The Red Supergiant Progenitor of Type II Supernova 2024ggi

• Published in: Astrophysical journal. Letters Vol. 969; no. 1; p. L15
• Main Authors: Xiang, Danfeng, Mo, Jun, Wang, Xiaofeng, Wang, Lingzhi, Zhang, Jujia, Lin, Han, Chen, Liyang, Song, Cuiying, Liu, Liang-Duan, Wang, Zhenyu, Li, Gaici
• Format: Journal Article
• Language: English
• Published: Austin The American Astronomical Society 01.07.2024; IOP Publishing
• Subjects: Astronomical models; Hubble Space Telescope; Light curve; Luminosity; Massive stars; Metallicity; Parameters; Red giant stars; Red supergiant stars; Space telescopes; Spectral energy distribution; Spectroscopy; Stars; Stellar evolution; Stellar mass loss; Stellar models; Supergiant stars; Supernova; Supernovae; Type II supernovae; Variable stars
• ISSN: 2041-8205; 2041-8213
• DOI: 10.3847/2041-8213/ad54b3

We present a detailed analysis of the progenitor and its local environment for the recently discovered Type II supernova (SN) 2024ggi at a distance of about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space Telescope and Spitzer Space Telescope. The progenitor is identified as a red bright variable star, with absolute F814W-band magnitudes being −6.2 mag in 1995 to −7.2 mag in 2003, respectively, consistent with that of a normal red supergiant star. Combining with the historical mid-infrared light curves, a pulsational period of about 379 days can be inferred for the progenitor star. Fitting its spectral energy distribution with stellar spectral models yields the stellar parameters of temperature, radius, and bolometric luminosity as T * = 3290 − 27 + 19 K, R * = 887 − 51 + 60 R ⊙ , and log( L / L ⊙ ) = 4.92 − 0.04 + 0.05 , respectively. The above parameters indicate that the progenitor of SN 2024ggi is consistent with the stellar evolutionary track of a solar-metallicity massive star with an initial mass of 13 − 1 + 1 M ⊙ . Moreover, our analysis indicates a relatively low mass-loss rate (i.e., <3 × 10 −6 M ⊙ yr −1 ) for the progenitor compared to that inferred from flash spectroscopy and X-ray detection (i.e., 10 −2 –10 −5 M ⊙ yr −1 ), implying a significant enhancement in mass loss within a few years prior to the explosion.