A1 Refereed original research article in a scientific journal
The nebular phase of SN 2024ggi: A low-mass progenitor with no signs of interaction
Authors: Ferrari, Lucía; Folatelli, Gaston; Ertini, Keila; Kuncarayakti, Hanindyo; Regna, Tomás; Bersten, Melina C.; Ashall, Chris; Baron, Edward; Burns, Christopher R.; Galbany, Lluís; Hoogendam, Willem B.; Maeda, Keiichi; Medler, Kathryn; Morrell, Nidia Irene; Shappee, Benjamin; Stritzinger, Maximilian D.; Xiao, Hai
Publisher: EDP Sciences
Publication year: 2025
Journal: Astronomy and Astrophysics
Article number: A12
Volume: 703
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202556652
Publication's open availability at the time of reporting: Open Access
Publication channel's open availability : Open Access publication channel
Web address : https://doi.org/10.1051/0004-6361/202556652
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/505468969
Context
SN 2024ggi is a Type II supernova (SN) discovered in the nearby galaxy NGC 3621 (D ≈ 6.7 ± 0.4 Mpc) on 2024 April 03.21 UT. Its proximity has prompted a detailed investigation of the SN’s properties and its progenitor star. This work focuses on the optical evolution of SN 2024ggi at the nebular phase.
Aims
We investigate the progenitor properties and possible asymmetries in the ejecta by studying the nebular phase evolution between days 287 and 400 after the explosion.
Methods
We present the optical photometry and spectroscopy of SN 2024ggi during the nebular phase, obtained with the Las Campanas and Gemini South Observatories. Four nebular spectra were taken at 287, 288, 360, and 396 days post-explosion, supplemented by late-time uBVgri-band photometry spanning 320–400 days. The analysis of the nebular emission features was performed to probe the ejecta asymmetries. Based on the [O I] flux and [O I]/[Ca II] ratio, coupled with comparisons with spectra models from the literature, we arrived at an estimate of the progenitor mass. Additionally, we constructed the bolometric light curve from optical photometry and near-infrared data to derive the synthesized nickel mass.
Results
Our analysis suggests a progenitor zero-age main sequence mass between 12 − 15 M⊙. The late-time bolometric light curve is consistent with a synthesized 56Ni mass of 0.05 − 0.06 M⊙. The line profiles exhibit only minor changes over the observed period, suggesting roughly symmetrical ejecta, with a possible clump of oxygen-rich material moving towards the observer. There were no signatures of circumstellar material interaction detected up to 400 days after the explosion.
Downloadable publication This is an electronic reprint of the original article. |  |
Funding information in the publication:
L. F. acknowledges financial support from Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET). L.G. acknowledges financial support from AGAUR, CSIC, MCIN and AEI 10.13039/501100011033 under projects PID2023-151307NB-I00, PIE 20215AT016, CEX2020-001058-M, ILINK23001, COOPB2304, and 2021-SGR-01270. K.M. acknowledges support from NASA grants JWST-GO-02114, JWST-GO-02122, JWST-GO-04522, JWST-GO-04217, JWST-GO-04436, JWST-GO-03726, JWST-GO-05057, JWST-GO-05290, JWST-GO-06023, JWST-GO-06677, JWST-GO-06213, JWST-GO-06583. Support for programs #2114, #2122, #3726, #4217, #4436, #4522, #5057, #6023, #6213, #6583, and #6677 were provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. Some of this material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under Grant Nos. 1842402 and 2236415. Any opinions, findings, conclusions, or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. M.D. Stritzinger is funded by the Independent Research Fund Denmark (IRFD, grant number 10.46540/2032-00022B) and by an Aarhus University Research Foundation Nova project (AUFF-E-2023-9-28).
