Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations
Wenxiong Li(Las Cumbres Observatory Global Telescope Network), Xiaofeng Wang(Tsinghua University), J. Vinkó(University of Szeged), J. Mo(Tsinghua University), G. Hosseinzadeh(Las Cumbres Observatory Global Telescope Network), David J. Sand(University of Arizona), Jujia Zhang(Chinese Academy of Sciences), H. Lin(Tsinghua University), PTSS/TNTS(Chinese Academy of Sciences), Jujia Zhang(Mitchell Institute), Lingzhi Wang(Tsinghua University), Jujia Zhang(Tsinghua University), Zhihao Chen(Tsinghua University), Danfeng Xiang(Tsinghua University), L. Rui(Shanghai Jiao Tong University), Fan Huang(Tsinghua University), Xue Li(Tsinghua University), Xiaodan Zhang(Tsinghua University), Leshan Li(University of Oklahoma), E. Baron(University of Oklahoma), James M. DerKacy(Tianjin University of Technology), Xulin Zhao(Tsinghua University), H. Sai(The University of Texas at Austin), Kaicheng Zhang(Chinese Academy of Sciences), Lingzhi Wang(Las Cumbres Observatory Global Telescope Network), LCO(Las Cumbres Observatory Global Telescope Network), D. A. Howell(Las Cumbres Observatory Global Telescope Network), C. McCully(University of California, Davis), I. Arcavi(Las Cumbres Observatory Global Telescope Network), S. Valenti(Las Cumbres Observatory Global Telescope Network), D. Hiramatsu(Space Telescope Science Institute), J. Burke(University of Notre Dame), KEGS(Australian National University), A. Rest(Space Telescope Science Institute), P. Garnavich(University of Maryland, College Park), B. Tucker(Gemini South Observatory), Gautham Narayan(Cerro Tololo Inter-American Observatory), E. Shaya(Center for Astrophysics Harvard & Smithsonian), S. Margheim(University of California, Santa Cruz), A. Zenteno(University of California, Santa Cruz), V. Ashley Villar(University of California, Santa Cruz), UCSC(University of California, Santa Cruz), G. Dimitriadis(Space Telescope Science Institute), R. J. Foley(Rutgers, The State University of New Jersey), Y. C. Pan(University of California, Santa Cruz), D. A. Coulter(Lawrence Berkeley National Laboratory), Ori D. Fox(University of California, Santa Cruz), Saurabh W. Jha(Carnegie Institution for Science), D. O. Jones(Space Telescope Science Institute), Daniel Kasen(University of California, Santa Cruz), C. D. Kilpatrick(University of Hawaii System), Anthony L. Piro(Carnegie Institution for Science), Adam G. Riess(The Ohio State University), C. Rojas-Bravo(Carnegie Institution for Science), ASAS-SN(The Ohio State University), B. J. Shappee(The Ohio State University), T. W. S. Holoien(The Ohio State University), K. Z. Stanek(Peking University), M. R. Drout(Liverpool John Moores University), Katie Auchettl, C. S. Kochanek(Peking University), J. S. Brown(Peking University), S. Bose(Aarhus University), D. Bersier(Universitat de València), J. Brimacombe(University of Iowa), Ping Chen(Post University), Subo Dong(Millennium Institute of Astrophysics), S. Holmbo(The Ohio State University), J. A. Muñoz(University of Iowa), R. L. Mutel(The Ohio State University), R. S. Post(The Ohio State University), J. L. Prieto(The Ohio State University), J. Shields(Queen's University Belfast), D. Tallon(Queen's University Belfast), Todd A. Thompson(University of Hawaiʻi at Mānoa), P. Vallely(University of Hawaiʻi at Mānoa), Steven Villanueva(University of Hawaiʻi at Mānoa), Pan-STARRS(University of Hawaiʻi at Mānoa), S. J. Smartt(University of Hawaiʻi at Mānoa), K. Smith(University of Hawaiʻi at Mānoa), K. C. Chambers(University of Hawaiʻi at Mānoa), H. Flewelling(University of Hawaiʻi at Mānoa), M. E. Huber(University of Hawaiʻi at Mānoa), E. A. Magnier(Konkoly Observatory), C. Waters(Konkoly Observatory), A. S. B. Schultz(Mitchell Institute), J. Bulger(Konkoly Observatory), T. Lowe(Konkoly Observatory), M. Willman(Konkoly Observatory), Konkoly/Texas(Konkoly Observatory), K. Sárneczky(Konkoly Observatory), András Pál(Konkoly Observatory), J. C. Wheeler(Konkoly Observatory), Attila Bódi(Konkoly Observatory), Zsófia Bognár(Konkoly Observatory), B. Csák(Konkoly Observatory), B. Cseh(Konkoly Observatory), G. Csörnyei, O. Hanyecz(Konkoly Observatory), Bernadett Ignácz(Konkoly Observatory), Csilla Kalup(Konkoly Observatory), Réka Könyves-Tóth(Konkoly Observatory), L. Kriskovics(University of Arizona), A. Ordasi(University