TY - JOUR
T1 - Discovery and Extensive Follow-up of SN 2024ggi, a Nearby Type IIP Supernova in NGC 3621
AU - Chen, Ting-Wan
AU - Yang, Sheng
AU - Srivastav, Shubham
AU - Moriya, Takashi J.
AU - Smartt, Stephen J.
AU - Rest, Sofia
AU - Rest, Armin
AU - Lin, Hsing Wen
AU - Miao, Hao-Yu
AU - Cheng, Yu-Chi
AU - Aryan, Amar
AU - Cheng, Chia-Yu
AU - Fraser, Morgan
AU - Huang, Li-Ching
AU - Lee, Meng-Han
AU - Lai, Cheng-Han
AU - Liu, Yu-Hsuan
AU - Sankar.K, Aiswarya
AU - Smith, Ken W.
AU - Stevance, Heloise F.
AU - Wang, Ze-Ning
AU - Anderson, Joseph P.
AU - Angus, Charlotte R.
AU - de Boer, Thomas
AU - Chambers, Kenneth
AU - Duan, Hao-Yuan
AU - Erasmus, Nicolas
AU - Fulton, Michael
AU - Gao, Hua
AU - Herman, Joanna
AU - Hou, Wei-Jie
AU - Hsiao, Hsiang-Yao
AU - Huber, Mark E.
AU - Lin, Chien-Cheng
AU - Lin, Hung-Chin
AU - Magnier, Eugene A.
AU - MAN, Ka Kit
AU - Moore, Thomas
AU - Ngeow, Chow-Choong
AU - Nicholl, Matt
AU - Ou, Po-Sheng
AU - Pignata, Giuliano
AU - Shiau, Yu-Chien
AU - Sommer, Julian Silvester
AU - Tonry, John L.
AU - Wang, Xiao-Feng
AU - Wainscoat, Richard
AU - Young, David R.
AU - Yeh, You-Ting
AU - Zhang, Jujia
N1 - T.-W.C. and A.A. acknowledge the Yushan Young Fellow Program by the Ministry of Education, Taiwan, for the financial support (MOE-111- YSFMS-0008-001-P1). S.Y. and Z.-N.W. are supported by the National Natural Science Foundation of China under grant No. 12303046 and the Henan Province High-Level Talent Interna- tional Training Program. Numerical computations were in part carried out on the PC cluster at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. This work was supported by the JSPS Core-to-Core Program (grant No. JPJSCCA20210003). This work was funded by ANID, Millennium Science Initiative, ICN12_009. M.F. is supported by a Royal Society—Science Foundation Ireland University Research Fellowship. M.N. is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 948381) and by UK Space Agency grant No. ST/Y000692/1. G.P. acknowledges support from ANID through Millennium Science Initiative Programs ICN12 009. H.F.S. is supported by the Eric and Wendy Schmidt AI in Science Fellowship. X.W. is supported by the National Natural Science Foundation of China (NSFC grants 12288102 and 1203300) and the Tencent Xplorer Prize. J.Z. is supported by the National Key R&D Program of China with No. 2021YFA1600404, the National Natural Science Foundation of China (12173082), the Yunnan Province Founda- tion (202201AT070069), the Top-notch Young Talents Program of Yunnan Province, the Light of West China Program provided by the Chinese Academy of Sciences, the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). We acknowledge WISeREP (https://www.wiserep.org). This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. The Asteroid Terrestrial- impact Last Alert System (ATLAS) project is primarily funded to search for near-Earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; by- products of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889 and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and the Millennium Institute of Astrophysics (MAS), Chile. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard- Smithsonian Center for Astrophysics, the Las Cumbres Obser- vatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This research is based on observations made with the mission, obtained from the MAST data archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This publication has made use of data collected at Lulin Observatory, partly supported by MoST grant 109-2112-M-008-001.
Publisher Copyright:
© 2025. The Author(s). Published by the American Astronomical Society
PY - 2025/4/10
Y1 - 2025/4/10
N2 - We present the discovery and early observations of the nearby Type II supernova (SN) 2024ggi in NGC 3621 at 6.64 ± 0.3 Mpc. The SN was caught hr after its explosion by the ATLAS survey. Early-phase, high-cadence, and multiband photometric follow-up was performed by the Kilonova Finder (Kinder) project, collecting over 1000 photometric data points within 1 week. The combined o- and r-band light curves show a rapid rise of 3.3 mag in 13.7 hr, much faster than SN 2023ixf (another nearby and well-observed SN II). Between 13.8 and 18.8 hr after explosion, SN 2024ggi became bluer, with u − g color dropping from 0.53 to 0.15 mag. The rapid blueward evolution indicates a wind shock breakout (SBO) scenario. No hour-long brightening expected for the SBO from a bare stellar surface was detected during our observations. The classification spectrum, taken 17 hr after the SN explosion, shows flash features of high-ionization species such as Balmer lines, He i, C iii, and N iii. Detailed light-curve modeling provides critical insights into the circumstellar material (CSM). Our favored model has an explosion energy of 2 × 1051 erg, a mass-loss rate of 10−3 M⊙ yr−1 (with an assumed 10 km s−1 wind), and a confined CSM radius of 6 × 1014 cm. The corresponding CSM mass is 0.4 M⊙. Comparisons with SN 2023ixf highlight that SN 2024ggi has a less dense confined CSM, resulting in a faster rise and fainter UV flux. Citizen astronomer collaboration and extensive data are essential for SBO searches and detailed SN characterizations.
AB - We present the discovery and early observations of the nearby Type II supernova (SN) 2024ggi in NGC 3621 at 6.64 ± 0.3 Mpc. The SN was caught hr after its explosion by the ATLAS survey. Early-phase, high-cadence, and multiband photometric follow-up was performed by the Kilonova Finder (Kinder) project, collecting over 1000 photometric data points within 1 week. The combined o- and r-band light curves show a rapid rise of 3.3 mag in 13.7 hr, much faster than SN 2023ixf (another nearby and well-observed SN II). Between 13.8 and 18.8 hr after explosion, SN 2024ggi became bluer, with u − g color dropping from 0.53 to 0.15 mag. The rapid blueward evolution indicates a wind shock breakout (SBO) scenario. No hour-long brightening expected for the SBO from a bare stellar surface was detected during our observations. The classification spectrum, taken 17 hr after the SN explosion, shows flash features of high-ionization species such as Balmer lines, He i, C iii, and N iii. Detailed light-curve modeling provides critical insights into the circumstellar material (CSM). Our favored model has an explosion energy of 2 × 1051 erg, a mass-loss rate of 10−3 M⊙ yr−1 (with an assumed 10 km s−1 wind), and a confined CSM radius of 6 × 1014 cm. The corresponding CSM mass is 0.4 M⊙. Comparisons with SN 2023ixf highlight that SN 2024ggi has a less dense confined CSM, resulting in a faster rise and fainter UV flux. Citizen astronomer collaboration and extensive data are essential for SBO searches and detailed SN characterizations.
UR - http://www.scopus.com/inward/record.url?scp=105003028528&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/adb428
DO - 10.3847/1538-4357/adb428
M3 - Journal article
SN - 0004-637X
VL - 983
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 86
ER -
