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http://hdl.handle.net/20.500.12386/29333
Title: | SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries | Authors: | 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, Stefano Berton, Marco Bostroem, K. A. Bulla, M. Burke, J. Chen, S. Chomiuk, L. Cikota, A. Congiu, E. Cseh, B. Davis, Scott ELIAS DE LA ROSA, NANCY DEL CARMEN 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, Andrea Patat, F. Phillips, M. Pignata, G. Prentice, S. Reguitti, A. Reichart, D. E. Rodríguez, Ó. Rui, Liming Sanwal, Pankaj Sárneczky, K. Shahbandeh, M. Singh, Mridweeka Smartt, S. Strader, J. Stritzinger, M. D. Szakáts, R. TARTAGLIA, LEONARDO Wang, Huijuan Wang, Lingzhi Wang, Xiaofeng Wheeler, J. C. Xiang, Danfeng Yaron, O. Young, D. R. Zhang, Junbo |
Issue Date: | 2019 | Journal: | THE ASTROPHYSICAL JOURNAL | Number: | 885 | Issue: | 1 | First Page: | 43 | 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 <SUB>☉</SUB> progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M <SUB>☉</SUB> of <SUP>56</SUP>Ni are present, if the light curve is solely powered by radioactive decay, although the <SUP>56</SUP>Ni 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. | URI: | http://hdl.handle.net/20.500.12386/29333 | URL: | https://iopscience.iop.org/article/10.3847/1538-4357/ab43e3 | ISSN: | 0004-637X | DOI: | 10.3847/1538-4357/ab43e3 | Bibcode ADS: | 2019ApJ...885...43A | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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2019ApJ_885_43A_postprint.pdf | preprint | 1.64 MB | Adobe PDF | View/Open |
Andrews_2019_ApJ_885_43.pdf | pdf editoriale | 2.67 MB | Adobe PDF | View/Open |
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