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The Spectacular Ultraviolet Flash from the Peculiar Type Ia Supernova 2019yvq

Miller, AACenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, 1800 Sherman Road, Evanston, IL 60201, USAMagee, MRSchool of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, IrelandAbigail PolinDepartments of Physics and Astronomy, University of California, Berkeley, Berkley, CA 94720, USAK. MaguireSchool of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, IrelandE. ZimmermanDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, 76100 Rehovot, IsraelYuhan YaoCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAJ. SollermanDepartment of Astronomy, The Oskar Klein Center, Stockholm University, AlbaNova, SE-10691 Stockholm, SwedenS. SchulzeDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, 76100 Rehovot, IsraelPerley, DAAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKMarkus KromerHeidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, GermanySuhail DhawanThe Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-10691 Stockholm, SwedenMattia BullaNordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, SE-106 91 Stockholm, SwedenIgor AndreoniCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USABellm, ECDIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, USAKishalay DeCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USARichard DekanyCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAAlex DelacroixCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAC. FremlingCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAA. Gal‐YamDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, 76100 Rehovot, IsraelGoldstein, DACahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAGolkhou, VZThe eScience Institute, University of Washington, Seattle, WA 98195, USAA. GoobarThe Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-10691 Stockholm, SwedenGraham, MJCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAI. IraniDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, 76100 Rehovot, IsraelKasliwal, MMCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAStephen KayeCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAKim, Y-LUniversité de Lyon, Université Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, F-69622, Villeurbanne, FranceLaher, RRIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USAMahabal, AACenter for Data Driven Discovery, California Institute of Technology, Pasadena, CA 91125, USAMasci, FJIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USANugent, PEDepartments of Physics and Astronomy, University of California, Berkeley, Berkley, CA 94720, USAE. O. OfekDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, 76100 Rehovot, IsraelPhinney, ESCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAPrentice, SJSchool of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, IrelandReed RiddleCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAM. RigaultUniversité Clermont Auvergne, CNRS/IN2P3, Laboratoire de Physique de Clermont, F-63000 Clermont-Ferrand, FranceBen RusholmeIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USAT. SchweyerDepartment of Astronomy, The Oskar Klein Center, Stockholm University, AlbaNova, SE-10691 Stockholm, SwedenShupe, DLIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USASoumagnac, MTLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAG. TerreranCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, 1800 Sherman Road, Evanston, IL 60201, USARichard WaltersCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USALin YanCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USAJeffry ZolkowerCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAKulkarni, SRCahill Center for Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA

2020en

ABI

Annotatsiya

Early observations of Type Ia supernovae (SNe Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN 2019yvq, the second observed SN Ia, after iPTF 14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN 2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for an SN Ia (${M}_{g}\\approx -18.5$ mag at peak) yet featured very high absorption velocities ($v\\approx 15{\\rm{,0}}00$ km s−1 for Si ii λ6355 at peak). We find that many of the observational features of SN 2019yvq, aside from the flash, can be explained if the explosive yield of radioactive 56Ni is relatively low (we measure ${M}_{{56}_{\\mathrm{Ni}}}=0.31\\pm 0.05\\,{M}_{\\odot }$) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN 2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of 56Ni in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN 2019yvq. In closing, we predict that the nebular spectra of SN 2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca ii] emission, if it was a double detonation, or narrow [O i] emission, if it was due to a violent merger.

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