Diversity in Hydrogen-rich Envelope Mass of Type II Supernovae. II. SN 2023ixf as Explosion of Partially Stripped Intermediate Massive Star
: Fang, Qiliang; Moriya, Takashi J.; Ferrari, Lucía; Maeda, Keiichi; Folatelli, Gaston; Ertini, Keila Y.; Kuncarayakti, Hanindyo; Andrews, Jennifer E.; Matsumoto, Tatsuya
Publisher: IOP Publishing Ltd
: BRISTOL
: 2025
: Astrophysical Journal
: ASTROPHYSICAL JOURNAL
: ASTROPHYS J
: 36
: 978
: 1
: 10
: 0004-637X
: 1538-4357
DOI: https://doi.org/10.3847/1538-4357/ad8d5a
: https://iopscience.iop.org/article/10.3847/1538-4357/ad8d5a
: https://research.utu.fi/converis/portal/detail/Publication/485074507
SN 2023ixf is one of the most well-observed core-collapse supernovae in recent decades, yet there is inconsistency in the inferred zero-age main-sequence (ZAMS) mass M- ZAMS of its progenitor. Direct observations of the pre-supernova (SN) red supergiant (RSG) estimate M ZAMS spanning widely from 11 to 18 M- circle dot. Additional constraints, including the host environment and the pulsation of its progenitor RSG, suggest a massive progenitor with M- ZAMS > 17 M- circle dot. However, the analysis of the SN properties, from light-curve modeling to late-phase spectroscopy, favors a relatively low-mass scenario (M- ZAMS < 15 M (circle dot)). In this work, we conduct a systematic analysis of SN 2023ixf, from the RSG progenitor, plateau phase light curve to late-phase spectroscopy. Using MESA+STELLA to simulate the RSG progenitor and their explosions, we find that a range of the RSG models having M (ZAMS) that vary from 12 to 17.5 M- circle dot can reproduce its multiband light curves if the hydrogen-rich envelope mass and the explosion energy are allowed to vary. Using late-phase spectroscopy as an independent measurement, the oxygen line [O i] indicates an intermediate-massive progenitor (M- ZAMS similar to 16.0 M (circle dot)). By incorporating the velocity structure derived from the light-curve modeling into an axisymmetric model, we generated [O i] line profiles that are consistent with the [O i] line observed in late-phase spectroscopy of SN 2023ixf. Bringing these analyses together, we conclude that SN 2023ixf is the aspherical explosion of an intermediate-massive star (M- ZAMS = 15-16 M (circle dot)), with the hydrogen envelope being stripped to 4-5 M (circle dot) prior to its explosion.
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The authors would like to thank the anonymous reviewer for the comments that helped to improve the manuscript Q.F. acknowledges support from JSPS KAKENHI grant 24KF0080. T.J.M. is supported by the Grants-in-Aid for Scientific Research of the Japan Society for the Promotion of Science (JP20H00174, JP21K13966, JP21H04997). K.M. acknowledges support from JSPS KAKENHI grants JP20H00174, JP24H01810, and 24KK0070. K.M. and H.K. are supported by the JSPS bilateral program between Japan and Finland (JPJSBP120229923). T.M. acknowledges support from the Hakubi project at Kyoto University.
