Probing the Shock Breakout Signal of SN 2024ggi from the Transformation of Early Flash Spectroscopy

TL;DR

This study captures early spectral data of SN 2024ggi, revealing detailed interactions between the supernova shock and surrounding circumstellar material, and uncovers complex mass loss history of its red-supergiant progenitor.

Contribution

It provides the first detailed early-time spectral analysis of SN 2024ggi, revealing the structure and dynamics of the circumstellar environment and its implications for progenitor mass loss.

Findings

Detected rapid ionization increase in CSM within 63 hours.

Estimated dense CSM extending up to 4x10^{14} cm.

Revealed a high mass loss rate exceeding 5x10^{-3} M_sun/yr.

Abstract

We present early-time, hour-to-day cadence spectroscopy of the nearby type II supernova (SN II) 2024ggi, which was discovered at a phase when the SN shock just emerged from the red-supergiant (RSG) progenitor star. Over the first few days after the first light, SN 2024ggi exhibited prominent narrow emission lines formed through intense and persistent photoionization of the nearby circumstellar material (CSM). In the first 63 hours, spectral lines of He, C, N, and O revealed a rapid rise in ionization, as a result of the progressive sweeping-up of the CSM by the shock. The duration of the IIn-like spectra indicates a dense and relatively confined CSM distribution extending up to $\sim 4 \times 10^{14}$ cm. Spectral modeling reveals a CSM mass loss rate at this region exceeding $5 \times 10^{-3}{\rm M}_{\odot}$ yr$^{-1}$ is required to reproduce low-ionization emissions, which dramatically exceeds that of an RSG. Analyzing H$\alpha$ emission shift implies the velocity of the unshocked outer CSM to be between 20 and 40 km s$^{-1}$, matching the typical wind velocity of an RSG. The differences between the inner and outer layers of the CSM and an RSG progenitor highlight a complex mass loss history before the explosion of SN 2024ggi.