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Characterizing the Ordinary Broad-line Type Ic SN 2023pel from the Energetic GRB 230812B

Srinivasaragavan, GP, Swain, V, O’Connor, B, Anand, S, Ahumada, T, Perley, D, Stein, R, Sollerman, J, Fremling, C, Cenko, SB, Antier, S, Guessoum, N, Hussenot-Desenonges, T, Hello, P, Lesage, S, Hammerstein, E, Miller, MC, Andreoni, I, Bhalerao, V, Bloom, JS , Dutta, A, Gal-Yam, A, Hinds, KR, Jaodand, A, Kasliwal, M, Kumar, H, Kutyrev, AS, Ragosta, F, Ravi, V, Sharma, K, Singh Teja, R, Yang, S, Anupama, GC, Bellm, EC, Coughlin, MW, Mahabal, AA, Masci, FJ, Pathak, U, Purdum, J, Roberts, OJ, Smith, R and Wold, A (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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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
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
SWORD Depositor: A Symplectic
Date Deposited: 16 Feb 2024 15:22
Last Modified: 16 Feb 2024 15:30
DOI or ID number: 10.3847/2041-8213/ad16e7
URI: https://researchonline.ljmu.ac.uk/id/eprint/22641
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