Refereed journal article or data article (A1)
The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
List of Authors: Gutierrez CP, Bersten MC, Orellana M, Pastorello A, Ertini K, Folatelli G, Pignata G, Anderson JP, Smartt S, Sullivan M, Pursiainen M, Inserra C, Elias-Rosa N, Fraser M, Kankare E, Moran S, Reguitti A, Reynolds TM, Stritzinger M, Burke J, Frohmaier C, Galbany L, Hiramatsu D, Howell DA, Kuncarayakti H, Mattila S, Muller-Bravo T, Pellegrino C, Smith M
Publisher: OXFORD UNIV PRESS
Publication year: 2021
Journal: Monthly Notices of the Royal Astronomical Society
Journal name in source: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Journal acronym: MON NOT R ASTRON SOC
Volume number: 504
Start page: 4907
End page: 4922
Number of pages: 16
ISSN: 0035-8711
eISSN: 1365-2966
DOI: http://dx.doi.org/10.1093/mnras/stab1009
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/66402878
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.
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