Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi

Abstract We present high-cadence photometric and spectroscopic observations of supernova (SN) 2024ggi, a Type II SN with flash spectroscopy features, which exploded in the nearby galaxy NGC 3621 at ∼7 Mpc. The light-curve evolution over the first 30 hr can be fit by two power-law indices with a break after 22 hr, rising from M V ≈ −12.95 mag at +0.66 day to M V ≈ −17.91 mag after 7 days. In addition, the densely sampled color curve shows a strong blueward evolution over the first few days and then behaves as a normal SN II with a redward evolution as the ejecta cool. Such deviations could be due to interaction with circumstellar material (CSM). Early high- and low-resolution spectra clearly show high-ionization flash features from the first spectrum to +3.42 days after the explosion. From the high-resolution spectra, we calculate the CSM velocity to be 37 ± 4 km s −1 . We also see the line strength evolve rapidly from 1.22 to 1.49 days in the earliest high-resolution spectra. Comparison of the low-resolution spectra with CMFGEN models suggests that the pre-explosion mass-loss rate of SN 2024ggi falls in the range of 10 −3 –10 −2 M ☉ yr −1 , which is similar to that derived for SN 2023ixf. However, the rapid temporal evolution of the narrow lines in the spectra of SN 2024ggi ( R CSM ∼ 2.7 × 10 14 cm) could indicate a smaller spatial extent of the CSM than in SN 2023ixf ( R CSM ∼ 5.4 × 10 14 cm), which in turn implies a lower total CSM mass for SN 2024ggi.

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Publication Details

Journal
The Astrophysical Journal Letters
Published
2024-08-26
DOI
https://doi.org/10.3847/2041-8213/ad6907
Citations
36
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
11.93

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article

Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi

Jujia Zhang, M. Lundquist, G. E. Medina, Yi Yang et al.
36 citations
The Astrophysical Journal Letters
Gamma-ray bursts and supernovae
11.93
article

Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi

Jujia Zhang, M. Lundquist, G. E. Medina, Yi Yang, Lindsey A. Kwok, Daryl Janzen, Ting S. Li, Saurabh W. Jha, C. Pellegrino, Nathan Smith, Jeniveve Pearson, Jacob E. Jencson, Aravind P. Ravi, P. J. Brown, Brad E. Tucker, Jennifer E. Andrews, D. Hiramatsu, G. Hosseinzadeh, Estefania Padilla Gonzalez, J. C. Wheeler, Michaela Schwab, Ricardo R. Muñoz, Yize Dong, Emily Hoang, S. Valenti, Joseph Farah, David J. Sand, Darshana Mehta, N. Meza, G. Terreran, C. McCully, C. P. Gutiérrez, Brian Hsu, Megan Newsome, D. A. Howell, Anjasha Gangopadhyay, Manisha Shrestha, Colin W. Macrie, Aidan Martas, Xiaofeng Wang, K. Azalee Bostroem, Qian Zhai, Paula Diaz
article en
36 citations

Abstract

Abstract We present high-cadence photometric and spectroscopic observations of supernova (SN) 2024ggi, a Type II SN with flash spectroscopy features, which exploded in the nearby galaxy NGC 3621 at ∼7 Mpc. The light-curve evolution over the first 30 hr can be fit by two power-law indices with a break after 22 hr, rising from M V ≈ −12.95 mag at +0.66 day to M V ≈ −17.91 mag after 7 days. In addition, the densely sampled color curve shows a strong blueward evolution over the first few days and then behaves as a normal SN II with a redward evolution as the ejecta cool. Such deviations could be due to interaction with circumstellar material (CSM). Early high- and low-resolution spectra clearly show high-ionization flash features from the first spectrum to +3.42 days after the explosion. From the high-resolution spectra, we calculate the CSM velocity to be 37 ± 4 km s −1 . We also see the line strength evolve rapidly from 1.22 to 1.49 days in the earliest high-resolution spectra. Comparison of the low-resolution spectra with CMFGEN models suggests that the pre-explosion mass-loss rate of SN 2024ggi falls in the range of 10 −3 –10 −2 M ☉ yr −1 , which is similar to that derived for SN 2023ixf. However, the rapid temporal evolution of the narrow lines in the spectra of SN 2024ggi ( R CSM ∼ 2.7 × 10 14 cm) could indicate a smaller spatial extent of the CSM than in SN 2023ixf ( R CSM ∼ 5.4 × 10 14 cm), which in turn implies a lower total CSM mass for SN 2024ggi.

The Astrophysical Journal LettersVol. 972(1)
Rutgers, The State University of New Jersey (US), Australian National University (AU), California Institute of Technology (US), Las Cumbres Observatory Global Telescope Network (US), Institute of Space Sciences (ES), University of Arizona (US), University of California, Santa Barbara (US), Stockholm University (SE), University of Toronto (CA), Chinese Academy of Sciences (CN), W.M. Keck Observatory (US), Yunnan Observatories (CN), Mount Stromlo Observatory (AU), University of Saskatchewan (CA), Institut d'Estudis Espacials de Catalunya (ES), Gemini North Observatory (US), Université Bourgogne Franche-Comté (FR), Center for Astrophysics Harvard & Smithsonian (US), The NSF AI Institute for Artificial Intelligence and Fundamental Interactions (US), Infrared Processing and Analysis Center (US), University of Virginia (US), University of Chile (CL), University of California, Davis (US), The University of Texas at Austin (US), Texas A&M University (US), Universitat Politècnica de Catalunya (ES), Tsinghua University (CN)
National Science Foundation, National Aeronautics and Space Administration, John Templeton Foundation, California Institute of Technology, Heising-Simons Foundation, University of Leicester, European Commission, National Natural Science Foundation of China, Generalitat de Catalunya, University of Toronto, Ministerio de Ciencia e Innovación, People's Government of Yunnan Province, Ministério da Ciência, Tecnologia, Inovações e Comunicações, Agencia Nacional de Investigación y Desarrollo, Natural Sciences and Engineering Research Council of Canada, Agencia Estatal de Investigación, Astrophysics Division
Openalex Percentile: Top 1%
Gamma-ray bursts and supernovae
11.93
DOIOpen Access PDFOpenAlex
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