Browsing by Author "Wang, Lingzhi"

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SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries
(2019-11-01) Andrews, Jennifer E.; Sand, D. J.; Valenti, S.; Smith, Nathan; Dastidar, Raya; Sahu, D. K.; Misra, Kuntal; Singh, Avinash; Hiramatsu, D.; Brown, P. J.; Hosseinzadeh, G.; Wyatt, S.; Vinko, J.; Anupama, G. C.; Arcavi, I.; Ashall, Chris; Benetti, S.; Berton, Marco; Bostroem, K. A.; 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, D. A.; Hsiao, E. Y.; 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, D. E.; Rodríguez; Rui, Liming; Sanwal, Pankaj; Sárneczky, K.; Shahbandeh, M.; Singh, Mridweeka; Smartt, S.; Strader, J.; Stritzinger, M. D.; Szakáts, R.; Tartaglia, L.; Wang, Huijuan; Wang, Lingzhi; Wang, Xiaofeng; Wheeler, J. C.; Xiang, Danfeng; Yaron, O.; Young, D. R.; Zhang, Junbo
A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä
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.