A1 Refereed original research article in a scientific journal
SN 2020pvb: A Type IIn-P supernova with a precursor outburst
Authors: Elias-Rosa, N.; Brennan, S.J.; Benetti, S.; Cappellaro, E.; Pastorello, A.; Kozyreva, A.; Lundqvist, P.; Fraser, M.; Anderson, J.P.; Cai, Y.Z.; Chen, T.W.; Dennefeld, M.; Gromadzki, M.; Gutiérrez, C.P.; Ihanec, N.; Inserra, C.; Kankare, E.; Kotak, R.; Mattila, S.; Moran, S.; Müller-Bravo, T.E.; Pessi, P.J.; Pignata, G.; Reguitti, A.; Reynolds, T.M.; Smartt, S.J.; Smith, K.; Tartaglia, L.; Valerin, G.; De Boer, T.; Chambers, K.; Gal-Yam, A.; Gao, H.; Geier, S.; Mazzali, P.A.; Nicholl, M.; Ragosta, F.; Rest, A.; Yaron, O.; Young, D.R.
Publisher: EDP Sciences
Publication year: 2024
Journal: Astronomy and Astrophysics
Journal name in source: Astronomy and Astrophysics
Article number: A13
Volume: 686
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/202348790
Web address : https://doi.org/10.1051/0004-6361/202348790
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/457243344
We present photometric and spectroscopic datasets for SN 2020pvb, a Type IIn-P supernova (SN) that is similar to SNe 1994W, 2005cl, 2009kn, and 2011ht, with a precursor outburst detected (PS1 w band ∼- 13.8 mag) around four months before the B-band maximum light. SN 2020pvb presents a relatively bright light curve that peaked at MB = -17.95 ± 0.30 mag and a plateau that lasted at least 40 days before going into solar conjunction. After this, the object was no longer visible at phases > 150 days above - 12.5 mag in the B band, suggesting that the SN 2020pvb ejecta interact with a dense, spatially confined circumstellar envelope. SN 2020pvb shows strong Balmer lines and a forest of Fe II lines with narrow P Cygni profiles in its spectra. Using archival images from the Hubble Space Telescope, we constrained the progenitor of SN 2020pvb to have a luminosity of log(L/L⊙)≤5.4, ruling out any single star progenitor over 50 M⊙. SN 2020pvb is a Type IIn-P whose progenitor star had an outburst*sim;0.5 yr before the final explosion; the material lost during this outburst probably plays a role in shaping the physical properties of the SN.
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N.E.R. thanks T. Matsumoto for useful discussions. We thank the staff at the different observatories for performing the observations. N.E.R., S.B., E.C., A.P., A.R., G.V. acknowledge support from the PRIN-INAF 2022, “Shedding light on the nature of gap transients: from the observations to the models”. S.J.B. would like to thank their support from Science Foundation Ireland and the Royal Society (RS-EA/3471). M.F. is supported by a Royal Society – Science Foundation Ireland University Research Fellowship. M.G. is supported by the EU Horizon 2020 research and innovation programme under grant agreement No. 101004719. N.I. was partially supported by Polish NCN DAINA grant No. 2017/27/L/ST9/03221. S.M. was funded by the Research Council of Finland project 350458. S.M. acknowledges support from the Magnus Ehrnrooth Foundation and the Vilho, Yrjö, and Kalle Väisälä Foundation. T.E.M.B. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the I-LINK 2021 LINKA20409, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. M.N. is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 948381) and by a Fellowship from the Alan Turing Institute. Support for G.P. is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS). T.M.R. acknowledges the financial support of the Vilho, Yrjö and Kalle Väisälä Foundation of the Finnish academy of Science and Letters. S.J.S. is funded through STFC grant ST/T000198/1 L.T. acknowledges support from MIUR (PRIN 2017 grant 20179ZF5KS). Y.-Z. Cai is supported by the National Natural Science Foundation of China (NSFC, Grant No. 12303054) and the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). C.P.G. 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 PID2020-115253GA-I00 HOSTFLOWS project, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. This work made use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as last described in Eldridge et al. (2017), Stanway & Eldridge (2018). This work was funded by ANID, Millennium Science Initiative, ICN12_009. This work makes use of observations from the Las Cumbres Observatory global telescope network. This work is 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; ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT; 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; the Liverpool Telescope 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 Can
