SN 2024ggi in NGC 3621: Rising Ionization in a Nearby, CSM-Interacting Type II Supernova
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arXiv
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2024
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| author | Jacobson-Galán, W. V. Davis, K. W. Kilpatrick, C. D. Dessart, L. Margutti, R. Chornock, R. Foley, R. J. Arunachalam, P. Auchettl, K. Bom, C. R. Cartier, R. Coulter, D. A. Dimitriadis, G. Dickinson, D. Drout, M. R. Gagliano, A. T. Gall, C. Garretson, B. Izzo, L. Jones, D. O. LeBaron, N. Miao, H. -Y. Milisavljevic, D. Pan, Y. -C. Rest, A. Rojas-Bravo, C. Santos, A. Sears, H. Subrayan, B. M. Taggart, K. Tinyanont, S. |
| author_facet | Jacobson-Galán, W. V. Davis, K. W. Kilpatrick, C. D. Dessart, L. Margutti, R. Chornock, R. Foley, R. J. Arunachalam, P. Auchettl, K. Bom, C. R. Cartier, R. Coulter, D. A. Dimitriadis, G. Dickinson, D. Drout, M. R. Gagliano, A. T. Gall, C. Garretson, B. Izzo, L. Jones, D. O. LeBaron, N. Miao, H. -Y. Milisavljevic, D. Pan, Y. -C. Rest, A. Rojas-Bravo, C. Santos, A. Sears, H. Subrayan, B. M. Taggart, K. Tinyanont, S. |
| contents | We present UV/optical/NIR observations and modeling of supernova (SN) 2024ggi, a type II supernova (SN II) located in NGC 3621 at 7.2 Mpc. Early-time ("flash") spectroscopy of SN 2024ggi within +0.8 days of discovery shows emission lines of H I, He I, C III, and N III with a narrow core and broad, symmetric wings (i.e., IIn-like) arising from the photoionized, optically-thick, unshocked circumstellar material (CSM) that surrounded the progenitor star at shock breakout. By the next spectral epoch at +1.5 days, SN 2024ggi showed a rise in ionization as emission lines of He II, C IV, N IV/V and O V became visible. This phenomenon is temporally consistent with a blueward shift in the UV/optical colors, both likely the result of shock breakout in an extended, dense CSM. The IIn-like features in SN 2024ggi persist on a timescale of $t_{\rm IIn} = 3.8 \pm 1.6$ days at which time a reduction in CSM density allows the detection of Doppler broadened features from the fastest SN material. SN 2024ggi has peak UV/optical absolute magnitudes of $M_{\rm w2} = -18.7$ mag and $M_{\rm g} = -18.1$ mag that are consistent with the known population of CSM-interacting SNe II. Comparison of SN 2024ggi with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium (nLTE) radiative-transfer simulations suggests a progenitor mass-loss rate of $\dot{M} = 10^{-2}$M$_{\odot}$ yr$^{-1}$ ($v_w$ = 50 km/s), confined to a distance of $r < 5\times 10^{14}$ cm. Assuming a wind velocity of $v_w$ = 50 km/s, the progenitor star underwent an enhanced mass-loss episode in the last ~3 years before explosion. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2404_19006 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | SN 2024ggi in NGC 3621: Rising Ionization in a Nearby, CSM-Interacting Type II Supernova Jacobson-Galán, W. V. Davis, K. W. Kilpatrick, C. D. Dessart, L. Margutti, R. Chornock, R. Foley, R. J. Arunachalam, P. Auchettl, K. Bom, C. R. Cartier, R. Coulter, D. A. Dimitriadis, G. Dickinson, D. Drout, M. R. Gagliano, A. T. Gall, C. Garretson, B. Izzo, L. Jones, D. O. LeBaron, N. Miao, H. -Y. Milisavljevic, D. Pan, Y. -C. Rest, A. Rojas-Bravo, C. Santos, A. Sears, H. Subrayan, B. M. Taggart, K. Tinyanont, S. High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We present UV/optical/NIR observations and modeling of supernova (SN) 2024ggi, a type II supernova (SN II) located in NGC 3621 at 7.2 Mpc. Early-time ("flash") spectroscopy of SN 2024ggi within +0.8 days of discovery shows emission lines of H I, He I, C III, and N III with a narrow core and broad, symmetric wings (i.e., IIn-like) arising from the photoionized, optically-thick, unshocked circumstellar material (CSM) that surrounded the progenitor star at shock breakout. By the next spectral epoch at +1.5 days, SN 2024ggi showed a rise in ionization as emission lines of He II, C IV, N IV/V and O V became visible. This phenomenon is temporally consistent with a blueward shift in the UV/optical colors, both likely the result of shock breakout in an extended, dense CSM. The IIn-like features in SN 2024ggi persist on a timescale of $t_{\rm IIn} = 3.8 \pm 1.6$ days at which time a reduction in CSM density allows the detection of Doppler broadened features from the fastest SN material. SN 2024ggi has peak UV/optical absolute magnitudes of $M_{\rm w2} = -18.7$ mag and $M_{\rm g} = -18.1$ mag that are consistent with the known population of CSM-interacting SNe II. Comparison of SN 2024ggi with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium (nLTE) radiative-transfer simulations suggests a progenitor mass-loss rate of $\dot{M} = 10^{-2}$M$_{\odot}$ yr$^{-1}$ ($v_w$ = 50 km/s), confined to a distance of $r < 5\times 10^{14}$ cm. Assuming a wind velocity of $v_w$ = 50 km/s, the progenitor star underwent an enhanced mass-loss episode in the last ~3 years before explosion. |
| title | SN 2024ggi in NGC 3621: Rising Ionization in a Nearby, CSM-Interacting Type II Supernova |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2404.19006 |