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The Rapid Reddening and Featureless Optical Spectra of the Optical Counterpart of GW170817, AT 2017gfo, during the First Four Days
McCully, Curtis1,2; Hiramatsu, Daichi1,2; Howell, D. Andrew1,2; Hosseinzadeh, Griffin1,2; Arcavi ,Iair1,2; Kasen, Daniel3,4,5; Barnes, Jennifer6; Shara, Michael M.7,8; Williams, Ted B.9; Väisänen, Petri9,10; Potter, Stephen B.9; Romero-Colmenero, Encarni9,10; Crawford, Steven M.9,10; Buckley, David A. H.9,10; Cooke, Jeffery11,12,13; Andreoni, Igor11,13,14; Pritchard, Tyler A.11; Mao JR(毛基荣)15,16,17; Gromadzki, Mariusz18; Burke, Jamison1,2
Source PublicationThe Astrophysical Journal Letters
2017-10-16
Volume848Issue:2
DOI10.3847/2041-8213/aa9111
Contribution Rank第15完成单位
Indexed BySCI
KeywordBinaries: Close Gamma-ray Burst: Individual (Grb 170817a, Grb 130603b) Gravitational Waves Stars: Neutron Stars: Winds, Outflows
Abstract

Abstract We present the spectroscopic evolution of AT 2017gfo, the optical counterpart of the first binary neutron star (BNS) merger detected by LIGO and Virgo, GW170817. While models have long predicted that a BNS merger could produce a kilonova (KN), we have not been able to definitively test these models until now. From one day to four days after the merger, we took five spectra of AT 2017gfo before it faded away, which was possible because it was at a distance of only 39.5 Mpc in the galaxy NGC 4993. The spectra evolve from blue (~6400 K) to red (~3500 K) over the three days we observed. The spectra are relatively featureless—some weak features exist in our latest spectrum, but they are likely due to the host galaxy. However, a simple blackbody is not sufficient to explain our data: another source of luminosity or opacity is necessary. Predictions from simulations of KNe qualitatively match the observed spectroscopic evolution after two days past the merger, but underpredict the blue flux in our earliest spectrum. From our best-fit models, we infer that AT 2017gfo had an ejecta mass of 0.03 M ⊙ , high ejecta velocities of 0.3c, and a low mass fraction ~10?4 of high-opacity lanthanides and actinides. One possible explanation for the early excess of blue flux is that the outer ejecta is lanthanide-poor, while the inner ejecta has a higher abundance of high-opacity material. With the discovery and follow-up of this unique transient, combining gravitational-wave and electromagnetic astronomy, we have arrived in the multi-messenger era.

Funding ProjectNSF[AST-1313484] ; National Aeronautics and Space Administration[PF6-170148] ; National Aeronautics and Space Administration[PF7-180162] ; National Aeronautics Space Administration[NAS8-03060] ; Department of Energy (DOE) Early Career award[DE-SC0008067] ; DOE Office of Nuclear Physics[DE-SC0017616] ; DOE SciDAC award[DE-SC0018297] ; Office of Energy Research, Office of High Energy and Nuclear Physics, Divisions of Nuclear Physics, of the U.S. Department of Energy[DE-AC02-05CH11231] ; Newmans Own Foundation ; South African National Research Foundation ; Australian Research Council (ARC) Centre of Excellence for Gravitational Wave Discovery (OzGrav)[CE170100004] ; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO)[CE110001020] ; ARC Future Fellowship grant[FT130101219] ; Australian Astronomical Observatory (AAO) ; Hundred Talent Program ; Major Program of the Chinese Academy of Sciences[KJZD-EW-M06] ; National Natural Science Foundation of China[11673062] ; Oversea Talent Program of Yunnan Province ; Polish NCN grant OPUS[2015/17/B/ST9/03167] ; Office of Science of the U.S. Department of Energy[DE-AC02-05CH11231]
Funding OrganizationNSF[AST-1313484] ; National Aeronautics and Space Administration[PF6-170148, PF7-180162] ; National Aeronautics Space Administration[NAS8-03060] ; Department of Energy (DOE) Early Career award[DE-SC0008067] ; DOE Office of Nuclear Physics[DE-SC0017616] ; DOE SciDAC award[DE-SC0018297] ; Office of Energy Research, Office of High Energy and Nuclear Physics, Divisions of Nuclear Physics, of the U.S. Department of Energy[DE-AC02-05CH11231] ; Newmans Own Foundation ; South African National Research Foundation ; Australian Research Council (ARC) Centre of Excellence for Gravitational Wave Discovery (OzGrav)[CE170100004] ; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO)[CE110001020] ; ARC Future Fellowship grant[FT130101219] ; Australian Astronomical Observatory (AAO) ; Hundred Talent Program ; Major Program of the Chinese Academy of Sciences[KJZD-EW-M06] ; National Natural Science Foundation of China[11673062] ; Oversea Talent Program of Yunnan Province ; Polish NCN grant OPUS[2015/17/B/ST9/03167] ; Office of Science of the U.S. Department of Energy[DE-AC02-05CH11231]
Language英语
Subject Area天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeAritcle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN2041-8205
URL查看原文
WOS IDWOS:000413099200020
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordCompact Object Mergers ; Neutron-star Mergers ; Kilonova Light Curves ; Mass Ejection ; Macronova
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/11949
Collection丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
Corresponding AuthorMcCully, Curtis
Affiliation1.Las Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA
2.Department of Physics, University of California, Santa Barbara, CA 93106-9530, USA
3.Department of Physics, University of California, Berkeley, CA 94720, USA
4.Department of Astronomy and Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA
5.Nuclear Science Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA
6.Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
7.Department of Astrophysics, American Museum of Natural History, Central Park West and 79th Street, New York, NY 10024, USA
8.Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
9.South African Astronomical Observatory, P.O. Box 9, Observatory 7935, Cape Town, South Africa
10.Southern African Large Telescope Foundation, P.O. Box 9, Observatory 7935, Cape Town, South Africa
11.Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, H29, Hawthorn, VIC 3122, Australia
12.The Australian Research Council Centre of Excellence for All-Sky Astrophysics (CAASTRO), Australia
13.The Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Australia
14.Australian Astronomical Observatory, 105 Delhi Road, North Ryde, NSW 2113, Australia
15.Yunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, Yunnan Province, China
16.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, 100012 Beijing, China
17.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011 Kunming, China
18.Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, PL-00-478, Warszawa, Poland
Recommended Citation
GB/T 7714
McCully, Curtis,Hiramatsu, Daichi,Howell, D. Andrew,et al. The Rapid Reddening and Featureless Optical Spectra of the Optical Counterpart of GW170817, AT 2017gfo, during the First Four Days[J]. The Astrophysical Journal Letters,2017,848(2).
APA McCully, Curtis.,Hiramatsu, Daichi.,Howell, D. Andrew.,Hosseinzadeh, Griffin.,Arcavi ,Iair.,...&Burke, Jamison.(2017).The Rapid Reddening and Featureless Optical Spectra of the Optical Counterpart of GW170817, AT 2017gfo, during the First Four Days.The Astrophysical Journal Letters,848(2).
MLA McCully, Curtis,et al."The Rapid Reddening and Featureless Optical Spectra of the Optical Counterpart of GW170817, AT 2017gfo, during the First Four Days".The Astrophysical Journal Letters 848.2(2017).
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