Carnegie Supernova Project II: The Slowest Rising Type Ia Supernova LSQ14fmg and Clues to the Origin of Super-Chandrasekhar/03fg-like Events
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Carnegie Supernova Project II : The Slowest Rising Type Ia Supernova LSQ14fmg and Clues to the Origin of Super-Chandrasekhar/03fg-like Events. / Hsiao, E. Y.; Hoeflich, P.; Ashall, C.; Lu, J.; Contreras, C.; Burns, C. R.; Phillips, M. M.; Galbany, L.; Anderson, J. P.; Baltay, C.; Baron, E.; Castellón, S.; Davis, S.; Freedman, Wendy L.; Gall, C.; Gonzalez, C.; Graham, M. L.; Hamuy, M.; Holoien, T. W.S.; Karamehmetoglu, E.; Krisciunas, K.; Kumar, S.; Kuncarayakti, H.; Morrell, N.; Moriya, T. J.; Nugent, P. E.; Perlmutter, S.; Persson, S. E.; Piro, A. L.; Rabinowitz, D.; Roth, M.; Shahbandeh, M.; Shappee, B. J.; Stritzinger, M. D.; Suntzeff, N. B.; Taddia, F.; Uddin, S. A.
I: Astrophysical Journal, Bind 900, Nr. 2, 140, 2020.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Carnegie Supernova Project II
T2 - The Slowest Rising Type Ia Supernova LSQ14fmg and Clues to the Origin of Super-Chandrasekhar/03fg-like Events
AU - Hsiao, E. Y.
AU - Hoeflich, P.
AU - Ashall, C.
AU - Lu, J.
AU - Contreras, C.
AU - Burns, C. R.
AU - Phillips, M. M.
AU - Galbany, L.
AU - Anderson, J. P.
AU - Baltay, C.
AU - Baron, E.
AU - Castellón, S.
AU - Davis, S.
AU - Freedman, Wendy L.
AU - Gall, C.
AU - Gonzalez, C.
AU - Graham, M. L.
AU - Hamuy, M.
AU - Holoien, T. W.S.
AU - Karamehmetoglu, E.
AU - Krisciunas, K.
AU - Kumar, S.
AU - Kuncarayakti, H.
AU - Morrell, N.
AU - Moriya, T. J.
AU - Nugent, P. E.
AU - Perlmutter, S.
AU - Persson, S. E.
AU - Piro, A. L.
AU - Rabinowitz, D.
AU - Roth, M.
AU - Shahbandeh, M.
AU - Shappee, B. J.
AU - Stritzinger, M. D.
AU - Suntzeff, N. B.
AU - Taddia, F.
AU - Uddin, S. A.
N1 - Publisher Copyright: © 2020. The American Astronomical Society. All rights reserved..
PY - 2020
Y1 - 2020
N2 - 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 to B-band maximum, LSQ14fmg is already brighter than MV = -19 mag before host extinction correction. The observed color curves show a flat evolution from the earliest observation to approximately 1 week after maximum. The near-infrared light curves peak brighter than -20.5 mag in the J and H bands, 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 56Ni. 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 past B-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.
AB - 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 to B-band maximum, LSQ14fmg is already brighter than MV = -19 mag before host extinction correction. The observed color curves show a flat evolution from the earliest observation to approximately 1 week after maximum. The near-infrared light curves peak brighter than -20.5 mag in the J and H bands, 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 56Ni. 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 past B-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.
U2 - 10.3847/1538-4357/abaf4c
DO - 10.3847/1538-4357/abaf4c
M3 - Journal article
AN - SCOPUS:85091015134
VL - 900
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 140
ER -
ID: 270668727