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Das, KK, Kasliwal, MM, Sollerman, J, Fremling, C, Irani, I, Leung, SC, Yang, S, Wu, S, Fuller, J, Anand, S, Andreoni, I, Barbarino, C, Brink, TG, De, K, Dugas, A, Groom, SL, Helou, G, Hinds, KR, Ho, AYQ, Karambelkar, V , Kulkarni, SR, Perley, DA, Purdum, J, Regnault, N, Schulze, S, Sharma, Y, Sit, T, Sravan, N, Srinivasaragavan, GP, Stein, R, Taggart, K, Tartaglia, L, Tzanidakis, A, Wold, A, Yan, L, Yao, Y and Zolkower, J (2024) Probing Presupernova Mass Loss in Double-peaked Type Ibc Supernovae from the Zwicky Transient Facility. Astrophysical Journal, 972 (1). ISSN 0004-637X
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Probing Presupernova Mass Loss in Double-peaked Type Ibc Supernovae from the Zwicky Transient Facility.pdf - Published Version Available under License Creative Commons Attribution. Download (2MB) | Preview |
Abstract
Eruptive mass loss of massive stars prior to supernova (SN) explosion is key to understanding their evolution and end fate. An observational signature of pre-SN mass loss is the detection of an early, short-lived peak prior to the radioactive-powered peak in the lightcurve of the SN. This is usually attributed to the SN shock passing through an extended envelope or circumstellar medium. Such an early peak is common for double-peaked Type IIb SNe with an extended hydrogen envelope but uncommon for normal Type Ibc SNe with very compact progenitors. In this paper, we systematically study a sample of 14 double-peaked Type Ibc SNe out of 475 Type Ibc SNe detected by the Zwicky Transient Facility. The rate of these events is ∼3%-9% of Type Ibc SNe. A strong correlation is seen between the peak brightness of the first and the second peak. We perform a holistic analysis of this sample’s photometric and spectroscopic properties. We find that six SNe have ejecta mass less than 1.5 M ⊙. Based on the nebular spectra and lightcurve properties, we estimate that the progenitor masses for these are less than ∼12 M ⊙. The rest have an ejecta mass >2.4 M ⊙ and a higher progenitor mass. This sample suggests that the SNe with low progenitor masses undergo late-time binary mass transfer. Meanwhile, the SNe with higher progenitor masses are consistent with wave-driven mass loss or pulsation-pair instability-driven mass-loss simulations.
| Item Type: | Article |
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| Uncontrolled Keywords: | 0201 Astronomical and Space Sciences; 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics; 0306 Physical Chemistry (incl. Structural); Astronomy & Astrophysics |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | American Astronomical Society |
| SWORD Depositor: | A Symplectic |
| Date Deposited: | 03 Oct 2024 14:22 |
| Last Modified: | 03 Oct 2024 14:30 |
| DOI or ID number: | 10.3847/1538-4357/ad595f |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/24398 |
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