JWST Observations of SN 2023ixf. II. The Panchromatic Evolution between 250 and 720 Days after the Explosion

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Medler, K orcid iconORCID: 0000-0001-7186-105X, Ashall, C orcid iconORCID: 0000-0002-5221-7557, Hoeflich, P orcid iconORCID: 0000-0002-4338-6586, Baron, E orcid iconORCID: 0000-0001-5393-1608, DerKacy, JM orcid iconORCID: 0000-0002-7566-6080, Shahbandeh, M orcid iconORCID: 0000-0002-9301-5302, Mera, T orcid iconORCID: 0000-0001-5888-2542, Pfeffer, CM orcid iconORCID: 0000-0002-7305-8321, Hoogendam, WB orcid iconORCID: 0000-0003-3953-9532, Jones, DO orcid iconORCID: 0000-0002-6230-0151, Shiber, S orcid iconORCID: 0000-0001-6107-0887, Fereidouni, E orcid iconORCID: 0009-0001-9148-8421, Fox, OD orcid iconORCID: 0000-0003-2238-1572, Jencson, J orcid iconORCID: 0000-0001-5754-4007, Galbany, L orcid iconORCID: 0000-0002-1296-6887, Hinkle, JT orcid iconORCID: 0000-0001-9668-2920, Tucker, MA orcid iconORCID: 0000-0002-2471-8442, Shappee, BJ orcid iconORCID: 0000-0003-4631-1149, Huber, ME orcid iconORCID: 0000-0003-1059-9603, Auchettl, K orcid iconORCID: 0000-0002-4449-9152 et al (2025) JWST Observations of SN 2023ixf. II. The Panchromatic Evolution between 250 and 720 Days after the Explosion. The Astrophysical Journal, 993 (2). p. 191. ISSN 0004-637X

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Abstract

We present the nebular phase spectroscopic and photometric observations of the nearby hydrogen-rich core-collapse supernova (CCSN) SN 2023ixf, obtained through our JWST programs. These observations, combined with ground-based optical and near-infrared spectra, cover +252.67–719.96 days, creating a comprehensive, panchromatic time-series data set spanning 0.32–30 μm. In this second paper of the series, we focus on identifying key spectral emission features and tracking their evolution through the nebular phase. The JWST data reveal hydrogen emission from the Balmer to Humphreys series, as well as prominent forbidden lines from Ne, Ar, Fe, Co, and Ni. NIRSpec observations display strong emission from the first-overtone and fundamental bands of carbon monoxide, which weaken with time as the ejecta cools and dust emission dominates. The spectral energy distribution shows a clear infrared excess emerging by +252.67 days peaking around 10.0 μm, with a secondary bump at 18.0 μm developing by +719.96 days. We suggest that this evolution could arise from multiple warm dust components. In upcoming papers in this series, we will present detailed modeling of the molecular and dust properties. Overall, this work provides the community with a unique data set that can be used to advance our understanding of the mid-infrared properties of CCSNe, offering an unprecedented resource for studying their late-time line, molecular, and dust emission.

Item Type: Article
Uncontrolled Keywords: 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
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society
Date of acceptance: 14 September 2025
Date of first compliant Open Access: 4 November 2025
Date Deposited: 04 Nov 2025 15:05
Last Modified: 04 Nov 2025 15:15
DOI or ID number: 10.3847/1538-4357/ae0736
URI: https://researchonline.ljmu.ac.uk/id/eprint/27489
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