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iPTF 16asu: A Luminous, Rapidly Evolving, and High-velocity Supernova

L. WhitesidesDepartment of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USAR. LunnanThe Oskar Klein Centre & Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenM. M. KasliwalDepartment of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USAD. A. PerleyAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Browlow Hill, Liverpool L3 5RF, UKA. CorsiDepartment of Physics and Astronomy, Texas Tech University, Box 41051, Lubbock, TX 79409-1051, USAS. B. CenkoJoint Space-Science Institute, University of Maryland, College Park, MD 20742, USAN. BlagorodnovaDepartment of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USAY. CaoDepartment of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USAD. O. CookDepartment of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USAGary DoranJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USAD. FrederiksIoffe Institute, Politekhnicheskaya 26, St. Petersburg 194021, RussiaC. FremlingThe Oskar Klein Centre & Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenK. HurleyUniversity of California, Berkeley, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720-7450, USAE. KaramehmetogluThe Oskar Klein Centre & Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenS. R. KulkarniDepartment of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USAG. LeloudasDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl Street, Rehovot, IsraelFrank J. MasciInfrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125, USAP. NugentDepartment of Astronomy, University of California, 501 Campbell Hall, Berkeley, CA 94720-3411, USAAndreas RitterDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USAA. RubinDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl Street, Rehovot, IsraelV. SavchenkoISDC, Department of Astronomy, University of Geneva, Chemin d'Écogia, 16 CH-1290 Versoix, SwitzerlandJ. SollermanThe Oskar Klein Centre & Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenD. SvinkinIoffe Institute, Politekhnicheskaya 26, St. Petersburg 194021, RussiaF. TaddiaThe Oskar Klein Centre & Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenP. M. VreeswijkDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl Street, Rehovot, IsraelP. R. WoźniakLos Alamos National Laboratory, MS-D466, Los Alamos, NM 87545, USA

2017en

ABI

Annotatsiya

Abstract Wide-field surveys are discovering a growing number of rare transients whose physical origin is not yet well understood. Here we present optical and UV data and analysis of intermediate Palomar Transient Factory (iPTF) 16asu, a luminous, rapidly evolving, high-velocity, stripped-envelope supernova (SN). With a rest-frame rise time of just four days and a peak absolute magnitude of mag, the light curve of iPTF 16asu is faster and more luminous than that of previous rapid transients. The spectra of iPTF 16asu show a featureless blue continuum near peak that develops into an SN Ic-BL spectrum on the decline. We show that while the late-time light curve could plausibly be powered by 56 Ni decay, the early emission requires a different energy source. Nondetections in the X-ray and radio strongly constrain the energy coupled to relativistic ejecta to be at most comparable to the class of low-luminosity gamma-ray bursts (GRBs). We suggest that the early emission may have been powered by either a rapidly spinning-down magnetar or by shock breakout in an extended envelope of a very energetic explosion. In either scenario a central engine is required, making iPTF 16asu an intriguing transition object between superluminous SNe, SNe Ic-BL, and low-luminosity GRBs.

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DOI: 10.3847/1538-4357/aa99de

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