Key points are not available for this paper at this time.
We present UV/optical/NIR observations and modeling of supernova (SN) 2024ggi, a type II supernova (SN II) located in NGC 3621 at 7. 2 Mpc. Early-time ("flash") spectroscopy of SN 2024ggi within +0. 8 days of discovery shows emission lines of H I, He I, C III, and N III with a narrow core and broad, symmetric wings (i. e. , IIn-like) arising from the photoionized, optically-thick, unshocked circumstellar material (CSM) that surrounded the progenitor star at shock breakout. By the next spectral epoch at +1. 5 days, SN 2024ggi showed a rise in ionization as emission lines of He II, C IV, N IV/V and O V became visible. This phenomenon is temporally consistent with a blueward shift in the UV/optical colors, both likely the result of shock breakout in an extended, dense CSM. The IIn-like features in SN 2024ggi persist on a timescale of t ₈₈₍ = 3. 8 1. 6 days at which time a reduction in CSM density allows the detection of Doppler broadened features from the fastest SN material. SN 2024ggi has peak UV/optical absolute magnitudes of M ₖ₂ = -18. 7 mag and M ₆ = -18. 1 mag that are consistent with the known population of CSM-interacting SNe II. Comparison of SN 2024ggi with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium (nLTE) radiative-transfer simulations suggests a progenitor mass-loss rate of Ṁ = 10^-2M_ yr^-1 (vw = 50 km/s), confined to a distance of r < 5 10^14 cm. Assuming a wind velocity of vw = 50 km/s, the progenitor star underwent an enhanced mass-loss episode in the last ~3 years before explosion.
Jacobson-Galán et al. (2024) studied this question.