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

Author: Abbott
and Abbott B. P.
and Abbott R.
and Abernathy T. D.
and Acernese M. R.
and Ackley F.
and Adams C.
and Adams K.
and Addesso T.
and Adhikari P.
and Adya R. X.
and Affeldt V. B.
and Agathos C.
and Agatsuma M.
and Aggarwal K.
and Aguiar N.
and Aiello O. D.
and Ain L.
and Ajith A.
and Akutsu P.
and Allen T.
and Allocca B.
and Altin A.
and Alvarez R.
and Ananyeva P. A.
and Anderson A.
and Anderson S. B.
and Ando W. G.
and Appert M.
and Arai S.
and Araya A.
and Araya K.
and Areeda M. C.
and Arnaud J. S.
and Arun N.
and Asada K. G.
and Ascenzi H.
and Ashton S.
and Aso G.
and Ast Y.
and Aston M.
and Astone S. M.
and Atsuta P.
and Aufmuth S.
and Aulbert P.
and Avila-Alvarez C.
and Awai A.
and Babak K.
and Bacon S.
and Bader P.
and Baiardi C. B.
and Baiotti M. K. M.
and Baker L.
and Baldaccini P. T.
and Ballardin F.
and Ballmer G.
and Barayoga S. W.
and Barclay J. C.
and Barish S. E.
and Barker B. C.
and Barone D.
and Barr F.
and Barsotti B.
and Barsuglia L.
and Barta M.
and Bartlett D.
and Barton J.
and Bartos M. A.
and Bassiri I.
and Basti R.
and Batch A.
and Baune J. C.
and Bavigadda C.
and Bazzan V.
and Becsy M.
and Beer B.
and Bejger C.
and Belahcene M.
and Belgin I.
and Bell M.
and Berger A. S.
and Bergmann B. K.
and Berry G.
and Bersanetti C. P. L.
and Bertolini D.
and Betzwieser A.
and Bhagwat J.
and Bhandare S.
and Bilenko R.
and Billingsley I. A.
and Billman G.
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and Birney J.
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and Bisht S.
and Bitossi A.
and Biwer M.
and Bizouard C.
and Blackburn M. A.
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and Vyatchanin W. D.
and Wade L.
and Wade S. P.
and Wakamatsu M.
and Walker T.
and Wallace M.
and Walsh L.
and Wang G.
and Wang H.
and Wang M.
and Wang S.
and Ward Y.
and Warner R. L.
and Was J.
and Watchi M.
and Weaver J.
and Wei B.
and Weinert L. -W.
and Weinstein M.
and Weiss A. J.
and Wen R.
and Wessels L.
and Westphal P.
and Wette T.
and Whelan K.
and Whiting J. T.
and Whittle B. F.
and Williams C.
and Williams D.
and Williamson R. D.
and Willis A. R.
and Willke J. L.
and Wimmer B.
and Winkler M. H.
and Wipf W.
and Wittel C. C.
and Woan H.
and Woehler G.
and Worden J.
and Wright J.
and Wu D. S.
and Wu J. L.
and Yam G.
and Yamamoto H.
and Yamamoto K.
and Yamamoto W.
and Yancey T.
and Yano C. C.
and Yap K.
and Yokoyama M. J.
and Yokozawa J.
and Yoon T.
and Yu Hang
and Yu T. H.
and Yuzurihara Haocun
and Yvert H.
and Zadrozny M.
and Zangrando A.
and Zanolin L.
and Zeidler M.
and Zendri S.
and Zevin J. -P.
and Zhang L.
and Zhang M.
and Zhang M.
and Zhang T.
and Zhao Y.
and Zhou C.
and Zhou M.
and Zhu S. J.
and Zhu Z.
and Zucker X. J.
and Zweizig M. E.
And D.
And M.
Calderon and Callister J.
Casanueva and Casentini J.
Cerboni and Cerretani L.
Da Silva and Dattilo C. F.
Dovale and Downes M.
Fernandez and Ferrante A.
Gonzalez and Gopakumar J. M.
Marchesoni F.
R. and E. A.
R. J
Travasso F.
Publication venue: 'Springer Science and Business Media LLC'
Publication date: 01/01/2018
Field of study

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– 20 deg2 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

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