of Arizona), I. Rajmon(University of Arizona), Á. Sódor(University of Arizona), R. Szabó(Mitchell Institute), Róbert Szakáts(Humboldt-Universität zu Berlin), Gabriella Zsidi(Lancaster University), Peter Milne(University of Pittsburgh), Jennifer E. Andrews(Centre National de la Recherche Scientifique), Nathan Smith(Lancaster University), Christopher Bilinski(University of Southampton), Swift(Queen's University Belfast), P. J. Brown(Cerro Tololo Inter-American Observatory), ePESSTO(European Southern Observatory), J. Nordin(University of Southampton), S. C. Williams(University of North Carolina at Chapel Hill), L. Galbany(University of North Carolina at Chapel Hill), J. T. Palmerio(University of North Carolina at Chapel Hill), I. Hook(University of Hawaii System), C. Inserra(University of Hawaii System), K. Maguire(University of Hawaii System), R. Cartier(University of Hawaii System), Alessandro Razza(Large Synoptic Survey Telescope Corporation), C. P. Gutiérrez(Ames Research Center), J. J. Hermes(Ames Research Center), Joshua S. Reding(Goddard Space Flight Center), Benjamin C. Kaiser(Ames Research Center), ATLAS(Ames Research Center), J. Tonry(Ames Research Center), A. Heinze(Ames Research Center), L. Denneau(Ames Research Center), H. Weiland(Ames Research Center), B. Stalder(Ames Research Center), K2 Mission Team, Geert Barentsen, Jessie Dotson, Thomas Barclay, Michael Gully-Santiago(Laboratory for Atmospheric and Space Physics), Christina Hedges(Laboratory for Atmospheric and Space Physics), Ann Marie Cody(Laboratory for Atmospheric and Space Physics), Steve B. Howell(Laboratory for Atmospheric and Space Physics), Kepler Spacecraft Team(Laboratory for Atmospheric and Space Physics), Jeffrey L. Coughlin(Laboratory for Atmospheric and Space Physics), Jeffrey E. Van Cleve(Laboratory for Atmospheric and Space Physics), José Vinícius de Miranda Cardoso(Laboratory for Atmospheric and Space Physics), K. A. Larson(Laboratory for Atmospheric and Space Physics), K. M. McCalmont-Everton(Laboratory for Atmospheric and Space Physics), C. Peterson(Laboratory for Atmospheric and Space Physics), S. Ross(Laboratory for Atmospheric and Space Physics), Lee Reedy(Laboratory for Atmospheric and Space Physics), Darren Osborne(Laboratory for Atmospheric and Space Physics), Chris McGinn(Laboratory for Atmospheric and Space Physics), L. Kohnert(Laboratory for Atmospheric and Space Physics), Lucas F. Migliorini(Laboratory for Atmospheric and Space Physics), A. Wheaton(Laboratory for Atmospheric and Space Physics), Brittany Spencer(Laboratory for Atmospheric and Space Physics), C. Labonde(Laboratory for Atmospheric and Space Physics), G. A. Rodríguez Castillo(Laboratory for Atmospheric and Space Physics), G. Beerman(Laboratory for Atmospheric and Space Physics), K. Steward(Laboratory for Atmospheric and Space Physics), M. Hanley(Laboratory for Atmospheric and Space Physics), R. Larsen(Laboratory for Atmospheric and Space Physics), R. Gangopadhyay(Laboratory for Atmospheric and Space Physics), R. Kloetzel, T. Weschler, V. Nystrom, J. Moffatt, M. Redick, K. Griest, M. Packard, M. Muszynski, Jennifer Kampmeier, R. Bjella, Sierra Flynn, B. Elsaesser
Cited by 85Open Access
Abstract
Abstract Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically confirmed Type Ia supernova (SN Ia) observed in the Kepler field. The Kepler data revealed an excess emission in its early light curve, allowing us to place interesting constraints on its progenitor system. Here we present extensive optical, ultraviolet, and near-infrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3 ± 0.3 days and Δ m 15 ( B ) = 0.96 ± 0.03 mag, but it seems to have bluer B − V colors. We construct the “UVOIR” bolometric light curve having a peak luminosity of 1.49 × 10 43 erg s −1 , from which we derive a nickel mass as 0.55 ± 0.04 M ⊙ by fitting radiation diffusion models powered by centrally located 56 Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of 56 Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a nondegenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia but is characterized by prominent and persistent carbon absorption features. The C ii features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in an SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.
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