Final Moments. III. Explosion Properties and Progenitor Constraints of CSM-interacting Type II Supernovae

Abstract We present analysis of the plateau and late-time phase properties of a sample of 39 Type II supernovae (SNe II) that show narrow, transient, high-ionization emission lines (i.e., “IIn-like”) in their early-time spectra from interaction with confined, dense circumstellar material (CSM). Originally presented by W. V. Jacobson-Galán et al., this sample also includes multicolor light curves and spectra extending to late-time phases of 35 SNe with no evidence for IIn-like features at <2 days after first light. We measure photospheric phase light-curve properties for the distance-corrected sample and find that SNe II with IIn-like features have significantly higher luminosities and decline rates at +50 days than the comparison sample, which could be connected to inflated progenitor radii, lower ejecta mass, and/or persistent CSM interaction. However, we find no statistical evidence that the measured plateau durations and 56 Ni masses of SNe II with and without IIn-like features arise from different distributions. We estimate progenitor zero-age main-sequence (ZAMS) masses for all SNe with nebular spectroscopy through spectral model comparisons and find that most objects, both with and without IIn-like features, are consistent with progenitor masses ≤12.5 M ⊙ . Combining progenitor ZAMS masses with CSM densities inferred from early-time spectra suggests multiple channels for enhanced mass loss in the final years before core collapse, such as a convection-driven chromosphere or binary interaction. Finally, we find spectroscopic evidence for ongoing ejecta-CSM interaction at radii >10 16 cm, consistent with substantial progenitor mass-loss rates of ∼10 −4 –10 −5 M ⊙ yr −1 ( v w < 50 km s −1 ) in the final centuries to millennia before explosion.

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Publication Details

Journal
The Astrophysical Journal
Published
2025-10-08
DOI
https://doi.org/10.3847/1538-4357/adfa23
Citations
4
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
4.62

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article

Final Moments. III. Explosion Properties and Progenitor Constraints of CSM-interacting Type II Supernovae

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4 citations
The Astrophysical Journal
Gamma-ray bursts and supernovae
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article

Final Moments. III. Explosion Properties and Progenitor Constraints of CSM-interacting Type II Supernovae

Jujia Zhang, R. J. Foley, C. D. Kilpatrick, J. P. Anderson, D. O. Jones, E. A. Magnier, Christa Gall, Yi Yang, Thomas de Boer, Saurabh W. Jha, C. Pellegrino, A. Rest, Kyle W. Davis, Anthony L. Piro, D. Hiramatsu, Natalie LeBaron, G. Hosseinzadeh, V. Ashley Villar, D. Farias, A. V. Filippenko, Estefania Padilla Gonzalez, R. Michael Rich, C. R. Angus, S. I. Raimundo, Shengyu Yan, Joseph Farah, R. Cartier, R. Chornock, WeiKang Zheng, K. Taggart, G. Terreran, S. Rest, D. A. Coulter, Katie Auchettl, Thomas G. Brink, Megan Newsome, W. V. Jacobson-Galán, K. Ertini, D. A. Howell, Hua Gao, Luc Dessart, C. Rojas-Bravo, M. R. Drout, Annastasia Haynie, Danial Langeroodi, Adaeze L. Ibik, A. R. Wasserman, R. Margutti, N. Earl, Huei Sears, Xiaofeng Wang, K. Azalee Bostroem, Manfred Gerlach, Fengjun Guo
article en
4 citations

