Detailed spectrophotometric analysis of the superluminous and fast evolving SN 2019neq
: Fiore Achille, Benetti Stefano, Tartaglia Leonardo, Jerkstrand Anders, Salmaso Irene, Tomasella Lina, Morales-Garoffolo Antonia, Geier Stefan, Elias-Rosa Nancy, Cappellaro Enrico, Wang Xiaofeng, Mo Jun, Chen Zhihao, Yan Shengyu, Pastorello Andrea, Mazzali Paolo A, Ciolfi Riccardo, Cai Yongzhi, Fraser Morgan, Gutiérrez Claudia P, Karamehmetoglu Emir, Kuncarayakti Hanindyo, Moran Shane, Ochner Paolo, Reguitti Andrea, Reynolds Thomas M, Valerin Giorgio
Publisher: Oxford University Press
: 2024
: Monthly Notices of the Royal Astronomical Society
: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
: MON NOT R ASTRON SOC
: 527
: 3
: 6473
: 6494
: 22
: 0035-8711
: 1365-2966
DOI: https://doi.org/10.1093/mnras/stad3655
: https://academic.oup.com/mnras/article/527/3/6473/7452888
: https://research.utu.fi/converis/portal/detail/Publication/387084423
SN 2019neq was a very fast evolving superluminous supernova. At a redshift z = 0.1059, its peak absolute magnitude was -21.5 +/- 0.2 mag in g band. In this work, we present data and analysis from an extensive spectrophotometric follow-up campaign using multiple observational facilities. Thanks to a nebular spectrum of SN 2019neq, we investigated some of the properties of the host galaxy at the location of SN 2019neq and found that its metallicity and specific star formation rate are in a good agreement with those usually measured for SLSNe-I hosts. We then discuss the plausibility of the magnetar and the circumstellar interaction scenarios to explain the observed light curves, and interpret a nebular spectrum of SN 2019neq using published SUMO radiative-transfer models. The results of our analysis suggest that the spin-down radiation of a millisecond magnetar with a magnetic field B similar or equal to 6 x 10(14) G could boost the luminosity of SN 2019neq.
