Andrews, Jennifer E and Sand, D J and Valenti, S and Smith, Nathan and Dastidar, Raya and Sahu, D K and Misra, Kuntal and Singh, Avinash and Hiramatsu, D and Brown, P J and Hosseinzadeh, G and Wyatt, S and Vinko, J and Anupama, G C and Arcavi, I and Ashall, Chris and Benetti, S and Berton, Marco and Bostroem, K A and Bulla, M and Burke, J and Chen, S and Chomiuk, L and Cikota, A and Congiu, E and Cseh, B and Davis, Scott and Elias-Rosa, N and Faran, T and Fraser, Morgan and Galbany, L and Gall, C and Gal-Yam, A and Gangopadhyay, Anjasha and Gromadzki, M and Haislip, J and Howell, D A and Hsiao, E Y and Inserra, C and Kankare, E and Kuncarayakti, H and Kouprianov, V and Kumar, Brajesh and Li, Xue and Lin, Han and Maguire, K and Mazzali, P and McCully, C and Milne, P and Mo, Jun and Morrell, N and Nicholl, M and Ochner, P and Olivares, F and Pastorello, A and Patat, F and Phillips, M and Pignata, G and Prentice, S and Reguitti, A and Reichart, D E and Rodriguez, O and Rui, Liming and Sanwal, Pankaj and Sarneczky, K and Shahbandeh, M and Singh, Mridweeka and Smartt, S and Strader, J and Stritzinger, M D and Szakats, R and Tartaglia, L and Wang, Huijuan and Wang, Lingzhi and Wang, Xiaofeng and Wheeler, J C and Xiang, Danfeng and Yaron, O and Young, D R and Zhang, Junbo (2019) SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries. In: ASTROPHYSICAL JOURNAL, 885 (1).
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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 progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130;;0.026 M of Ni-56 are present, if the light curve is solely powered by radioactive decay, although the Ni-56 mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of H? 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.
| Item Type: | Journal Article |
|---|---|
| Publication: | ASTROPHYSICAL JOURNAL |
| Publisher: | IOP PUBLISHING LTD |
| Additional Information: | Copyright of this article belongs to IOP PUBLISHING LTD |
| Keywords: | Type II supernovae; Core-collapse supernovae; Massive stars |
| Department/Centre: | Division of Physical & Mathematical Sciences > Astronomy and Astrophysics Programme |
| Date Deposited: | 17 Feb 2020 10:05 |
| Last Modified: | 17 Feb 2020 10:05 |
| URI: | http://eprints.iisc.ac.in/id/eprint/64116 |
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