SN2020cpg: an energetic link between Type IIb and Ib supernovae

Medler, K ORCID: 0000-0001-7186-105X, Mazzali, PA, Teffs, J ORCID: 0000-0001-8290-2881, Prentice, SJ ORCID: 0000-0003-0486-6242, Ashall, C ORCID: 0000-0002-5221-7557, Amenouche, M, Anderson, JP ORCID: 0000-0003-0227-3451, Burke, J, Chen, TW ORCID: 0000-0002-1066-6098, Galbany, L ORCID: 0000-0002-1296-6887, Gromadzki, M ORCID: 0000-0002-1650-1518, Gutierrez, CP, Hiramatsu, D, Howell, DA, Inserra, C ORCID: 0000-0002-3968-4409, Kankare, E, McCully, C, Muller-Bravo, TE, Nicholl, M, Pellegrino, C et al (2021) SN2020cpg: an energetic link between Type IIb and Ib supernovae. Monthly Notices of the Royal Astronomical Society, 506 (2). pp. 1832-1849. ISSN 0035-8711

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Abstract

Stripped-envelope supernovae (SE-SNe) show a wide variety of photometric and spectroscopic properties. This is due to the different potential formation channels and the stripping mechanism that allows for a large diversity within the progenitors outer envelope compositions. Here, the photometric and spectroscopic observations of SN 2020cpg covering ~130 d from the explosion date are presented. SN 2020cpg (z = 0.037) is a bright SE-SNe with the B-band peaking at MB = -17.75 ± 0.39 mag and a maximum pseudo-bolometric luminosity of Lmax = 6.03 ± 0.01 × 1042 erg s-1. Spectroscopically, SN 2020cpg displays a weak high- and low-velocity H α feature during the photospheric phase of its evolution, suggesting that it contained a detached hydrogen envelope prior to explosion. From comparisons with spectral models, the mass of hydrogen within the outer envelope was constrained to be ~0.1 M⊙. From the pseudo-bolometric light curve of SN 2020cpg a 56Ni mass of MNi ~0.27 ± 0.08 M⊙ was determined using an Arnett-like model. The ejecta mass and kinetic energy of SN 2020cpg were determined using an alternative method that compares the light curve of SN 2020cpg and several modelled SE-SNe, resulting in an ejecta mass of Mejc ~5.5 ± 2.0 M⊙ and a kinetic energy of EK ~9.0 ± 3.0 × 1051 erg. The ejected mass indicates a progenitor mass of 18-25 M⊙. The use of the comparative light curve method provides an alternative process to the commonly used Arnett-like model to determine the physical properties of SE-SNe.

Item Type:	Article
Additional Information:	This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2021 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords:	Science & Technology; Physical Sciences; Astronomy & Astrophysics; supernovae: general; supernovae: individual (SN2020cpg); LIGHT CURVES; PRESUPERNOVA EVOLUTION; BINARY PROGENITOR; UBVRI PHOTOMETRY; IC SUPERNOVA; EXPLOSION; SN-1993J; HELIUM; M81; CONSTRAINTS; 0201 Astronomical and Space Sciences; Astronomy & Astrophysics
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	Oxford University Press
Date of acceptance:	16 June 2021
Date of first compliant Open Access:	9 May 2022
Date Deposited:	09 May 2022 11:40
Last Modified:	05 Jul 2025 16:15
DOI or ID number:	10.1093/mnras/stab1761
URI:	https://researchonline.ljmu.ac.uk/id/eprint/16781

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