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A comparison between SALT/SAAO observations and kilonova models for AT 2017gfo: the first electromagnetic counterpart of a gravitational wave transient-GW170817
Buckley, David A. H.1,2; Andreoni, Igor3,4,5; Barway, Sudhanshu1; Cooke, Jeff3,4,6; Crawford, Steven M.1,2; Gorbovskoy, Evgeny7; Gromadzki, Mariusz8; Lipunov, Vladimir7,9; Mao JR(毛基荣)10,11,12; Potter, Stephen B.1; Pretorius, Magaretha L.1,13; Pritchard, Tyler A.3; Romero-Colmenero, Encarni1,2; Shara, Michael M.14,15; Vaisanen, Petri1,2; Williams, Ted B.1; Buckley, David A. H.(South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa)
发表期刊MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2018-02-01
卷号474期号:1页码:L71-L75
DOI10.1093/mnrasl/slx196
产权排序第10完成单位
收录类别SCI
关键词Gravitational Waves Binaries: Close Gamma-ray Burst: Individual: Grb 170817a Stars: Neutron Nuclear Reactions Stars: Winds Nucleosynthesis Outflows Abundances
摘要We report on SALT low-resolution optical spectroscopy and optical/IR photometry undertaken with other SAAO telescopes (MASTER-SAAO and IRSF) of the kilonova AT 2017gfo (a.k.a. SSS17a) in the galaxy NGC4993 during the first 10 d of discovery. This event has been identified as the first ever electromagnetic counterpart of a gravitational wave event, namely GW170817, which was detected by the LIGO and Virgo gravitational wave observatories. The event is likely due to a merger of two neutron stars, resulting in a kilonova explosion. SALT was the third observatory to obtain spectroscopy of AT 2017gfo and the first spectrum, 1.2 d after the merger, is quite blue and shows some broad features, but no identifiable spectral lines and becomes redder by the second night. We compare the spectral and photometric evolution with recent kilonova simulations and conclude that they are in qualitative agreement for post-merger wind models with proton: nucleon ratios of Y-e = 0.25-0.30. The blue colour of the first spectrum is consistent with the lower opacity of the lanthanide-free r-process elements in the ejecta. Differences between the models and observations are likely due to the choice of system parameters combined with the absence of atomic data for more elements in the ejecta models.
项目资助者Southern African Large Telescope (SALT) under the Director's Discretionary Time programme(2017-1-DDT-009) ; National Research Foundation (NRF) of South Africa ; PolishNCN grant(OPUS 2015/17/B/ST9/03167) ; Hundred Talent Program ; Chinese Academy of Sciences(KJZD-EW-M06) ; National Natural Science Foundation of China(11673062) ; Overseas Talent Program of Yunnan Province ; Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav)(CE170100004) ; Australian Research Council Future fellowship(FT130101219) ; MNiSW(DIR/WK/2016/07)
语种英语
学科领域天文学
文章类型Article
ISSN0035-8711
URL查看原文
WOS记录号WOS:000425491400015
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]NEUTRON-STAR MERGERS ; R-PROCESS ; NUCLEOSYNTHESIS ; BURSTS
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被引频次:10[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/12289
专题丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
通讯作者Buckley, David A. H.(South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa)
作者单位1.South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape Town, South Africa
2.Southern African Large Telescope Foundation, PO Box 9, Observatory 7935, Cape Town, South Africa
3.Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, H29, Hawthorn, VIC 3122, Australia
4.The Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Australia
5.Australian Astronomical Observatory, 105 Delhi Rd, North Ryde NSW 2113, Australia
6.The Australian Research Council Centre of Excellence for All-Sky Astrophysics (CAASTRO), Australia
7.M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr., 13, Moscow, 119234, Russia
8.Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, PL-00-478, Warszawa, Poland
9.M.V.Lomonosov Moscow State University, Physics Department, Leninskie gory, GSP-1, Moscow, 119991, Russia
10.Yunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, Yunnan Province, China
11.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, 100012 Beijing, China
12.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650011 Kunming, China
13.Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa
14.Department of Astrophysics, American Museum of Natural History, Central Park West and 79th Street, New York, NY 10024, USA
15.Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
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Buckley, David A. H.,Andreoni, Igor,Barway, Sudhanshu,et al. A comparison between SALT/SAAO observations and kilonova models for AT 2017gfo: the first electromagnetic counterpart of a gravitational wave transient-GW170817[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2018,474(1):L71-L75.
APA Buckley, David A. H..,Andreoni, Igor.,Barway, Sudhanshu.,Cooke, Jeff.,Crawford, Steven M..,...&Buckley, David A. H..(2018).A comparison between SALT/SAAO observations and kilonova models for AT 2017gfo: the first electromagnetic counterpart of a gravitational wave transient-GW170817.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,474(1),L71-L75.
MLA Buckley, David A. H.,et al."A comparison between SALT/SAAO observations and kilonova models for AT 2017gfo: the first electromagnetic counterpart of a gravitational wave transient-GW170817".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 474.1(2018):L71-L75.
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