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| Natura: | Preprint |
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2025
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| Accesso online: | https://arxiv.org/abs/2503.01577 |
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| author | Ertini, K. Regna, T. A. Ferrari, L. Bersten, M. C. Folatelli, G. Llorca, A. Mendez Fernández-Lajús, E. Ferrero, G. A. Díaz, E. Hueichapán Cartier, R. Aguilar, L. M. Román Putkuri, C. Piccirilli, M. P. Cellone, S. A. Moreno, J. Orellana, M. Prieto, J. L. Gerlach, M. Acosta, V. Ritacco, M. J. Schujman, J. C. Valdéz, J. |
| author_facet | Ertini, K. Regna, T. A. Ferrari, L. Bersten, M. C. Folatelli, G. Llorca, A. Mendez Fernández-Lajús, E. Ferrero, G. A. Díaz, E. Hueichapán Cartier, R. Aguilar, L. M. Román Putkuri, C. Piccirilli, M. P. Cellone, S. A. Moreno, J. Orellana, M. Prieto, J. L. Gerlach, M. Acosta, V. Ritacco, M. J. Schujman, J. C. Valdéz, J. |
| contents | SN 2024ggi is a Type II supernova that exploded in the nearby galaxy NGC 3621 at a distance of approximately 7 Mpc, making it one of the closest supernovae of the decade. This SN shows clear signs of interaction with a dense circumstellar material, and several studies have investigated the properties of its possible progenitor star using pre-explosion data. In this work we aim to constrain the progenitor properties of SN 2024ggi by performing hydrodynamical modeling of its bolometric light curve and expansion velocities. We present photometric and spectroscopic observations of SN 2024ggi obtained in the Complejo Astronómico El Leoncito, in Las Campanas Observatory, and in Las Cumbres Observatory Global Telescope Network, spanning from 2 to 106 days after explosion. We constructed its bolometric light curve and we characterize it by calculating its morphological parameters. Then, we computed a grid of one dimensional explosion models for evolved stars with varying masses and estimated the properties of the progenitor star of SN 2024ggi by comparing the models to the observations. The observed bolometric luminosity and expansion velocities are well-matched by a model involving the explosion of a star in the presence of a close circumstellar material (CSM), with a zero-age main sequence mass of $\mathrm{M_{ZAMS}}$ = 15 $M_{\odot}$, a pre-SN mass and radius of 14.1 $M_{\odot}$ and 517 $R_{\odot}$, respectively, an explosion energy of $1.3\times10^{51}$ erg, and a nickel mass below 0.035 $M_{\odot}$. Our analysis suggests that the progenitor suffered a mass-loss rate of $4 \times 10^{-3}$ $M_{\odot}$yr$^{-1}$, confined to a distance of 3000 $R_{\odot}$. The CSM distribution is likely a two-component structure that consists of a compact core and an extended tail. This analysis represents the first hydrodynamical model of SN 2024ggi with a complete coverage of the plateau phase. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_01577 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | SN 2024ggi: another year, another striking Type II supernova Ertini, K. Regna, T. A. Ferrari, L. Bersten, M. C. Folatelli, G. Llorca, A. Mendez Fernández-Lajús, E. Ferrero, G. A. Díaz, E. Hueichapán Cartier, R. Aguilar, L. M. Román Putkuri, C. Piccirilli, M. P. Cellone, S. A. Moreno, J. Orellana, M. Prieto, J. L. Gerlach, M. Acosta, V. Ritacco, M. J. Schujman, J. C. Valdéz, J. High Energy Astrophysical Phenomena Solar and Stellar Astrophysics SN 2024ggi is a Type II supernova that exploded in the nearby galaxy NGC 3621 at a distance of approximately 7 Mpc, making it one of the closest supernovae of the decade. This SN shows clear signs of interaction with a dense circumstellar material, and several studies have investigated the properties of its possible progenitor star using pre-explosion data. In this work we aim to constrain the progenitor properties of SN 2024ggi by performing hydrodynamical modeling of its bolometric light curve and expansion velocities. We present photometric and spectroscopic observations of SN 2024ggi obtained in the Complejo Astronómico El Leoncito, in Las Campanas Observatory, and in Las Cumbres Observatory Global Telescope Network, spanning from 2 to 106 days after explosion. We constructed its bolometric light curve and we characterize it by calculating its morphological parameters. Then, we computed a grid of one dimensional explosion models for evolved stars with varying masses and estimated the properties of the progenitor star of SN 2024ggi by comparing the models to the observations. The observed bolometric luminosity and expansion velocities are well-matched by a model involving the explosion of a star in the presence of a close circumstellar material (CSM), with a zero-age main sequence mass of $\mathrm{M_{ZAMS}}$ = 15 $M_{\odot}$, a pre-SN mass and radius of 14.1 $M_{\odot}$ and 517 $R_{\odot}$, respectively, an explosion energy of $1.3\times10^{51}$ erg, and a nickel mass below 0.035 $M_{\odot}$. Our analysis suggests that the progenitor suffered a mass-loss rate of $4 \times 10^{-3}$ $M_{\odot}$yr$^{-1}$, confined to a distance of 3000 $R_{\odot}$. The CSM distribution is likely a two-component structure that consists of a compact core and an extended tail. This analysis represents the first hydrodynamical model of SN 2024ggi with a complete coverage of the plateau phase. |
| title | SN 2024ggi: another year, another striking Type II supernova |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2503.01577 |