A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
The nearby He-rich superluminous supernova SN 2021bnw during photospheric phases; 
Tekijät: Fiore, A.; Kozyreva, A.; Yan, L.; Benetti, S.; Anderson, J. P.; Baklanov, P.; Cai, Y.-Z.; Cappellaro, E.; Chen, T.-W.; Elias-Rosa, N.; Gal-Yam, A.; Graham, M. J.; Gromadzki, M.; Groom, S. L.; Gutiérrez, C. P.; Hiramatsu, D.; Howell, D. A.; Inserra, C.; Kasliwal, M. M.; Könyves-Tóth, R.; Lundqvist, P.; McCully, C.; Mironov, A.; Moran, S.; Müller-Bravo, T. E.; Newsome, M.; Nicholl, M.; Ochner, P.; Padilla Gonzalez, E.; Pessi, P. J.; Pignata, G.; Ragosta, F.; Reguitti, A.; Reynolds, T. M.; Riddle, R. L.; Rusholme, B.; Salmaso, I.; Schulze, S.; Sollerman, J.; Tomasella, L.; Warshofsky, D.; Yang, S.; Young, D. R.
Kustantaja: EDP Sciences
Julkaisuvuosi: 2026
Lehti: Astronomy and Astrophysics
Artikkelin numero: A221
Vuosikerta: 710
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202659438
Julkaisun avoimuus kirjaamishetkellä: Avoimesti saatavilla
Julkaisukanavan avoimuus : Kokonaan avoin julkaisukanava
Verkko-osoite: https://doi.org/10.1051/0004-6361/202659438
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/527095601
Rinnakkaistallenteen lisenssi: CC BY
Rinnakkaistallennetun julkaisun versio: Kustantajan versio
Aims. We present and interpret the data of the nearby hydrogen-deficient but helium-rich superluminous supernova SN 2021bnw, which reached a magnitude of –20.7 at maximum luminosity in g band.
Methods. We discuss the light curves and spectra of SN 2021bnw based on its spectro-photometric follow-up, exploiting different observational facilities. We reproduced the near-IR spectrum of SN 2021bnw with TARDIS to inspect the chemical composition at late photospheric phases and identify helium features. We also used a STELLA model coupling hydrodynamics and radiation transport to constrain the physical parameters of the explosion assuming a 56Ni+CSM scenario.
Results. We suggest that SN 2021bnw was mainly powered by the interaction of the ejecta with a previously lost He-rich circumstellar material, coupled with a central power source.
Conclusions. This work expands the data sample of He-rich superluminous supernovae (SLSNe Ib), and for a single-progenitor scenario, it can constrain the masses and physics of their progenitors.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
Julkaisussa olevat rahoitustiedot:
We thank Ósmar Rodríguez and the anonymous referee for their valuable comments that improved our work. A. F. acknowledges funding by the European Union – NextGenerationEU RFF M4C2 1.1 PRIN 2022 project “2022RJLWHN URKA” and by INAF 2023 Theory Grant ObFu 1.05.23.06.06 “Understanding R-process & Kilonovae Aspects (URKA)”. A. R. acknowledges financial support from the GRAWITA Large Program Grant (PI P. D’Avanzo) and from the PRIN-INAF 2022 “Shedding light on the nature of gap transients: from the observations to the models”. T.E.M.B. is funded by Horizon Europe ERC grant no. 101125877. This work makes use of observations from the Las Cumbres Observatory network. MN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 948381). Y.-Z. Cai is supported by the National Natural Science Foundation of China (No. 12303054), the Yunnan Fundamental Research Projects (Grant Nos. 202401AU070063, 202501AS070078), the National Key Research and Development Program of China (Grant No. 2024YFA1611603), and the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). Y.-Z. Cai and A. R. also acknowledge financial support from the SOXS project (PI S. Campana). C. P. G. acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Program of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 program, 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. N. E. R. acknowledges support from the PRIN-INAF 2022, “Shedding light on the nature of gap transients: from the observations to the models” and 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. T.-W. C. acknowledges the financial support from the Yushan Fellow Program by the Ministry of Education, Taiwan (MOE-111-YSFMS-0008-001-P1) and the National Science and Technology Council, Taiwan (NSTC grant 114-2112-M-008-021-MY3). P. B. is supported by the grant RSF 24-12-00141 for modeling supernova light curves with the STELLA code. This work makes use of observations from the Las Cumbres Observatory network (LCO). The LCO team is supported by NSF grants AST-1911225 and AST-1911151. This research made use of TARDIS, a community-developed software package for spectral synthesis in supernovae (Kerzendorf & Sim 2014). The development of TARDIS received support from GitHub, the Google Summer of Code initiative, and from ESA’s Summer of Code in Space program. TARDIS is a fiscally sponsored project of NumFOCUS. TARDIS makes extensive use of Astropy and Pyne. Based on observations collected at the European organization for astronomical research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects). Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey – PI: Inserra). ePESSTO+ observations were obtained under ESO program IDs 1103.D-0328, 106.216C and 108.220C. 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 NOT. Based on observations collected at Copernico and Schmidt telescopes (Asiago, Italy) of the INAF-Osservatorio Astronomico di Padova. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann Institute of Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University of Warwick, Ruhr University Bochum, Cornell University, and Northwestern University. Operations are conducted by COO, IPAC, and UW. SED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171. The Gordon and Betty Moore Foundation, through both the Data-Driven Investigator Program and a dedicated grant, provided critical funding for SkyPortal (van der Walt et al. 2019; Coughlin et al. 2023).
