CaltechAUTHORS
  A Caltech Library Service

A Radio Counterpart to a Neutron Star Merger

Hallinan, G. and Corsi, A. and Mooley, K. P. and Hotokezaka, K. and Nakar, E. and Kasliwal, M. M. and Kaplan, D. L. and Frail, D. A. and Myers, S. T. and Murphy, T. and De, K. and Dobie, D. and Allison, J. R. and Bannister, K. W. and Bhalerao, V. and Chandra, P. and Clarke, T. E. and Giacintucci, S. and Ho, A. Y. Q. and Horesh, A. and Kassim, N. E. and Kulkarni, S. R. and Lenc, E. and Lockman, F. J. and Lynch, C. and Nichols, D. and Nissanke, S. and Palliyaguru, N. and Peters, W. M. and Piran, T. and Rana, J. and Sandler, E. M. and Singer, L. P. (2017) A Radio Counterpart to a Neutron Star Merger. Science, 358 (6370). pp. 1579-1583. ISSN 0036-8075. https://resolver.caltech.edu/CaltechAUTHORS:20171002-111130949

[img] PDF - Submitted Version
See Usage Policy.

1006Kb
[img] PDF (Materials and Methods; Supplementary Text; Figs. S1 to S5; Table S1; References) - Supplemental Material
See Usage Policy.

