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Abernathy, M. R.; Ackley, K.; Aggarwal, N.; Ain, A.; Ajith, P.; Appert, S.; Arnaud, N.; Bacon, P.; Barker, D.; Barsotti, L.; Bavigadda, V.; Bersanetti, D.; Birnholtz, O.; Biwer, C.; Bock, O.; Boer, M.; Boom, B. A.; Bozzi, A.; Brillet, A.; Camp, J. B.; Cannon, K. C.; Caride, S.; Chamberlin, S. J.; Chu, Q.; Chung, S.; Cohadon, P.-F.; Corbitt, T. R.; Couvares, P.; Covas, P. B.; Davier, M.; Díaz, M. C.; Edo, T. B.; Essick, R. C.; Etienne, Z.; Evans, T. M.; Fejer, M. M.; Fiori, I.; Frey, R.; Frey, V.; Goetz, R.; Gopakumar, A.; Gouaty, R.; Grado, A.; Hanke, M. M.; Harry, I. W.; Heintze, M. C.; Heptonstall, A. W.; Hofman, D.; Huerta, E. A.; Johnson, W. W.; Kajita, T.; Kawai, N.; Kimura, N.; Kirchhoff, R.; Koch, P.; Korth, W. Z.; Lasky, P. D.; Lazzarini, A.; Leavey, S.; Lee, K.; Lovelace, G.; Ma, Y.; Martin, I. W.; Mavalvala, N.; Meshkov, S.; Milano, L.; Nakao, K.; O’Reilly, B.; O’Shaughnessy, R.; Owen, B. J.; Palomba, C.; Pant, B. C.; Parker, W.; Pasqualetti, A.; Pele, A.; Perri, L. M.; Pinard, L.; Pürrer, M.; Quintero, E. A.; Rosińska, D.; Ryan, K.; Sadeghian, L.; Schale, P.; Sengupta, A. S.; Sigg, D.; Silva, A. D.; Smith, B.; Stevenson, S. P.; Suzuki, T.; Thorne, K. A.; Thrane, E.; Ushiba, T.; Vasúth, M.; Wallace, L.; Weaver, B.; Weinstein, A. J.; Wipf, C. C.; Zhang, L.; Zhang, T.; Zucker, M. E.
Deleted Journal, 2018/12, Volume: 21, Issue: 1Journal Article, Web Resource
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 deg 2 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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