A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Massive stars exploding in a He-rich circumstellar medium XI. Diverse evolution of five Ibn SNe 2020nxt, 2020taz, 2021bbv, 2023utc, and 2024aej
Tekijät: Wang, Z. -Y; Pastorello, A.; Cai, Y. -Z; Fraser, M.; Reguitti, A.; Lin, W. -l.; Tartaglia, L.; Andrew Howell, D.; Benetti, S.; Cappellaro, E.; Chen, Z. -h.; Elias-Rosa, N.; Farah, J.; Fiore, A.; Hiramatsu, D.; Kankare, E.; Li, Z. -t.; Lundqvist, P.; Mazzali, P. A.; McCully, C.; Mo, J.; Moran, S.; Newsome, M.; Padilla Gonzalez, E.; Pellegrino, C.; Peng, Z. -h.; Smartt, S. J.; Srivastav, S.; Stritzinger, M. D.; Terreran, G.; Tomasella, L.; Valerin, G.; Wang, G. -j.; Wang, X-F; de Boer, T.; Chambers, K. C.; Gao, H.; Guo, F. -z.; Gutierrez, C. P.; Kangas, T.; Karamehmetoglu, E.; Li, G. -c.; Lin, C. -c.; Lowe, T. B.; Ma, X. -r.; Magnier, E. A.; Minguez, P.; Pei, S. -p.; Reynolds, T. M.; Wainscoat, R. J.; Wang, B.; Williams, S.; Wu, C. -y.; Yan, S. -y.; Zhang, J-J; Zhang, X. -h.; Zhu, X. -J
Kustantaja: EDP SCIENCES S A
Julkaisuvuosi: 2025
Journal: Astronomy and Astrophysics
Artikkelin numero: A156
Vuosikerta: 700
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202554768
Verkko-osoite: https://www.aanda.org/articles/aa/full_html/2025/08/aa54768-25/aa54768-25.html
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/500429970
We present the photometric and spectroscopic analysis of five Type Ibn supernovae (SNe): SN 2020nxt, SN 2020taz, SN 2021bbv, SN 2023utc, and SN 2024aej. These events share key observational features and belong to a family of objects similar to the prototypical Type Ibn SN 2006jc. The SNe exhibit rise times of approximately 10 days and peak absolute magnitudes ranging from -16.5 to -19 mag. Notably, SN 2023utc is the faintest Type Ibn SN discovered to date, with an exceptionally low r-band absolute magnitude of -16.4 mag. The pseudo-bolometric light curves peak at (1 - 10)x10(42) erg s(-1), with total radiated energies on the order of (1 - 10)x10(48) erg. Spectroscopically, these SNe display a relatively slow spectral evolution. The early spectra are characterised by a hot blue continuum and prominent He I emission lines. The early spectra also show blackbody temperatures exceeding 10 000 K, with a subsequent decline in temperature during later phases. Narrow He I lines, which are indicative of unshocked circumstellar material (CSM), show velocities of approximately 1000 km s(-1). The spectra suggest that the progenitors of these SNe underwent significant mass loss prior to the explosion, resulting in a He-rich CSM. Our light curve modelling yielded estimates for the ejecta mass (M-ej) in the range 1 - 3 M-circle dot with kinetic energies (E-Kin) of (0.1 - 1)x10(50) erg. The inferred CSM mass ranges from 0.2 to 1 M-circle dot. These findings are consistent with expectations for core collapse events arising from relatively massive envelope-stripped progenitors.
