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Observations of SN 2017ein Reveal Shock Breakout Emission and a Massive Progenitor Star for a Type Ic Supernova

Danfeng XiangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People’s Republic of ChinaXiaofeng WangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People’s Republic of ChinaJun MoPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People’s Republic of ChinaLingjun WangAstroparticle Physics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaStephen SmarttAstrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKMorgan FraserSchool of Physics, University College Dublin, Belfield, Dublin 4, IrelandSh. A. EhgamberdievUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Uzbekistan, Tashkent, 100052, UzbekistanD. O. MirzaqulovUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Uzbekistan, Tashkent, 100052, UzbekistanJujia ZhangCenter for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of ChinaTianmeng ZhangNational Astronomical Observatory of China, Chinese Academy of Sciences, Beijing, 100012, People’s Republic of ChinaJozsef VinkoDepartment of Astronomy, University of Texas at Austin, Austin, TX 78712, USAJ. Craig WheelerDepartment of Astronomy, University of Texas at Austin, Austin, TX 78712, USAGriffin HosseinzadehDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USAD. Andrew HowellDepartment of Physics, University of California, Santa Barbara, CA 93106-9530, USACurtis McCullyLas Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USAJames M DerKacyHomer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USAE. BaronHomer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USAPeter 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, USAXianfei ZhangDepartment of Astronomy, Beijing Normal University, Beijing 100875, People’s Republic of ChinaShaolan BiDepartment of Astronomy, Beijing Normal University, Beijing 100875, People’s Republic of ChinaHao SongPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People’s Republic of ChinaKaicheng ZhangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, People’s Republic of ChinaA. RestDepartment of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USAKen’ichi NomotoKavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, JapanAlexey TolstovKavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, JapanSergei BlinnikovAll-Russia Research Institute of Automatics (VNIIA), 127055, Moscow, Russia

The Astrophysical Journaljournal2019en

ABI

Аннотация

Abstract We present optical and ultraviolet observations of nearby Type Ic supernova (SN Ic) SN 2017ein, as well as a detailed analysis of its progenitor properties from both the early-time observations and the prediscovery Hubble Space Telescope ( HST ) images. The optical light curves started from within 1 day to ∼275 days after explosion, and optical spectra range from ∼2 days to ∼90 days after explosion. Compared to other normal SNe Ic like SN 2007gr and SN 2013ge, SN 2017ein seems to have more prominent C ii absorption and higher expansion velocities in early phases, suggestive of relatively lower ejecta mass. The earliest photometry obtained for SN 2017ein shows indications of shock cooling. The best fit obtained by including a shock-cooling component gives an estimate of the envelope mass as ∼0.02 M ⊙ and stellar radius as 8 ± 4 R ⊙ . Examining the pre-explosion images taken with the HST WFPC2, we find that the SN position coincides with a luminous and blue point-like source, with an extinction-corrected absolute magnitude of M V ∼ −8.2 mag and M I ∼ −7.7 mag. Comparisons of the observations to the theoretical models indicate that the counterpart source was either a single W-R star or a binary whose members had high initial masses, or a young compact star cluster. To further distinguish between different scenarios requires revisiting the site of the progenitor with HST after the SN fades away.

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DOI: 10.3847/1538-4357/aaf8b0

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