Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

KAGRA Collaboration, LIGO Scientific Collaboration and Virgo Collaboration

doi:10.1007/s41114-018-0012-9

Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

KAGRA Collaboration, LIGO Scientific Collaboration and Virgo Collaboration

(Astro)-Particles Physics

Research output: Contribution to Journal › Review article › Academic › peer-review

Abstract

We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90 % credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5–20deg2 requires at least three detectors of sensitivity within a factor of ∼ 2 of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.

Original language	English
Article number	3
Pages (from-to)	1-57
Number of pages	57
Journal	LIVING REVIEWS IN RELATIVITY
Volume	21
Early online date	26 Apr 2018
DOIs	https://doi.org/10.1007/s41114-018-0012-9
Publication status	Published - Dec 2018

Funding

Acknowledgements The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidència i Conselleria d’Innovació, Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Educació, Investigació, Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFI), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources. The authors gratefully acknowledge the support in Japan by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, MEXT Grant-in-Aid for Scientific Research on Innovative Areas 24103005, JSPS Core-to-Core Program, A. Advanced Research Networks, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, and Computing Infrastructure Project of KISTI-GSDC in Korea. This article has been assigned LIGO Document number P1200087, Virgo Document number VIR-0288A-12, and KAGRA Document number JGW-P1706792.

Funders	Funder number
Not added	ST/N005422/1, ST/M000095/1, ST/P002218/1, ST/P006892/1, ST/N005406/2, ST/K000845/1, ST/H002006/1, ST/M005844/1, ST/I006269/1, ST/M003035/1, ST/N000633/1, ST/N000072/1, ST/N005481/1, ST/J00166X/1, ST/L000911/1
KISTI-GSDC
National Science Foundation	1707965, 1708081, 1455090, 1506254, 1242090
Directorate for Mathematical and Physical Sciences
Kavli Foundation
National Kidney Foundation of Iowa
Canadian Institute for Advanced Research
Natural Sciences and Engineering Research Council of Canada
Ontario Ministry of Economic Development and Innovation
Science and Technology Facilities Council	PPA/G/S/2002/00652, Gravitational Waves, ST/N005430/1
Leverhulme Trust
Royal Society
Scottish Funding Council
Scottish Universities Physics Alliance
European Commission
Australian Research Council
Department of Science and Technology, Ministry of Science and Technology, India
Council of Scientific and Industrial Research, India
Japan Society for the Promotion of Science	15K05070, 17K05431, 16H03986, 16H06341, 17H06133, 17K05437, 15H02082, 16K05347, 17J08115, 16H03972, 18K18729
Ministry of Education, Culture, Sports, Science and Technology
Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung
National Natural Science Foundation of China
Science and Engineering Research Board
Russian Foundation for Basic Research
Research Grants Council, University Grants Committee
Nederlandse Organisatie voor Wetenschappelijk Onderzoek
Generalitat Valenciana
Hungarian Scientific Research Fund
National Research Foundation of Korea
Instituto Nazionale di Fisica Nucleare
Narodowe Centrum Nauki
Ministry of Human Resource Development
Ministry of Science and Technology, Taiwan
Centre National de la Recherche Scientifique
Russian Science Foundation
European Regional Development Fund
Universitat de les Illes Balears
Nemzeti Kutatási Fejlesztési és Innovációs Hivatal
Agencia Estatal de Investigación
Ministério da Ciência, Tecnologia, Inovações e Comunicações
Istituto Nazionale di Fisica Nucleare
ICTP South American Institute for Fundamental Research

Keywords

Data analysis
Electromagnetic counterparts
Gravitational waves
Gravitational-wave detectors