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This study is supported by the National Natural Science Foundation of China (Grant Nos. 12303054,12225304), the National Key Research and Development Program of China (Grant No. 2024YFA1611603), the Yunnan Fundamental Research Projects (Grant Nos. 202401AU070063, 202501AS070078), and the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). AP, AR, SB, EC, NER, LT, GV acknowledge support from the PRIN-INAF 2022, "Shedding light on the nature of gap transients: from the observations to the models". AR also acknowledges financial support from the GRAWITA Large Program Grant (PI P. D’Avanzo). WLL is supported by the National Natural Science Foundation of China (NSFC grants 12473045, 12033003 and 12494572) and the Natural Science Foundation of Xiamen city (grant 3502Z202471015). EC acknowledges support from MIUR, PRIN 2020 (METE, grant 2020KB33TP). N.E.R. acknowledges support from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. JRF is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. (NSF 2139319). A.F. acknowledges the support by the State of Hesse within the Research Cluster ELEMENTS (Project ID 500/10.006). Shane Moran is funded by Leverhulme Trust grant RPG-2023-240. M.D. Stritzinger is funded by the Independent Research Fund Denmark (IRFD, grant number 10.46540/2032-00022B). GJW acknowledges the Africa Europe Cluster of Research Excellence (CoRE-AI) fellowship. XFW is supported by the National Natural Science Foundation of China (NSFC grants 12288102, 12033003, and 11633002) and the Tencent Xplorer Prize. CPG acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2023-151307NB-I00 SNNEXT project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant. T.K. acknowledges support from the Research Council of Finland project 360274. Song-Peng Pei is supported by the Science and Technology Foundation of Guizhou Province (QKHJC-ZK[2023]442). T.M.R is part of the Cosmic Dawn Center (DAWN), which is funded by the Danish National Research Foundation under grant DNRF140. T.M.R acknowledges support from the Research Council of Finland project 350458. C.-Y. Wu is supported by the National Natural Science Foundation of China (NSFC, Grant No.12473032), the Yunnan Revitalization Talent Support Program–Young Talent project, and the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). J.Z. is supported by the National Key R&D Program of China with No. 2021YFA1600404, the National Natural Science Foundation of China (12173082, 12333008), the Yunnan Fundamental Research Projects (grants 202401BC070007 and 202201AT070069), the Top-notch Young Talents Program of Yunnan Province, the Light of West China Program provided by the Chinese Academy of Sciences, and the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). XJZ is supported by the National Natural Science Foundation of China (Grant No. 12203004) and by the Fundamental Research Funds for the Central Universities. We acknowledge the support of the staffs of the various observatories at which data were obtained. We thank Melissa L. Graham for providing an APO-3.5m spectrum of SN 2020taz, and Kenta Taguchi for sharing a spectrum of SN 2023utc obtained through the 3.8 m Seimei Telescope. We acknowledge the support of the staff of the Xinglong 80 cm telescope (TNT). Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku, and the University of Oslo, representing Denmark, Finland, and Norway, the University of Iceland, and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Observations from the NOT were obtained through the NUTS2 collaboration which is supported in part by the Instrument Centre for Danish Astrophysics (IDA), and the Finnish Centre for Astronomy with ESO (FINCA) via Academy of Finland grant nr 306531. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Based on observations collected at Copernico and Schmidt telescopes (Asiago, Italy) of the INAF – Osservatorio Astronomico di Padova. Based on observations obtained with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes 106.216C.004/010 (D/J): ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects). 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; byproducts 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. This work makes use of data from the Las Cumbres Observatory Network and the Global Supernova Project. The LCO team is supported by U.S. NSF grants AST-1911225 and AST-1911151, and NASA. We thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grants GBMF5490 and GBMF10501 to the Ohio State University, and also funded in part by the Alfred P. Sloan Foundation grant G-2021-14192. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA), and the Villum Foundation. Pan-STARRS is a project of the Institute for Astronomy of the University of Hawaii, and is supported by the NASA SSO Near Earth Observation Program under grants 80NSSC18K0971, NNX14AM74G, NNX12AR65G, NNX13AQ47G, NNX08AR22G, 80NSSC21K1572 and by the State of Hawaii. 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 Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, STScI, NASA under grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, NSF grant AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. The Zwicky Transient Facility (ZTF) is supported by the National Science Foundation under Grants No. AST-1440341 and AST-2034437 and involves a collaboration that includes current partners such as Caltech, IPAC, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of California, Berkeley, the University of Wisconsin-Milwaukee, the University of Warwick, Ruhr University, Cornell University, Northwestern University, and Drexel University.
