The fast, luminous ultraviolet transient AT2018cow: extreme supernova, or disruption of a star by an intermediate-mass black hole?
D. A. PerleyAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKP. A. MazzaliAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKLin YanDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAS. B. CenkoAstrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USASuvi GezariDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAK. TaggartAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKNadia BlagorodnovaDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAC. FremlingDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USABrenna MocklerDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, DK-2100 Copenhagen, DenmarkAvinash SinghIndian Institute of Astrophysics, II Block Koramangala, Bengaluru 560034, IndiaNozomu TominagaDepartment of Physics, Faculty of Science and Engineering, Konan University, 8-9-1 Okamoto, Kobe, Hyogo 658-8501, JapanMasaomi TanakaAstronomical Institute, Tohoku University, Aoba, Sendai 980-8578, JapanA. M. WatsonInstituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 México, CDMX, MéxicoTomás AhumadaDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAG. C. AnupamaIndian Institute of Astrophysics, II Block Koramangala, Bengaluru 560034, IndiaC. AshallDepartment of Physics, Florida State Universiy, Tallahassee, FL 32306, USAR. L. BecerraInstituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 México, CDMX, MéxicoD. BersierAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKV. BhaleraoPhysics Department, Indian Institute of Technology Bombay, Powai, Mumbai 400076, IndiaJ. S. BloomDepartment of Astronomy, University of California, Berkeley, CA 94720, USAN. ButlerSchool of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USAC. CopperwheatAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKM. W. CoughlinDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAKishalay DeDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAA. J. DrakeDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USADmitry A. DuevDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USASara FrederickDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAJ. González‐HernándezInstituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 México, CDMX, MéxicoA. GoobarThe Oskar Klein Centre, Department of Physics, AlbaNova, Stockholm University, SE-106 91 Stockholm, SwedenM. HeidaDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAA. Y. Q. HoDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAJ. Chuck HorstDepartment of Astronomy/Mount Laguna Observatory, San Diego State University, 5500 Campanile Drive, San Diego, CA 92812-1221, USAT. HungDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAR. ItohDepartment of Physics, School of Science, Tokyo Institute of Technology, 2-12-1 Ohokayama, Meguro, Tokyo 152-8551, JapanJ. E. JencsonDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAM. M. KasliwalDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAN. KawaiDepartment of Physics, School of Science, Tokyo Institute of Technology, 2-12-1 Ohokayama, Meguro, Tokyo 152-8551, JapanTanazza KhanamPhysics Department, Indian Institute of Technology Bombay, Powai, Mumbai 400076, IndiaS. R. KulkarniCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USABrajesh KumarIndian Institute of Astrophysics, II Block Koramangala, Bengaluru 560034, IndiaHarsh KumarPhysics Department, Indian Institute of Technology Bombay, Powai, Mumbai 400076, IndiaA. KutyrevDeleted InstitutionWilliam H. LeeInstituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 México, CDMX, MéxicoKeiichi MaedaDepartment of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, JapanAshish A MahabalCenter for Data Driven Discovery, California Institute of Technology, Pasadena, CA 91125, USAKatsuhiro L. MurataDepartment of Physics, School of Science, Tokyo Institute of Technology, 2-12-1 Ohokayama, Meguro, Tokyo 152-8551, JapanJames D. NeillDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAChow‐Choong NgeowGraduate Institute of Astronomy, National Central University, 32001 Taipei , TaiwanBryan E. PenpraseSoka University of America, 1 University Drive, Aliso Viejo, CA 92656, USAE. PianINAF OAS, Via Piero Gobetti, 101, I-40129 Bologna, ItalyR. M. QuimbyDepartment of Astronomy/Mount Laguna Observatory, San Diego State University, 5500 Campanile Drive, San Diego, CA 92812-1221, USAE. Ramírez-RuizDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, DK-2100 Copenhagen, DenmarkM. G. RicherInstituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 México, CDMX, MéxicoC. Román-ZúñigaInstituto de Astronomía UNAM, Unidad Académica en Ensenada, 22860 Ensenada BC, MéxicoD. K. SahuIndian Institute of Astrophysics, II Block Koramangala, Bengaluru 560034, IndiaShubham SrivastavPhysics Department, Indian Institute of Technology Bombay, Powai, Mumbai 400076, IndiaQ. SociaDepartment of Astronomy/Mount Laguna Observatory, San Diego State University, 5500 Campanile Drive, San Diego, CA 92812-1221, USAJ. SollermanThe Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm, SwedenY. TachibanaDepartment of Physics, School of Science, Tokyo Institute of Technology, 2-12-1 Ohokayama, Meguro, Tokyo 152-8551, JapanF. TaddiaThe Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm, SwedenSamaporn TinyanontDivision of Physics, Math, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAE. TrojaAstrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USACharlotte WardDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAJerrick WeeYale-NUS College, 16 College Avenue West, Singapore 138527, SingaporeP.-C. YuGraduate Institute of Astronomy, National Central University, 32001 Taipei , Taiwan
2018en
ABI
Annotatsiya
Wide-field optical surveys have begun to uncover large samples of fast (t_rise < 5d), luminous (M_peak < -18), blue transients. While commonly attributed to the breakout of a supernova shock into a dense wind, the great distances to the transients of this class found so far have hampered a detailed investigation of their properties until now. We present photometry and spectroscopy from a comprehensive worldwide campaign to observe AT2018cow (ATLAS18qqn), the first fast-luminous optical transient to be found in real time at low redshift. Our first spectra (<2 days after discovery) are entirely featureless. A very broad absorption feature suggestive of near-relativistic velocities develops between 3-8 days, then disappears. Broad emission features of H and He develop after >10 days. The spectrum remains extremely hot throughout its evolution, and the photospheric radius contracts with time (receding below R<10^14 cm after 1 month). This behavior does not match that of any known supernova, although a relativistic jet within a fallback supernova could explain some of the observed features. Alternatively, the transient could originate from the disruption of a star by an intermediate-mass black hole, although this would require long-lasting emission of highly super-Eddington thermal radiation. In either case, AT 2018cow suggests that the population of fast luminous transients represents a new class of astrophysical event. Intensive follow-up of this event in its late phases, and of any future events found at comparable distance, will be essential to better constrain their origins.
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