Far-ultraviolet to Near-infrared Observations of SN 2023ixf: A High-energy Explosion Engulfed in Complex Circumstellar Material

We present early-phase panchromatic photometric and spectroscopic coverage spanning the far-ultraviolet to near-infrared regime of the nearest hydrogen-rich core-collapse supernova (SN) in the last 25 yr, SN 2023ixf. We observe early “flash” features in the optical spectra due to confined dense circ...

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Published in:Astrophysical journal. Letters 2023-09, Vol.954 (1), p.L12
Main Authors: Teja, Rishabh Singh, Singh, Avinash, Basu, Judhajeet, Anupama, G. C., Sahu, D. K., Dutta, Anirban, Swain, Vishwajeet, Nakaoka, Tatsuya, Pathak, Utkarsh, Bhalerao, Varun, Barway, Sudhanshu, Kumar, Harsh, A. J., Nayana, Imazawa, Ryo, Kumar, Brajesh, Kawabata, Koji S.
Format: Article
Language:English
Subjects:
Absorption
Core-collapse supernovae
Ejecta
Emissions
Explosions
Extreme ultraviolet astronomy
Far ultraviolet radiation
H alpha line
Infrared photometry
Ionization
Near infrared astronomy
Near infrared observations
Observational astronomy
Red giant stars
Supergiant stars
Supernova
Type II supernovae
Ultraviolet spectra
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Summary:We present early-phase panchromatic photometric and spectroscopic coverage spanning the far-ultraviolet to near-infrared regime of the nearest hydrogen-rich core-collapse supernova (SN) in the last 25 yr, SN 2023ixf. We observe early “flash” features in the optical spectra due to confined dense circumstellar material (CSM). We observe high-ionization absorption lines (Fe ii , Mg ii ) in the ultraviolet spectra from very early on. We also observe a multipeaked emission profile of H α in the spectrum beginning at ∼16 days, which indicates ongoing interaction of the SN ejecta with a preexisting shell-shaped CSM having an inner radius of ∼75 au and an outer radius of ∼140 au. The shell-shaped CSM is likely a result of enhanced mass loss ∼35–65 yr before the explosion assuming a standard red supergiant wind. The UV spectra are dominated by multiple highly ionized narrow absorption and broad emission features from elements such as C, N, O, Si, Fe, and Ni. Based on early light-curve models of Type II SNe, we infer that the nearby dense CSM confined to 7 ± 3 × 10 14 cm (∼45 au) is a result of enhanced mass loss (10 −3.0±0.5 M ⊙ yr −1 ) two decades before the explosion.
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/acef20