Abstract

Abstract We present analysis of the plateau and late-time phase properties of a sample of 39 Type II supernovae (SNe II) that show narrow, transient, high-ionization emission lines (i.e., “IIn-like”) in their early-time spectra from interaction with confined, dense circumstellar material (CSM). Originally presented by W. V. Jacobson-Galán et al., this sample also includes multicolor light curves and spectra extending to late-time phases of 35 SNe with no evidence for IIn-like features at <2 days after first light. We measure photospheric phase light-curve properties for the distance-corrected sample and find that SNe II with IIn-like features have significantly higher luminosities and decline rates at +50 days than the comparison sample, which could be connected to inflated progenitor radii, lower ejecta mass, and/or persistent CSM interaction. However, we find no statistical evidence that the measured plateau durations and 56 Ni masses of SNe II with and without IIn-like features arise from different distributions. We estimate progenitor zero-age main-sequence (ZAMS) masses for all SNe with nebular spectroscopy through spectral model comparisons and find that most objects, both with and without IIn-like features, are consistent with progenitor masses ≤12.5 M ⊙ . Combining progenitor ZAMS masses with CSM densities inferred from early-time spectra suggests multiple channels for enhanced mass loss in the final years before core collapse, such as a convection-driven chromosphere or binary interaction. Finally, we find spectroscopic evidence for ongoing ejecta-CSM interaction at radii >10 16 cm, consistent with substantial progenitor mass-loss rates of ∼10 −4 –10 −5 M ⊙ yr −1 ( v w < 50 km s −1 ) in the final centuries to millennia before explosion.

The Astrophysical JournalVol. 992(1)
Rutgers, The State University of New Jersey (US), Northwestern University (US), University of Southern California (US), California Institute of Technology (US), University of Copenhagen (DK), Queen's University Belfast (GB), Las Cumbres Observatory Global Telescope Network (US), Centre National de la Recherche Scientifique (FR), Space Telescope Science Institute (US), Universidad de Antofagasta (CL), University of Hawaii System (US), University of Arizona (US), Johns Hopkins University (US), Consejo Nacional de Investigaciones Científicas y Técnicas (AR), University of California, Santa Barbara (US), University of Illinois Urbana-Champaign (US), University of California, Los Angeles (US), Pontificia Universidad Católica de Chile (CL), The University of Melbourne (AU), University of California, Santa Cruz (US), Chinese Academy of Sciences (CN), Yunnan Observatories (CN), Institut d'Astrophysique de Paris (FR), University of Hawaii at Hilo (US), University of California San Diego (US), Sorbonne Université (FR), Millennium Institute of Astrophysics (CL), Canadian Institute for Theoretical Astrophysics (CA), Université Bourgogne Franche-Comté (FR), Center for Astrophysics Harvard & Smithsonian (US), Carnegie Observatories (US), European Southern Observatory (CL), National Center for Supercomputing Applications (US), The NSF AI Institute for Artificial Intelligence and Fundamental Interactions (US), University of Southampton (GB), Instituto de Astrofísica de La Plata, University of Virginia (US), Universidad Nacional de La Plata (AR), University of California, Berkeley (US), Tsinghua University (CN)
National Science Foundation, Smithsonian Institution, National Aeronautics and Space Administration, W. M. Keck Foundation, John Templeton Foundation, Gordon and Betty Moore Foundation, California Institute of Technology, Aarhus Universitet, University of Washington, Johns Hopkins University, Villum Fonden, National Centre for Supercomputing Applications, Space Telescope Science Institute, European Commission, Queen's University Belfast, Durham University, Deutsche Forschungsgemeinschaft, Canada Research Chairs, National Natural Science Foundation of China, Queen's University, University of Toronto, Nuclear Safety and Security Commission, Max-Planck-Gesellschaft, National Central University, Universitetet i Oslo, Háskóli Íslands, Turun Yliopisto, Stockholms Universitet, Eötvös Loránd Tudományegyetem, Grand Équipement National De Calcul Intensif, People's Government of Yunnan Province, Agencia Nacional de Investigación y Desarrollo, Max-Planck-Institut für Astronomie, University of Illinois at Urbana-Champaign, Smithsonian Astrophysical Observatory, University of California Observatories, Science Mission Directorate, Natural Sciences and Engineering Research Council of Canada, Australian Research Council, Deutsches Elektronen-Synchrotron, Planetary Science Division, Lawrence Berkeley National Laboratory, Los Alamos National Laboratory
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Gamma-ray bursts and supernovae
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