Carnegie Supernova Project II: The Slowest Rising Type Ia Supernova LSQ14fmg and Clues to the Origin of Super-Chandrasekhar/03fg-like Events
Author
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Hsiao, E. Y.
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Hoeflich, P.
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Ashall, C.
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Lu, J.
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Contreras, C.
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Burns, C. R.
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Phillips, M. M.
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Galbany, L.
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Anderson, J. P.
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Baltay, C.
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Baron, E.
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Castellón, S.
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Davis, S.
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Freedman, Wendy L.
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Gall, C.
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González, C.
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Graham, M. L.
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Hamuy Wackenhut, Mario
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Holoien, T. W.-S.
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Karamehmetoglu, E.
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Krisciunas, K.
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Kumar, S.
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Kuncarayakti, H.
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Morrell, N.
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Moriya, T. J.
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Nugent, P. E.
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Perlmutter, S.
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Persson, S. E.
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Piro, A. L.
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Rabinowitz, D.
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Roth, M.
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Shahbandeh, M.
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Shappee, B. J.
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Stritzinger, M. D.
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Suntzeff, N. B.
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Taddia, F.
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Uddin, S. A.
Admission date
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2021-01-25T19:06:34Z
Available date
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2021-01-25T19:06:34Z
Publication date
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2020
Cita de ítem
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Astrophysical Journal, 900 (2) 2020
es_ES
Identifier
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10.3847/1538-4357/abaf4c
Identifier
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https://repositorio.uchile.cl/handle/2250/178319
Abstract
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The Type Ia supernova (SN Ia) LSQ14fmg exhibits exaggerated properties that may help to reveal the origin of the "super-Chandrasekhar" (or 03fg-like) group. The optical spectrum is typical of a 03fg-like SN Ia, but the light curves are unlike those of any SNe Ia observed. The light curves of LSQ14fmg rise extremely slowly. At -23 rest-frame days relative toB-band maximum, LSQ14fmg is already brighter thanJandHbands, far more luminous than any 03fg-like SNe Ia with near-infrared observations. At 1 month past maximum, the optical light curves decline rapidly. The early, slow rise and flat color evolution are interpreted to result from an additional excess flux from a power source other than the radioactive decay of the synthesized Ni-56. The excess flux matches the interaction with a typical superwind of an asymptotic giant branch (AGB) star in density structure, mass-loss rate, and duration. The rapid decline starting at around 1 month pastB-band maximum may be an indication of rapid cooling by active carbon monoxide (CO) formation, which requires a low-temperature and high-density environment. These peculiarities point to an AGB progenitor near the end of its evolution and the core degenerate scenario as the likely explosion mechanism for LSQ14fmg.
es_ES
Patrocinador
dc.description.sponsorship
National Science Foundation (NSF)
AST-1008343
AST-1613426
AST-1613455
AST-1613472
AST-1008962
AST-1907570
AST1920392
AST-1911074
AST-1515927
AST1908570
AST-0908816
Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant
European Union's Horizon 2020 research and innovation program under Marie Sklodowska-Curie grant
839090
European Union (EU)
PGC2018-095317-B-C21
DiRAC Institute in the Department of Astronomy at the University of Washington
George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy
Mitchell Foundation
Academy of Finland
324504
328898
National Aeronautics & Space Administration (NASA)
80NSSC19K1717
Gordon and Betty Moore Foundation
GBMF5490
Mt. Cuba Astronomical Foundation
Ohio State University
Chinese Academy of Sciences South America Center for Astronomy (CASSACA)
Villum Foundation
Independent Research Fund Denmark (IRFD)
8021-00170B
VILLUM FONDEN
13261
28021
ESO Telescopes at the Paranal Observatory
099. D-0022(A)