The nearby Type II supernova 2024ggi beyond 600 days: circumstellar interaction and dust formation

Abstract

The Type II SN 2024ggi is one of the nearest core-collapse SNe to have exploded in recent decades. Its proximity has enabled extensive multiwavelength monitoring from early times through the nebular phase. Signatures of late-time interaction between the SN ejecta and hydrogen-rich circumstellar material (CSM) have recently been reported. Here we extend its study using late-time optical photometry and spectroscopy from 570 to 820 d after explosion. We investigate the emergence and evolution of late-time ejecta-CSM interaction and constrain the geometry of the interaction region and the properties of newly formed dust. Comparisons with other interacting SNe II and with synthetic spectra are presented. We model the Hα profile with the Monte Carlo radiative-transfer code Damocles, including both gas and dust components. Spectroscopic signatures of interaction precede the photometric flattening. The spectra evolve from ejecta-dominated to interaction-dominated as Hα develops a broad, boxy profile. The optical light curves subsequently flatten relative to the ⁵⁶Co decay rate at approximately 650-670 d. The emission lines show a systematic blue-to-red asymmetry that requires a dust component newly formed within the ejecta. The inferred dust mass formed in the ejecta is 10⁻⁶−10⁻⁵ M_⊙ if the grains are amorphous carbon or a carbon-silicate mixture, but can reach up to 10⁻³ M_⊙ for pure silicates.

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BibTeX RIS

BibTeX

@misc{ferrari2026nearby,
  title = {{The nearby Type II supernova 2024ggi beyond 600 days: circumstellar interaction and dust formation}},
  author = {L. Ferrari and G. Folatelli and C. P. Gutiérrez and A. Méndez and C. Ashall and K. Medler and K. Ertini and H. Kuncarayakti and N. Morrell and M. Stritzinger and W. Hoogendam and E. Hueichapán and R. Cartier and J. P. Anderson and M. Bersten and L. Galbany and J. L. Prieto and C. Cárdenas Uribe and S. Vazhayil},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.17140},
  eprint = {2610.17140},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.17140},
}

RIS

TY  - UNPB
TI  - The nearby Type II supernova 2024ggi beyond 600 days: circumstellar interaction and dust formation
AU  - L. Ferrari
AU  - G. Folatelli
AU  - C. P. Gutiérrez
AU  - A. Méndez
AU  - C. Ashall
AU  - K. Medler
AU  - K. Ertini
AU  - H. Kuncarayakti
AU  - N. Morrell
AU  - M. Stritzinger
AU  - W. Hoogendam
AU  - E. Hueichapán
AU  - R. Cartier
AU  - J. P. Anderson
AU  - M. Bersten
AU  - L. Galbany
AU  - J. L. Prieto
AU  - C. Cárdenas Uribe
AU  - S. Vazhayil
PY  - 2026
DA  - 2026/10/12
PB  - arXiv
DO  - 10.48550/arxiv.2610.17140
UR  - https://arxiv.org/abs/2610.17140
AB  - The Type II SN 2024ggi is one of the nearest core-collapse SNe to have exploded in recent decades. Its proximity has enabled extensive multiwavelength monitoring from early times through the nebular phase. Signatures of late-time interaction between the SN ejecta and hydrogen-rich circumstellar material (CSM) have recently been reported. Here we extend its study using late-time optical photometry and spectroscopy from 570 to 820 d after explosion. We investigate the emergence and evolution of late-time ejecta-CSM interaction and constrain the geometry of the interaction region and the properties of newly formed dust. Comparisons with other interacting SNe II and with synthetic spectra are presented. We model the Hα profile with the Monte Carlo radiative-transfer code Damocles, including both gas and dust components. Spectroscopic signatures of interaction precede the photometric flattening. The spectra evolve from ejecta-dominated to interaction-dominated as Hα develops a broad, boxy profile. The optical light curves subsequently flatten relative to the ^56Co decay rate at approximately 650-670 d. The emission lines show a systematic blue-to-red asymmetry that requires a dust component newly formed within the ejecta. The inferred dust mass formed in the ejecta is 10^−6−10^−5 M_⊙ if the grains are amorphous carbon or a carbon-silicate mixture, but can reach up to 10^−3 M_⊙ for pure silicates.
ER  -

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