Early-time millimeter observations of the nearby Type II SN 2024ggi

TL;DR

This study used early ALMA millimeter observations of supernova SN 2024ggi to constrain the circumstellar environment, finding no detection but setting limits on the progenitor's mass-loss history and CSM properties.

Contribution

First multi-epoch millimeter observations of SN 2024ggi providing constraints on CSM models and progenitor mass-loss rates, highlighting the potential of early ALMA data.

Findings

Non-detection constrains CSM density and mass-loss rate.

Wind model inconsistent with early spectral features.

Eruptive model suggests a mass-loss rate of ~5×10^-3 Msun/year.

Abstract

The short-lived ionized emission lines in early spectroscopy of the nearby type II supernova SN 2024ggi signify the presence of dense circumstellar matter (CSM) close to its progenitor star. We proposed the Atacama Large Millimeter/submillimeter Array (ALMA) observations by its Director's Discretionary Time program to catch the potential synchrotron radiation associated with the ejecta-CSM interaction. Multi-epoch observations were conducted using ALMA band 6 at +8, +13, and +17 days after the discovery. The data show non-detections at the position of SN 2024ggi with a 3sigma upper limit of less than 0.15 mJy, corresponding to a luminosity of approximately 8*10^24 erg/s/Hz. In this paper, we leverage the non-detections to place constraints on the properties of CSM surrounding SN 2024ggi. We investigate both the Wind and Eruptive models for the radial distribution of CSM, assuming a constant mass-loss rate in the Wind model and a distance-variant mass-loss rate in the Eruptive model. The derived CSM distribution for the Wind model does not align with the early-time spectral features, while the ALMA observations suggest a mass-loss rate of ~ 5*10^-3 Msun/year for the Eruptive model. Conducting multi-epoch millimeter/submillimeter observations shortly after the explosion, with a cadence of a few days, could offer a promising opportunity to capture the observable signature of the Eruptive model.