학술논문
SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries
Document Type
article
Author
Andrews, Jennifer E; Sand, DJ; Valenti, S; Smith, Nathan; Dastidar, Raya; Sahu, DK; Misra, Kuntal; Singh, Avinash; Hiramatsu, D; Brown, PJ; Hosseinzadeh, G; Wyatt, S; Vinko, J; Anupama, GC; Arcavi, I; Ashall, Chris; Benetti, S; Berton, Marco; Bostroem, KA; Bulla, M; Burke, J; Chen, S; Chomiuk, L; Cikota, A; Congiu, E; Cseh, B; Davis, Scott; Elias-Rosa, N; Faran, T; Fraser, Morgan; Galbany, L; Gall, C; Gal-Yam, A; Gangopadhyay, Anjasha; Gromadzki, M; Haislip, J; Howell, DA; Hsiao, EY; Inserra, C; Kankare, E; Kuncarayakti, H; Kouprianov, V; Kumar, Brajesh; Li, Xue; Lin, Han; Maguire, K; Mazzali, P; McCully, C; Milne, P; Mo, Jun; Morrell, N; Nicholl, M; Ochner, P; Olivares, F; Pastorello, A; Patat, F; Phillips, M; Pignata, G; Prentice, S; Reguitti, A; Reichart, DE; Rodríguez, Ó; Rui, Liming; Sanwal, Pankaj; Sárneczky, K; Shahbandeh, M; Singh, Mridweeka; Smartt, S; Strader, J; Stritzinger, MD; Szakáts, R; Tartaglia, L; Wang, Huijuan; Wang, Lingzhi; Wang, Xiaofeng; Wheeler, JC; Xiang, Danfeng; Yaron, O; Young, DR; Zhang, Junbo
Source
The Astrophysical Journal. 885(1)
Subject
Language
Abstract
We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R o progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M o of 56Ni are present, if the light curve is solely powered by radioactive decay, although the 56Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.