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SN 2015bn: A DETAILED MULTI-WAVELENGTH VIEW OF A NEARBY SUPERLUMINOUS SUPERNOVA

M. NichollHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAE. BergerHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAStephen SmarttAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKR. MarguttiCenter for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USAA. KambleHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAK. D. AlexanderHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAChen, T. -W.Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße 1, D-85748, Garching, GermanyC. InserraAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKArcavi, I.Las Cumbres Observatory Global Telescope, 6740 Cortona Drive, Suite 102, Goleta, CA 93111, USAP. K. BlanchardHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAR. CartierSchool of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UKK. C. ChambersInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USAM. ChildressSchool of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UKR. ChornockAstrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USAP. S. CowperthwaiteHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAM. R. DroutHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAH. FlewellingInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USAMorgan FraserInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UKA. Gal‐YamBenoziyo Center for Astrophysics, Weizmann Institute of Science, Rehovot 76100, IsraelL. GalbanyMillennium Institute of Astrophysics, Vicuña Mackenna 4860, 7820436 Macul, Santiago, ChileJ. HarmanenTuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikki, FinlandHoloien, T. W. -S.Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USAGriffin HosseinzadehLas Cumbres Observatory Global Telescope, 6740 Cortona Drive, Suite 102, Goleta, CA 93111, USAD. A. HowellDepartment of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USAM. E. HuberInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USAAnders JerkstrandAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKE. KankareAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKC. S. KochanekDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USALin, Z. -Y.Institute of Astronomy, National Central University, Chung-Li 32054, TaiwanR. LunnanAstronomy Department, California Institute of Technology, Pasadena, CA 91125, USAE. A. MagnierInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USAK. MaguireAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKCurtis McCullyDepartment of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USAM. McDonaldKavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USABrian D. MetzgerColumbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USAD. MilisavljevicHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAAyan MitraCNRS, UMR 7585, Laboratoire de Physique Nucleaire et des Hautes Energies, 4 place Jussieu, F-75005 Paris, FranceT. ReynoldsNordic Optical Telescope, Apartado 474, E-38700 Santa Cruz de La Palma, SpainJ. SaarioTuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikki, FinlandB. J. ShappeeCarnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USAK. SmithAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKStefano ValentiDepartment of Physics, University of California, Davis, CA 95616, USAV. Ashley VillarHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAC. WatersInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USAD. R. YoungAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK

2016en

ABI

Annotatsiya

We present observations of SN 2015bn (= PS15ae = CSS141223-113342+004332 = MLS150211-113342+004333), a Type I superluminous supernova (SLSN) at redshift $z=0.1136$. As well as being one of the closest SLSNe I yet discovered, it is intrinsically brighter ($M_U\approx-23.1$) and in a fainter galaxy ($M_B\approx-16.0$) than other SLSNe at $z\sim0.1$. We used this opportunity to collect the most extensive dataset for any SLSN I to date, including densely-sampled spectroscopy and photometry, from the UV to the NIR, spanning $-$50 to +250 days from optical maximum. SN 2015bn fades slowly, but exhibits surprising undulations in the light curve on a timescale of 30-50 days, especially in the UV. The spectrum shows extraordinarily slow evolution except for a rapid transformation between +7 and +20-30 days. No narrow emission lines from slow-moving material are observed at any phase. We derive physical properties including the bolometric luminosity, and find slow velocity evolution and non-monotonic temperature and radial evolution. A deep radio limit rules out a healthy off-axis gamma-ray burst, and places constraints on the pre-explosion mass loss. The data can be consistently explained by a $\gtrsim10\,{\rm M}_\odot$ stripped progenitor exploding with $\sim 10^{51}\,$erg kinetic energy, forming a magnetar with a spin-down timescale of $\sim20$ days (thus avoiding a gamma-ray burst) that reheats the ejecta and drives ionization fronts. The most likely alternative scenario -- interaction with $\sim20\,{\rm M}_\odot$ of dense, inhomogeneous circumstellar material -- can be tested with continuing radio follow-up.

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DOI: 10.17863/cam.738

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