iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Taddia, Francesco; Fremling, C.; Sollerman, J.; Corsi, A.; Gal-Yam, A.; Karamehmetoglu, E.; Lunnan, R.; Bue, B.; Ergon, M.; Kasliwal, M.; Vreeswijk, P. M.; Wozniak, Przemyslaw R.

doi:10.1051/0004-6361/201628703

Title: iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Journal Article · Thu Aug 04 00:00:00 EDT 2016 · Astronomy and Astrophysics

DOI:https://doi.org/10.1051/0004-6361/201628703· OSTI ID:1412870

Taddia, Francesco ^[1]; Fremling, C. ^[1]; Sollerman, J. ^[1]; Corsi, A. ^[2]; Gal-Yam, A. ^[3]; Karamehmetoglu, E. ^[1]; Lunnan, R. ^[4]; Bue, B. ^[5]; Ergon, M. ^[1]; Kasliwal, M. ^[6]; Vreeswijk, P. M. ^[3];

^[7]

Stockholm Univ. (Sweden). Oskar Klein Centre, Dept. of Astronomy
Texas Tech Univ., Lubbock, TX (United States). Dept. of Physics
Weizmann Inst. of Science, Rehovot (Israel). Dept. of Particle Physics & Astrophysics
California Inst. of Technology (CalTech), Pasadena, CA (United States). Dept. of Astronomy
California Inst. of Technology (CalTech), La Canada Flintridge, CA (United States). Jet Propulsion Lab.
California Inst. of Technology (CalTech), Pasadena, CA (United States). Cahill Center for Astrophysics
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

Type Ic supernovae (SNe Ic) arise from the core-collapse of H- (and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (~10-15 d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D). Here, we have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (~30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star. Methods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (~10 M_⊙) and strong ⁵⁶Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended (≳500 R_⊙), low-mass (≳0.045 M_⊙) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored. In conclusion, the large ejecta mass and the presence of H- and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive (≳35 M_⊙) WR star that experienced strong mass loss.

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Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE Laboratory Directed Research and Development (LDRD) Program; National Science Foundation (NSF); Knut and Alice Wallenberg Foundation

Grant/Contract Number:: AC52-06NA25396

OSTI ID:: 1412870

Report Number(s):: LA-UR-17-27746; TRN: US1800385

Journal Information:: Astronomy and Astrophysics, Vol. 592; ISSN 0004-6361

Publisher:: EDP SciencesCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 41 works

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