SN 2024ggi in NGC 3621: Rising Ionization in a Nearby, Circumstellar-material-interacting Type II Supernova

Abstract We present UV–optical–near-infrared observations and modeling of supernova (SN) 2024ggi, a type II supernova (SN II) located in NGC 3621 at 7.2 Mpc. Early-time (“flash”) spectroscopy of SN 2024ggi within +0.8 days of discovery shows emission lines of H i , He i , C iii , and N iii with a narrow core and broad, symmetric wings (i.e., “IIn-like”) arising from the photoionized, optically thick, unshocked circumstellar material (CSM) that surrounded the progenitor star at shock breakout (SBO). By the next spectral epoch at +1.5 days, SN 2024ggi showed a rise in ionization as emission lines of He ii , C iv , N iv/v , and O v became visible. This phenomenon is temporally consistent with a blueward shift in the UV–optical colors, both likely the result of SBO in an extended, dense CSM. The IIn-like features in SN 2024ggi persist on a timescale of t IIn = 3.8 ± 1.6 days, at which time a reduction in CSM density allows the detection of Doppler-broadened features from the fastest SN material. SN 2024ggi has peak UV–optical absolute magnitudes of M w2 = −18.7 mag and M g = −18.1 mag, respectively, that are consistent with the known population of CSM-interacting SNe II. Comparison of SN 2024ggi with a grid of radiation hydrodynamics and non–local thermodynamic equilibrium radiative-transfer simulations suggests a progenitor mass-loss rate of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> yr −1 ( v w = 50 km s −1 ), confined to a distance of r &lt; 5 × 10 14 cm. Assuming a wind velocity of v w = 50 km s −1 , the progenitor star underwent an enhanced mass-loss episode in the last ∼3 yr before explosion.

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Publication Details

Journal
The Astrophysical Journal
Published
2024-09-01
DOI
https://doi.org/10.3847/1538-4357/ad5c64
Citations
28
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
9.28

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article

SN 2024ggi in NGC 3621: Rising Ionization in a Nearby, Circumstellar-material-interacting Type II Supernova

R. J. Foley, C. D. Kilpatrick, D. O. Jones, Christa Gall et al.
28 citations
The Astrophysical Journal
Gamma-ray bursts and supernovae
9.28
article

SN 2024ggi in NGC 3621: Rising Ionization in a Nearby, Circumstellar-material-interacting Type II Supernova

R. J. Foley, C. D. Kilpatrick, D. O. Jones, Christa Gall, G. Dimitriadis, Y. C. Pan, A. Rest, Kyle W. Davis, Samaporn Tinyanont, Natalie LeBaron, Prasiddha Arunachalam, Danielle Dickinson, Alexander Gagliano, Clécio R. Bom, Hao-Yu Miao, Angelo Santos, R. Cartier, R. Chornock, Dan Milisavljevic, K. Taggart, D. A. Coulter, Luca Izzo, Bhagya Subrayan, Katie Auchettl, W. V. Jacobson-Galán, Braden Garretson, Luc Dessart, C. Rojas-Bravo, M. R. Drout, R. Margutti, Huei Sears
article en
28 citations

Abstract

Abstract We present UV–optical–near-infrared observations and modeling of supernova (SN) 2024ggi, a type II supernova (SN II) located in NGC 3621 at 7.2 Mpc. Early-time (“flash”) spectroscopy of SN 2024ggi within +0.8 days of discovery shows emission lines of H i , He i , C iii , and N iii with a narrow core and broad, symmetric wings (i.e., “IIn-like”) arising from the photoionized, optically thick, unshocked circumstellar material (CSM) that surrounded the progenitor star at shock breakout (SBO). By the next spectral epoch at +1.5 days, SN 2024ggi showed a rise in ionization as emission lines of He ii , C iv , N iv/v , and O v became visible. This phenomenon is temporally consistent with a blueward shift in the UV–optical colors, both likely the result of SBO in an extended, dense CSM. The IIn-like features in SN 2024ggi persist on a timescale of t IIn = 3.8 ± 1.6 days, at which time a reduction in CSM density allows the detection of Doppler-broadened features from the fastest SN material. SN 2024ggi has peak UV–optical absolute magnitudes of M w2 = −18.7 mag and M g = −18.1 mag, respectively, that are consistent with the known population of CSM-interacting SNe II. Comparison of SN 2024ggi with a grid of radiation hydrodynamics and non–local thermodynamic equilibrium radiative-transfer simulations suggests a progenitor mass-loss rate of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> yr −1 ( v w = 50 km s −1 ), confined to a distance of r &lt; 5 × 10 14 cm. Assuming a wind velocity of v w = 50 km s −1 , the progenitor star underwent an enhanced mass-loss episode in the last ∼3 yr before explosion.

The Astrophysical JournalVol. 972(2)
Institut d'Astrophysique de Paris (FR)
National Science Foundation, National Aeronautics and Space Administration, Gordon and Betty Moore Foundation, University of California, Santa Cruz, Villum Fonden, Space Telescope Science Institute, National Astronomical Research Institute of Thailand, Deutsche Forschungsgemeinschaft, Canada Research Chairs, University of Toronto, Conselho Nacional de Desenvolvimento Científico e Tecnológico, Nuclear Safety and Security Commission, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Financiadora de Estudos e Projetos, National Science and Technology Council, Horizon 2020 Framework Programme, University of California Observatories, Natural Sciences and Engineering Research Council of Canada, Science and Technology Facilities Council, H2020 European Research Council
Openalex Percentile: Top 2%
Gamma-ray bursts and supernovae
9.28
DOIOpen Access PDFOpenAlex
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