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@article{099df910b4994e858f14420e7d5d0193,

title = "Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA",

abstract = "We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90 % credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5–20deg2 requires at least three detectors of sensitivity within a factor of ∼ 2 of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.",

keywords = "Data analysis, Electromagnetic counterparts, Gravitational waves, Gravitational-wave detectors",

author = "Abbott, {B. P.} and R. Abbott and Abbott, {T. D.} and Abernathy, {M. R.} and F. Acernese and K. Ackley and C. Adams and T. Adams and P. Addesso and Adhikari, {R. X.} and Adya, {V. B.} and C. Affeldt and M. Agathos and K. Agatsuma and N. Aggarwal and Aguiar, {O. D.} and L. Aiello and A. Ain and P. Ajith and T. Akutsu and B. Allen and A. Allocca and Altin, {P. A.} and A. Ananyeva and Anderson, {S. B.} and Anderson, {W. G.} and M. Ando and S. Appert and K. Arai and A. Araya and Araya, {M. C.} and Areeda, {J. S.} and N. Arnaud and Arun, {K. G.} and H. Asada and S. Ascenzi and G. Ashton and Y. Aso and M. Ast and Bader, {M. K.M.} and Bulten, {H. J.} and {Del Pozzo}, W. and Jonker, {R. J.G.} and Leong, {J. R.} and Li, {T. G.F.} and J. Meidam and Rabeling, {D. S.} and {van Bakel}, N. and {van den Brand}, {J. F.J.} and J. Veitch and {KAGRA Collaboration, LIGO Scientific Collaboration and Virgo Collaboration}",

year = "2018",

month = dec,

doi = "10.1007/s41114-018-0012-9",

language = "English",

volume = "21",

pages = "1--57",

journal = "LIVING REVIEWS IN RELATIVITY",

issn = "1433-8351",

publisher = "Springer Verlag",

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TY - JOUR

T1 - Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

AU - Abbott, B. P.

AU - Abbott, R.

AU - Abbott, T. D.

AU - Abernathy, M. R.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, C.

AU - Adams, T.

AU - Addesso, P.

AU - Adhikari, R. X.

AU - Adya, V. B.

AU - Affeldt, C.

AU - Agathos, M.

AU - Agatsuma, K.

AU - Aggarwal, N.

AU - Aguiar, O. D.

AU - Aiello, L.

AU - Ain, A.

AU - Ajith, P.

AU - Akutsu, T.

AU - Allen, B.

AU - Allocca, A.

AU - Altin, P. A.

AU - Ananyeva, A.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Ando, M.

AU - Appert, S.

AU - Arai, K.

AU - Araya, A.

AU - Araya, M. C.

AU - Areeda, J. S.

AU - Arnaud, N.

AU - Arun, K. G.

AU - Asada, H.

AU - Ascenzi, S.

AU - Ashton, G.

AU - Aso, Y.

AU - Ast, M.

AU - Bader, M. K.M.

AU - Bulten, H. J.

AU - Del Pozzo, W.

AU - Jonker, R. J.G.

AU - Leong, J. R.

AU - Li, T. G.F.

AU - Meidam, J.

AU - Rabeling, D. S.

AU - van Bakel, N.

AU - van den Brand, J. F.J.

AU - Veitch, J.

AU - KAGRA Collaboration, LIGO Scientific Collaboration and Virgo Collaboration

PY - 2018/12

Y1 - 2018/12

N2 - We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90 % credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5–20deg2 requires at least three detectors of sensitivity within a factor of ∼ 2 of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.

AB - We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90 % credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5–20deg2 requires at least three detectors of sensitivity within a factor of ∼ 2 of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.

KW - Data analysis

KW - Electromagnetic counterparts

KW - Gravitational waves

KW - Gravitational-wave detectors

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U2 - 10.1007/s41114-018-0012-9

DO - 10.1007/s41114-018-0012-9

M3 - Review article

AN - SCOPUS:85046034556

SN - 1433-8351

VL - 21

SP - 1

EP - 57

JO - LIVING REVIEWS IN RELATIVITY

JF - LIVING REVIEWS IN RELATIVITY

M1 - 3

ER -

Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

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