JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion

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Baron, E orcid iconORCID: 0000-0001-5393-1608, Ashall, C orcid iconORCID: 0000-0002-5221-7557, DerKacy, JM orcid iconORCID: 0000-0002-7566-6080, Hoeflich, P orcid iconORCID: 0000-0002-4338-6586, Medler, K orcid iconORCID: 0000-0001-7186-105X, Shahbandeh, M orcid iconORCID: 0000-0002-9301-5302, Fereidouni, E orcid iconORCID: 0009-0001-9148-8421, Pfeffer, CM orcid iconORCID: 0000-0002-7305-8321, Mera, T orcid iconORCID: 0000-0001-5888-2542, Hoogendam, WB orcid iconORCID: 0000-0003-3953-9532, Shiber, S orcid iconORCID: 0000-0001-6107-0887, Auchettl, K orcid iconORCID: 0000-0002-4449-9152, Brown, PJ orcid iconORCID: 0000-0001-6272-5507, Burns, CR orcid iconORCID: 0000-0003-4625-6629, Burrow, A orcid iconORCID: 0000-0002-5380-0816, Coulter, DA orcid iconORCID: 0000-0003-4263-2228, Engesser, M orcid iconORCID: 0000-0003-0209-674X, Folatelli, G orcid iconORCID: 0000-0001-5247-1486, Fox, O orcid iconORCID: 0000-0003-2238-1572, Galbany, L orcid iconORCID: 0000-0002-1296-6887 et al (2025) JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion. The Astrophysical Journal, 994 (2). ISSN 0004-637X

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Abstract

We present panchromatic 0.4–21 μm observations of the nearby (∼7.2 Mpc) Type II supernova (SN) 2024ggi, obtained during the plateau phase at ∼55 days past explosion. Our data set includes JWST spectra spanning 1.7–14 μm, mid-infrared (MIR) imaging at 7.7 and 21 μm, and near-simultaneous ground-based optical and near-infrared (NIR) spectra covering 0.32−1.8 μm. The NIR and MIR spectral features of SN 2024ggi are dominated by H i emission. We present line IDs and a toy PHOENIX/1D model that reproduces the observations well, especially the continuum redward of 0.9 μm. We compare SN 2024ggi to SN 2022acko and SN 2023ixf, two other Type II SNe that were also observed by JWST, and highlight key similarities and differences in their spectral features. No evidence for a MIR excess or dust is found at these epochs, with the model matching the observed flux out to 21 μm. We discuss the model’s shortcomings, focusing on the density profile, which suppresses line blanketing and produces features in the optical that are too narrow. Our results show the power of panchromatic studies in both exploring the nature of the SN ejecta and constraining detailed models of SNe.

Item Type: Article
Uncontrolled Keywords: 5109 Space Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics; 0306 Physical Chemistry (incl. Structural); Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society
Date of acceptance: 29 September 2025
Date of first compliant Open Access: 5 June 2026
Date Deposited: 05 Jun 2026 10:26
Last Modified: 05 Jun 2026 10:26
DOI or ID number: 10.3847/1538-4357/ae0e15
URI: https://researchonline.ljmu.ac.uk/id/eprint/28746
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