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

Media type: E-Article
Title: Characterizing the Ordinary Broad-line Type Ic SN 2023pel from the Energetic GRB 230812B
Contributor: Srinivasaragavan, Gokul P.; Swain, Vishwajeet; O’Connor, Brendan; Anand, Shreya; Ahumada, Tomás; Perley, Daniel; Stein, Robert; Sollerman, Jesper; Fremling, Christoffer; Cenko, S. Bradley; Antier, S.; Guessoum, Nidhal; Hussenot-Desenonges, Thomas; Hello, Patrice; Lesage, Stephen; Hammerstein, Erica; Miller, M. Coleman; Andreoni, Igor; Bhalerao, Varun; Bloom, Joshua S.; Dutta, Anirban; Gal-Yam, Avishay; Hinds, K-Ryan; Jaodand, Amruta; [...]
imprint: American Astronomical Society, 2024
Published in: The Astrophysical Journal Letters
Language: Not determined
DOI: 10.3847/2041-8213/ad16e7
ISSN: 2041-8205; 2041-8213
Origination:
Footnote:
Description: <jats:title>Abstract</jats:title> <jats:p>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 (<jats:italic>z</jats:italic> = 0.36) and high energy (<jats:italic>E</jats:italic> <jats:sub> <jats:italic>γ</jats:italic>,iso</jats:sub> ∼ 10<jats:sup>53</jats:sup> 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 <jats:italic>r</jats:italic>-band magnitude of <jats:italic>M</jats:italic> <jats:sub> <jats:italic>r</jats:italic> </jats:sub> = −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 <jats:italic>M</jats:italic> <jats:sub>Ni</jats:sub> = 0.38 ± 0.01 <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> and a peak bolometric luminosity of <jats:italic>L</jats:italic> <jats:sub>bol</jats:sub> ∼ 1.3 × 10<jats:sup>43</jats:sup> erg s<jats:sup>−1</jats:sup>. 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 <jats:italic>r</jats:italic> band and derive a photospheric expansion velocity of <jats:italic>v</jats:italic> <jats:sub>ph</jats:sub> = 11,300 ± 1600 km s<jats:sup>−1</jats:sup> at that phase. Extrapolating this velocity to the time of maximum light, we derive the ejecta mass <jats:italic>M</jats:italic> <jats:sub>ej</jats:sub> = 1.0 ± 0.6 <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> and kinetic energy <jats:inline-formula> <jats:tex-math> <?CDATA ${E}_{\mathrm{KE}}={1.3}_{-1.2}^{+3.3}\times {10}^{51}\,\mathrm{erg}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>E</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>KE</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.3</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>3.3</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>51</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em" /> <mml:mi>erg</mml:mi> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlad16e7ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>. 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 <jats:italic>E</jats:italic> <jats:sub> <jats:italic>γ</jats:italic>,iso</jats:sub> 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.</jats:p>
Access State: Open Access

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