicHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Alicia M. SoderbergHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Raffaella MarguttiHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Maria R. DroutHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]G. Howie MarionHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Nathan E. SandersHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Eric Y. HsiaoCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileRagnhild LunnanHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Ryan ChornockHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Robert A. Fesen6127 Wilder Lab, Department of Physics & Astronomy, Dartmouth College, Hanover, NH 03755, USAJerod T. Parrent6127 Wilder Lab, Department of Physics & Astronomy, Dartmouth College, Hanover, NH 03755, USAEmily M. LevesqueEdo BergerHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Ryan J. FoleyHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Pete ChallisHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Robert P. KirshnerHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Jason DittmannHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Allyson BierylaHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Atish KambleHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Sayan ChakrabortiHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected]Gisella De RosaDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAMichael FausnaughDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAKevin N. Hainline6127 Wilder Lab, Department of Physics & Astronomy, Dartmouth College, Hanover, NH 03755, USAChien-Ting Chen6127 Wilder Lab, Department of Physics & Astronomy, Dartmouth College, Hanover, NH 03755, USARyan C. Hickox6127 Wilder Lab, Department of Physics & Astronomy, Dartmouth College, Hanover, NH 03755, USANidia MorrellCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileMark M. PhillipsCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileMaximilian StritzingerDepartment of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

2013en

ABI

Annotatsiya

We present optical and near-infrared observations of SN 2012au, a slow-evolving supernova (SN) with properties that suggest a link between subsets of energetic and H-poor SNe and superluminous SNe. SN 2012au exhibited conspicuous SN Ib-like He I lines and other absorption features at velocities reaching ≈ 2×104 km s−1 in its early spectra, and a broad light curve that peaked at MB = −18.1 mag. Models of these data indicate a large explosion kinetic energy of ∼ 1052 erg and 56Ni mass ejection of MNi ≈ 0.3M⊙ on par with SN 1998bw. SN 2012au’s spectra almost one year after explosion show a blend of persistent Fe II P-Cyg absorptions and nebular emissions originating from two distinct velocity regions. These late-time emissions include strong [Fe II], [Ca II], [O I], Mg I], and Na I lines at velocities & 4500 km s−1, as well as O I and Mg I lines at noticeably smaller velocities . 2000 km s−1. Many of the late-time properties of SN 2012au are similar to the slow-evolving hypernovae SN 1997dq and SN 1997ef, and the superluminous SN 2007bi. Our observations suggest that a single explosion mechanism may unify all of these events that span −21 . MB . −17 mag. The aspherical and possibly jetted explosion was most likely initiated by the core collapse of a massive progenitor star and created substantial high-density, low-velocity Ni-rich material.

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DOI: 10.1088/2041-8205/770/2/l38

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