Srinivasaragavan, GP ORCID: 0000-0002-6428-2700, Swain, V
ORCID: 0000-0002-7942-8477, O’Connor, B
ORCID: 0000-0002-9700-0036, Anand, S
ORCID: 0000-0003-3768-7515, Ahumada, T
ORCID: 0000-0002-2184-6430, Perley, D
ORCID: 0000-0001-8472-1996, Stein, R
ORCID: 0000-0003-2434-0387, Sollerman, J
ORCID: 0000-0003-1546-6615, Fremling, C
ORCID: 0000-0002-4223-103X, Cenko, SB
ORCID: 0000-0003-1673-970X, Antier, S
ORCID: 0000-0002-7686-3334, Guessoum, N
ORCID: 0000-0003-1585-8205, Hussenot-Desenonges, T
ORCID: 0009-0009-2434-432X, Hello, P, Lesage, S
ORCID: 0000-0001-8058-9684, Hammerstein, E
ORCID: 0000-0002-5698-8703, Miller, MC
ORCID: 0000-0002-2666-728X, Andreoni, I
ORCID: 0000-0002-8977-1498, Bhalerao, V
ORCID: 0000-0002-6112-7609, Bloom, JS
ORCID: 0000-0002-7777-216X et al
(2024)
Characterizing the Ordinary Broad-line Type Ic SN 2023pel from the Energetic GRB 230812B.
Astrophysical Journal Letters, 960 (2).
L18-L18.
ISSN 2041-8205
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Characterizing the Ordinary Broadline Type Ic SN 2023pel from the Energetic GRB 230812B.pdf - Published Version Available under License Creative Commons Attribution. Download (2MB) | Preview |
Abstract
We report observations of the optical counterpart of the long gamma-ray burst (GRB) GRB 230812B and its associated supernova (SN) SN 2023pel. The proximity (z = 0.36) and high energy (E γ,iso ∼ 1053 erg) make it an important event to study as a probe of the connection between massive star core collapse and relativistic jet formation. With a phenomenological power-law model for the optical afterglow, we find a late-time flattening consistent with the presence of an associated SN. SN 2023pel has an absolute peak r-band magnitude of M r = −19.46 ± 0.18 mag (about as bright as SN 1998bw) and evolves on quicker timescales. Using a radioactive heating model, we derive a nickel mass powering the SN of M Ni = 0.38 ± 0.01 M ⊙ and a peak bolometric luminosity of L bol ∼ 1.3 × 1043 erg s−1. We confirm SN 2023pel’s classification as a broad-line Type Ic SN with a spectrum taken 15.5 days after its peak in the r band and derive a photospheric expansion velocity of v ph = 11,300 ± 1600 km s−1 at that phase. Extrapolating this velocity to the time of maximum light, we derive the ejecta mass M ej = 1.0 ± 0.6 M ⊙ and kinetic energy E KE = 1.3 − 1.2 + 3.3 × 10 51 erg . We find that GRB 230812B/SN 2023pel has SN properties that are mostly consistent with the overall GRB-SN population. The lack of correlations found in the GRB-SN population between SN brightness and E γ,iso for their associated GRBs across a broad range of 7 orders of magnitude provides further evidence that the central engine powering the relativistic ejecta is not coupled to the SN powering mechanism in GRB-SN systems.
Item Type: | Article |
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Uncontrolled Keywords: | 0201 Astronomical and Space Sciences; Astronomy & Astrophysics |
Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
Divisions: | Astrophysics Research Institute |
Publisher: | American Astronomical Society |
Date of acceptance: | 9 December 2023 |
Date of first compliant Open Access: | 16 February 2024 |
Date Deposited: | 16 Feb 2024 15:22 |
Last Modified: | 04 Jul 2025 14:00 |
DOI or ID number: | 10.3847/2041-8213/ad16e7 |
URI: | https://researchonline.ljmu.ac.uk/id/eprint/22641 |
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