Gaia17biu/SN 2017egm in NGC 3191: The Closest Hydrogen-poor Superluminous Supernova to Date Is in a “Normal,” Massive, Metal-rich Spiral Galaxy
S. BoseKavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Road 5, Hai Dian District, Beijing 100871, People’s Republic of ChinaSubo DongKavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Road 5, Hai Dian District, Beijing 100871, People’s Republic of ChinaA. PastorelloINAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyA. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAC. S. KochanekCenter for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USAJon C. MauerhanDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USACristina Romero-CañizalesMillennium Institute of Astrophysics, Santiago, ChileThomas G. BrinkDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAPing ChenKavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Road 5, Hai Dian District, Beijing 100871, People’s Republic of ChinaJose L. PrietoMillennium Institute of Astrophysics, Santiago, ChileR. S. PostPost Observatory, Lexington, MA 02421, USAC. AshallDepartment of Physics, Florida State University, 77 Chieftain Way, Tallahassee, FL 32306, USAD. GrupeDepartment of Earth and Space Science, Morehead State University, 235 Martindale Dr., Morehead, KY 40351, USAL. TomasellaINAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyS. BenettiINAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyB. J. ShappeeCarnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USAK. Z. StanekCenter for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USAZheng CaiUCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064, USAE. FalcoHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAPeter LundqvistDepartment of Astronomy and The Oskar Klein Centre, AlbaNova University Center, Stockholm University, SE-10691 Stockholm, SwedenS. MattilaTuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, FinlandR. L. MutelDepartment of Physics and Astronomy, University of Iowa, USAP. OchnerDipartimento di Fisica e Astronomia, Universit‘a di Padova, via Marzolo 8, I-35131 Padova, ItalyD. PooleyTrinity University, Department of Physics & Astronomy, One Trinity Place, San Antonio, TX 78212, USAM. StritzingerDepartment of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, DenmarkSteven VillanuevaDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAWeiKang ZhengDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAR. J. BeswickJodrell Bank Centre for Astrophysics & e-MERLIN, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UKPeter J. BrownGeorge P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy, Texas A. & M. University, Department of Physics and Astronomy, 4242 TAMU, College Station, TX 77843, USAE. CappellaroINAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyScott DavisDepartment of Physics, Florida State University, 77 Chieftain Way, Tallahassee, FL 32306, USAMorgan FraserSchool of Physics, O’Brien Centre for Science North, University College Dublin, Belfield, Dublin 4, IrelandThomas de JaegerDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAN. Elias–RosaINAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyC. GallDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkB. Scott GaudiDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAGregory J. HerczegKavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Road 5, Hai Dian District, Beijing 100871, People’s Republic of ChinaJulia HestenesDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAT. W. S. HoloienCenter for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USAGriffin HosseinzadehDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAE. Y. HsiaoDepartment of Physics, Florida State University, 77 Chieftain Way, Tallahassee, FL 32306, USAShaoming HuShandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, People’s Republic of ChinaJaejin ShinAstronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, 151-742, Republic of KoreaB. JeffersDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAR. A. KoffAntelope Hills Observatory, 980 Antelope Drive West, Bennett, CO 80102, USASahana KumarDepartment of Physics, Florida State University, 77 Chieftain Way, Tallahassee, FL 32306, USAAlexander KurtenkovInstitute of Astronomy and NAO, Bulgarian Academy of Sciences, 72 Tsarigradsko Shose Blvd., 1784 Sofia, BulgariaMarie Wingyee LauUCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064, USAS. PrenticeAstrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, UKT. ReynoldsTuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, FinlandR. J. RudySpace Science Applications Laboratory, The Aerospace Corporation, Mail Stop: M2-266, P.O. Box 92957, Los Angeles, CA 90009-2957, USAMelissa ShahbandehDepartment of Physics, Florida State University, 77 Chieftain Way, Tallahassee, FL 32306, USAA. SomeroTuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, FinlandKeivan G. StassunDepartment of Physics & Astronomy, Vanderbilt University, 6301 Stevenson Center Lane, Nashville, TN 37235, USATodd A. ThompsonCenter for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USAStefano ValentiDepartment of Physics, University of California, Davis, CA 95616, USAJong-Hak WooAstronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, 151-742, Republic of KoreaSameen YunusDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USA
2018en
ABI
Аннотация
Abstract Hydrogen-poor superluminous supernovae (SLSNe-I) have been predominantly found in low-metallicity, star-forming dwarf galaxies. Here we identify Gaia17biu/SN 2017egm as an SLSN-I occurring in a “normal” spiral galaxy (NGC 3191) in terms of stellar mass (several times 10 10 M ⊙ ) and metallicity (roughly solar). At redshift z = 0.031, Gaia17biu is also the lowest-redshift SLSN-I to date, and the absence of a larger population of SLSNe-I in dwarf galaxies of similar redshift suggests that metallicity is likely less important to the production of SLSNe-I than previously believed. With the smallest distance and highest apparent brightness for an SLSN-I, we are able to study Gaia17biu in unprecedented detail. Its pre-peak near-ultraviolet to optical color is similar to that of Gaia16apd and among the bluest observed for an SLSN-I, while its peak luminosity ( M g = −21 mag) is substantially lower than that of Gaia16apd. Thanks to the high signal-to-noise ratios of our spectra, we identify several new spectroscopic features that may help to probe the properties of these enigmatic explosions. We detect polarization at the ∼0.5% level that is not strongly dependent on wavelength, suggesting a modest, global departure from spherical symmetry. In addition, we put the tightest upper limit yet on the radio luminosity of an SLSN-I with <5.4 × 10 26 erg s −1 Hz −1 at 10 GHz, which is almost a factor of 40 better than previous upper limits and one of the few measured at an early stage in the evolution of an SLSN-I. This limit largely rules out an association of this SLSN-I with known populations of gamma-ray-burst-like central engines.
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