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The diversity of Type II supernova versus the similarity in their progenitors

Stefano ValentiDepartment of Physics, University of California, Davis, CA 95616, USAD. A. HowellDepartment of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USAM. StritzingerDepartment of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, DenmarkM. L. GrahamDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAGriffin HosseinzadehDepartment of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USAI. ArcaviKavli Institute for Theoretical Physics, Kohn Hall, University of California, Santa Barbara, CA 93106-4030, USALars BildstenKavli Institute for Theoretical Physics, Kohn Hall, University of California, Santa Barbara, CA 93106-4030, USAAnders JerkstrandAstrophysics 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, USAA. PastorelloINAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, ItalyAnthony L. PiroCarnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USADavid SandPhysics Department, Texas Tech University, Lubbock, TX, 79409, USAStephen SmarttAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKG. TerreranAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKC. BaltayDepartment of Physics, Yale University, New Haven, CT 06520-8120, USAS. BenettiINAF Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, ItalyPeter J. BrownDepartment of Physics and Astronomy, George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, 4242 TAMU, College Station, TX 77843, USAA. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAMorgan FraserInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UKD. RabinowitzDepartment of Physics, Yale University, New Haven, CT 06520-8120, USAM. SullivanSchool of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UKF. YuanARC Centre of Excellence for All-Sky Astrophysics (CAASTRO)

2016en

ABI

Annotatsiya

High-quality collections of Type II supernova (SN) light curves are scarce because they evolve for hundreds of days, making follow-up observations time consuming and often extending over multiple observing seasons. In light of these difficulties, the diversity of SNe II is not fully understood. Here we present ultraviolet and optical photometry of 12 SNe II monitored by the Las Cumbres Observatory Global Telescope Network during 2013 to 2014, and compare them with previously studied SNe having well-sampled light curves. We explore SN II diversity by searching for correlations between the slope of the linear light-curve decay after maximum light (historically used to divide SNe II into IIL and IIP) and other measured physical properties. While SNe IIL are found to be on average more luminous than SNe IIP, SNe IIL do not appear to synthesize more 56 Ni than SNe IIP. Finally, optical nebular spectra obtained for several SNe in our sample are found to be consistent with models of red supergiant progenitors in the 12-16 M range. Consequently, SNe IIL appear not to account for the deficit of massive red supergiants as SN II progenitors.

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DOI: 10.1093/mnras/stw870

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