1463Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20171002-111130949

Abstract

Gravitational waves have been detected from a binary neutron star merger event, GW170817. The detection of electromagnetic radiation from the same source has shown that the merger occurred in the outskirts of the galaxy NGC 4993, at a distance of 40 megaparsecs from Earth. We report the detection of a counterpart radio source that appears 16 days after the event, allowing us to diagnose the energetics and environment of the merger. The observed radio emission can be explained by either a collimated ultrarelativistic jet, viewed off-axis, or a cocoon of mildly relativistic ejecta. Within 100 days of the merger, the radio light curves will enable observers to distinguish between these models, and the angular velocity and geometry of the debris will be directly measurable by very long baseline interferometry.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1126/science.aap9855DOIArticle
http://science.sciencemag.org/content/358/6370/1579PublisherArticle
http://www.sciencemag.org/cgi/content/full/science.aap9855/DC1PublisherSupplemental Materials
https://arxiv.org/abs/1710.05435arXivDiscussion Paper
ORCID:
AuthorORCID
Hallinan, G.0000-0002-7083-4049
Corsi, A.0000-0001-8104-3536
Mooley, K. P.0000-0002-2557-5180
Hotokezaka, K.0000-0002-2502-3730
Nakar, E.0000-0002-4534-7089
Kasliwal, M. M.0000-0002-5619-4938
Kaplan, D. L.0000-0001-6295-2881
Murphy, T.0000-0002-2686-438X
De, K.0000-0002-8989-0542
Dobie, D.0000-0003-0699-7019
Bhalerao, V.0000-0002-6112-7609
Ho, A. Y. Q.0000-0002-9017-3567
Horesh, A.0000-0002-5936-1156
Kulkarni, S. R.0000-0001-5390-8563
Lenc, E.0000-0002-9994-1593
Palliyaguru, N.0000-0002-4828-0262
Piran, T.0000-0002-7964-5420
Singer, L. P.0000-0001-9898-5597
Additional Information:© 2017 American Association for the Advancement of Science. Received 17 September 2017; accepted 9 October 2017; published online 16 October 2017. G.H., A.C., and K.P.M. acknowledge the support and dedication of the staff of the National Radio Astronomy Observatory and particularly thank the VLA director, M. McKinnon, as well as A. Mioduszewski and the VLA schedulers, for making the VLA campaign possible. We thank the staff of the GMRT that made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. We thank the Green Bank Observatory for their rapid response to our Director’s Discretionary Time GBT proposal. The National Radio Astronomy Observatory and the Green Bank Observatory are facilities of the National Science Foundation operated under a cooperative agreement by Associated Universities Inc. Supported by NSF award AST-1654815 (G.H.); NSF CAREER award 1455090 “Radio and gravitational-wave emission from the largest explosions since the Big Bang” (A.C. and N.P.); the Oxford Centre for Astrophysical Surveys, funded through the Hintze Family Charitable Foundation (K.P.M.); ERC starting grant GRB/SN and ISF grant 1277/13 (E.N.); the Government of India Department of Science and Technology via SwarnaJayanti Fellowship awards DST/SJF/PSA-01/2014-15 (P.C.); the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation (A.H.); Australian Research Council grant FT150100099 (T.M.); the GROWTH (Global Relay of Observatories Watching Transients Happen) project, funded by NSF under PIRE grant 1545949; NSF grant AST-1412421 (D.L.K.); Advanced ERC grant TReX (T.P.); the Science and Engineering Research Board, Department of Science and Technology, India, for the GROWTH-India project (V.B.); and NSF Graduate Research Fellowship DGE-1144469 (A.Y.Q.H.). GROWTH is a collaborative project of the California Institute of Technology, University of Maryland–College Park, University of Wisconsin–Milwaukee, Texas Tech University, San Diego State University, Los Alamos National Laboratory, Tokyo Institute of Technology, National Central University (Taiwan), Indian Institute of Astrophysics (India), Inter-University Center for Astronomy and Astrophysics (India), Weizmann Institute of Science (Israel), Oskar Klein Centre at Stockholm University (Sweden), Humboldt University (Germany), and Liverpool John Moores University (UK). This work is part of the research program Innovational Research Incentives Scheme (Vernieuwingsimpuls), financed by the Netherlands Organization for Scientific Research through NWO VIDI grant 639.042.612-Nissanke and NWO TOP grant 62002444-Nissanke. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics in 3D (ASTRO 3D), project CE170100013, and by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), project CE110001020. Basic research in radio astronomy at the Naval Research Laboratory (NRL) is funded by 6.1 Base funding. Construction and installation of VLITE was supported by NRL Sustainment Restoration and Maintenance funding. The VLA data reported in this paper are available from G.H. upon request.
Funders:
Funding AgencyGrant Number
Australian GovernmentUNSPECIFIED
NSFAST-1654815
NSFAST-1455090
Hintze Family Charitable FoundationUNSPECIFIED
European Research Council (ERC)TReX
Israel Science Foundation1277/13
Department of Science and Technology (India)DST/SJF/PSA-01/2014-15
I-CORE Program of the Planning and Budgeting CommitteeUNSPECIFIED
Israel Science FoundationUNSPECIFIED
Australian Research CouncilFT150100099
NSFAST-1545949
NSFAST-1412421
Science and Engineering Research Board (SERB)UNSPECIFIED
NSF Graduate Research FellowshipDGE-1144469
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)639.042.612-Nissanke
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)62002444-Nissanke
Australian Research CouncilCE170100013
Australian Research CouncilCE110001020
Naval Research Laboratory6.1 Base funding
Issue or Number:6370
Record Number:CaltechAUTHORS:20171002-111130949
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20171002-111130949
Official Citation:A radio counterpart to a neutron star merger. BY G. HALLINAN, A. CORSI, K. P. MOOLEY, K. HOTOKEZAKA, E. NAKAR, M. M. KASLIWAL, D. L. KAPLAN, D. A. FRAIL, S. T. MYERS, T. MURPHY, K. DE, D. DOBIE, J. R. ALLISON, K. W. BANNISTER, V. BHALERAO, P. CHANDRA, T. E. CLARKE, S. GIACINTUCCI, A. Y. Q. HO, A. HORESH, N. E. KASSIM, S. R. KULKARNI, E. LENC, F. J. LOCKMAN, C. LYNCH, D. NICHOLS, S. NISSANKE, N. PALLIYAGURU, W. M. PETERS, T. PIRAN, J. RANA, E. M. SADLER, L. P. SINGER. SCIENCE 22 DEC 2017 : 1579-1583
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:81949
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:02 Oct 2017 18:13
Last Modified:19 Nov 2019 04:36

Repository Staff Only: item control page