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Das, KK 
ORCID: 0000-0001-8372-997X, Kasliwal, MM ORCID: 0000-0002-5619-4938, Fremling, C ORCID: 0000-0002-4223-103X, Yang, S ORCID: 0000-0003-1546-6615, Schulze, S ORCID: 0000-0001-6797-1889, Sollerman, J, Sit, T ORCID: 0000-0001-8208-9755, De, K ORCID: 0000-0002-8989-0542, Tzanidakis, A ORCID: 0000-0003-0484-3331, Perley, DA ORCID: 0000-0001-8472-1996, Anand, S ORCID: 0000-0003-3768-7515, Andreoni, I ORCID: 0000-0002-8977-1498, Barbarino, C ORCID: 0000-0002-3821-6144, Brudge, K, Drake, A ORCID: 0000-0003-0228-6594, Gal-Yam, A ORCID: 0000-0002-3653-5598, Laher, RR ORCID: 0000-0003-2451-5482, Karambelkar, V ORCID: 0000-0003-2758-159X, Kulkarni, SR ORCID: 0000-0001-5390-8563, Masci, FJ ORCID: 0000-0002-8532-9395 et al
(2023)
Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility.
Astrophysical Journal, 959 (1).
p. 12.
ISSN 0004-637X
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Abstract
The fate of stars in the zero-age main-sequence (ZAMS) range ≈8-12 M ⊙ is unclear. They could evolve to form white dwarfs or explode as electron-capture supernovae (SNe) or iron core-collapse SNe (CCSNe). Even though the initial mass function indicates that this mass range should account for over 40% of all CCSN progenitors, few have been observationally confirmed, likely due to the faintness and rapid evolution of some of these transients. In this paper, we present a sample of nine Ca-rich/O-poor Type IIb SNe detected by the Zwicky Transient Facility with progenitors likely in this mass range. These sources have a [Ca ii] λ λ7291, 7324/[O i] λ λ6300, 6364 flux ratio of ≳2 in their nebular spectra. Comparing the measured [O i] luminosity (≲1039 erg s−1) and derived oxygen mass (≈0.01 M ⊙) with theoretical models, we infer that the progenitor ZAMS mass for these explosions is less than 12 M ⊙. The ejecta properties (M ej ≲ 1 M ⊙ and E kin ∼ 1050 erg) are also consistent. The low ejecta mass of these sources indicates a class of strongly-stripped SNe that is a transition between the regular stripped-envelope SNe and ultra-stripped SNe. The progenitor could be stripped by a main-sequence companion and result in the formation of a neutron star−main sequence binary. Such binaries have been suggested to be progenitors of neutron star−white dwarf systems that could merge within a Hubble time and be detectable with LISA.
| Item Type: | Article |
|---|---|
| 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; IOP Publishing |
| Date of acceptance: | 18 September 2023 |
| Date of first compliant Open Access: | 3 January 2024 |
| Date Deposited: | 03 Jan 2024 14:54 |
| Last Modified: | 04 Jul 2025 15:00 |
| DOI or ID number: | 10.3847/1538-4357/acfeeb |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/22165 |
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