The double-peaked type Ic Supernova 2019cad: another SN 2005bf-like object
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Oxford University Press
Supernovae: generalSupernovae: individual: SN 2019cad
Published version: Gutiérrez, C. P... [et al.] (2021). The double-peaked type Ic Supernova 2019cad: another SN 2005bf-like object. Monthly Notices of the Royal Astronomical Society. [https://doi.org/10.1093/mnras/stab1009]
SponsorshipEuropean Commission 615929; UNRN PI2018 40B696; Ministry of Education, Universities and Research (MIUR); Research Projects of National Relevance (PRIN) 20179ZF5KS; Science Foundation Ireland; Magnus Ehrnrooth foundation; Vilho, Yrjo and Kalle Vaisala Foundation of the Finnish academy of Science and Letters; VILLUM FONDEN 13261 28021; Independent Research Fund Denmark - European Union'sHorizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant 839090; National Science Foundation (NSF) AST-1911225; CONICYT PFCHA/DOCTORADOBECAS CHILE/2017-72180113; Spanish grant within the European Funds for Regional Development (FEDER) PGC2018-095317-B-C21; Instrument Centre for Danish Astrophysics (IDA); National Aeronautics & Space Administration (NASA) NN12AR55G 80NSSC18K0284 80NSSC18K1575; UK Research & Innovation (UKRI); Science & Technology Facilities Council (STFC); ANID -Millennium Science Initiative ICN12 009; Jenny and AnttiWihuri foundation; ANID BECAS/DOCTORADO NACIONAL 21202412 W19AN003
We present the photometric and spectroscopic evolution of supernova (SN) 2019cad during the first similar to 100 d from explosion. Based on the light-curve morphology, we find that SN 2019cad resembles the double-peaked Type Ib/c SN 2005bf and the Type Ic PTF11mnb. Unlike those two objects, SN 2019cad also shows the initial peak in the redder bands. Inspection of the g-band light curve indicates the initial peak is reached in similar to 8 d, while the r-band peak occurred similar to 15 d post-explosion. A second and more prominent peak is reached in all bands at similar to 45 d past explosion, followed by a fast decline from similar to 60 d. During the first 30 d, the spectra of SN 2019cad show the typical features of a Type Ic SN, however, after 40 d, a blue continuum with prominent lines of Si II lambda 6355 and C II lambda 6580 is observed again. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2019cad is consistent with a pre-SN mass of 11 M-circle dot, and an explosion energy of 3.5 x 10(51) erg. The light-curve morphology can be reproduced either by a double-peaked Ni-56 distribution with an external component of 0.041 M-circle dot, and an internal component of 0.3 M-circle dot or a double-peaked Ni-56 distribution plus magnetar model (P similar to 11 ms and B similar to 26 x 10(14) G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the Ni-56 model would require extreme values, while the magnetar model would still be feasible.