Exploring the sensitivity of next generation gravitational wave
					detectors

Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Ackley, K.; Adams, C.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Aggarwal, N.; Aguiar, O. D.; Ain, A.; Ajith, P.; Allen, B.; Altin, P. A.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Araya, M. C.; Arceneaux, C. C.; Areeda, J. S.; Arun, K. G.; Ashton, G.; Ast, M.; Aston, S. M.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P. T.; Ballmer, S. W.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker, D.; Barr, B.; Barsotti, L.; Bartlett, J.; Bartos, I.; Bassiri, R.; Batch, J. C.; Baune, C.; Bell, A. S.; Berger, B. K.; Bergmann, G.; Berry, C. P. L.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Birney, R.; Biscans, S.; Bisht, A.; Biwer, C.; Blackburn, J. K.; Blair, C. D.; Blair, D. G.; Blair, R. M.; Böck, O.; Bogan, C.; Bohé, A.; Bond, C.; Bork, R.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J.; Brinkmann, M.; Brockill, P.; Broida, J. E.; Brooks, A. F.; Brown, Duncan; Brown, D. D.; Brown, N. M.; Brunett, S.; Buchanan, C. C.; Buikema, A.; Buonanno, A.; Byer, Robert L.; Cabero, M.; Cadonati, L.; Cahillane, C.; Bustillo, J. Calderón; Callister, T. A.; Camp, J. B.; Cannon, K. C.; Cao, Junwei; Capano, C. D.; Caride, S.; Caudill, S.; Cavaglià, M.; Cepeda, C.; Chamberlin, S. J.; Chan, M.; Chao, S.; Charlton, P.; Cheeseboro, B. D.; Chen, H. Y.; Chen, Y.; Cheng, C.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.; Chu, Q.; Chung, S.; Ciani, G.; Clara, F.; Clark, J. A.; Collette, Christophe; Cominsky, L.; Constancio, M.; Cook, D.; Corbitt, T. R.; Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M. W.; Coughlin, S. B.; Countryman, S. T.; Couvares, P.; Cowan, E. E.; Coward, D. M.; Cowart, M. J.; Coyne, D. C.; Coyne, R.; Craig, K.; Creighton, J. D. E.; Cripe, J.; Crowder, S. G.; Cumming, A.; Cunningham, L.; Canton, T. Dal; Danilishin, S. L.; Danzmann, K.; Darman, N. S.; Dasgupta, Anirban; Costa, C. F. Da Silva; Dave, I.; Davies, G. S.; Daw, E. J.; De, S.; DeBra, D.; Pozzo, W. Del; Denker, T.; Dent, T.; Dergachev, V.; DeRosa, R. T.; DeSalvo, R.; Devine, R. C.; Dhurandhar, S.; Díaz, M. C.; Palma, I. Di; Donovan, F.; Dooley, K. L.; Doravari, S.; Douglas, R.; Downes, T. P.; Drago, M.; Drever, R. W. P.; Driggers, J. C.; Dwyer, S. E.; Edo, T. B.; Edwards, M. C.; Effler, A.; Eggenstein, H.-B.; Ehrens, P.; Eichholz, J.; Eikenberry, S. S.; Engels, W.; Essick, R. C.; Etzel, T.; Evans, M.; Evans, T. M.; Everett, R.; Factourovich, M.; Fair, H.; Fairhurst, S.; Fan, X.; Fang, Qi; Farr, B.; Farr, W. M.; Favata, M.; Fays, M.; Fehrmann, H.; Fejer, M. M.; Fenyvesi, E.; Ferreira, E. C.; Fisher, R. P.; Fletcher, M.; Frei, Z.; Freise, A.; Frey, R.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gabbard, H. A.; Gair, J. R.; Gaonkar, S. G.; Gaur, G.; Gehrels, N.; Geng, Peng; George, J.; Gergely, L.; Ghosh, Abhirup; Ghosh, Archisman; Giaime, J. A.; Giardina, K. 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K.; Jiménez-Forteza, F.; Johnson, W. W.; Jones, D. I.; Jones, R.; Li, Ju; Haris, K.; Kalaghatgi, C. V.; Kalogera, V.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Kapadia, S. J.; Karki, S.; Karvinen, K. S.; Kasprzack, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kaur, Tejinder; Kawabe, K.; Kehl, M. S.; Keitel, D.; Kelley, D. B.; Kells, W.; Kennedy, R.; Key, J. S.; Khalili, F. Y.; Khan, S.; Khan, Z.; Khazanov, E. A.; Kijbunchoo, N.; Kim, Chi Woong; Kim, Chunglee; Kim, J.; Kim, K.; Kim, N.; Kim, W.; Kim, Y. M.; Kimbrell, S. J.; King, E. J.; King, Peter; Kissel, J. S.; Klein, Bernd; Kleybolte, L.; Klimenko, S.; Koehlenbeck, S. M.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W. Z.; Kozak, D. B.; Kringel, V.; Krueger, C.; Kuehn, G.; Kumar, P.; Kumar, Rakesh; Kuo, L.; Lackey, B. D.; Landry, M.; Lange, J.; Lantz, B.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Leavey, S.; Lebigot, E. O.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, K.; Lenon, A.; Leong, J. R.; Levin, Y.; Lewis, Jeffrey B.; Li, T. G F; Libson, A.; Littenberg, T. B.; Lockerbie, N. A.; Lombardi, A. L.; London, L. T.; Lord, J. E.; Lormand, M.; Lough, J. D.; Lück, H.; Lundgren, A. P.; Lynch, R.; Ma, Y.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Magaña-Sandoval, F.; Zertuche, L. Magaña; Magee, R. M.; Mandic, V.; Mangano, V.; Mansell, G. L.; Manske, M.; Márka, S.; Márka, Z.; Markosyan, A. S.; Maros, E.; Martin, I. W.; Мартынов, Д. В.; Mason, K.; Massinger, T. J.; Masso-Reid, M.; Matichard, F.; Matone, L.; Mavalvala, N.; Mazumder, N.; McCarthy, R.; McClelland, D. E.; McCormick, S.; McGuire, S. C.; McIntyre, G.; McIver, J.; McManus, D. J.; McRae, T.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.; Melatos, A.; Mendell, G.; Mercer, R. A.; Merilh, E. L.; Meshkov, S.; Messenger, C.; Messick, C.; Meyers, P. M.; Miao, H.; Middleton, H.; Михайлов, Е. Е.; Miller, A.; Miller, A. L.; Miller, B. B.; Miller, John M.; Millhouse, M.; Ming, J.; Mirshekari, S.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Mohapatra, S. R. P.; Moore, B. C.; Moore, C. J.; Moraru, D.; Moreno, G.; Morriss, S. R.; Mossavi, K.; Mow–Lowry, C. M.; Mueller, G.; Muir, A. W.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, Sajal; Mukund, N.; Mullavey, A.; Münch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.; Nayak, R. K.; Nedkova, K.; Nelson, T. J. N.; Neunzert, A.; Newton, G.; Nguyen, T. T.; Nielsen, A. B.; Nitz, A.; Nolting, D.; Normandin, M. E. N.; Nuttall, L. K.; Oberling, J.; Ochsner, E.; O’Dell, J.; Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh, Sang Hoon; Ohme, F.; Oliver, M.; Oppermann, P.; Oram, Richard J.; O’Reilly, B.; O’Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pai, A.; Pai, S. A.; Palamos, J. R.; Palashov, O.; Pal-Singh, A.; Pan, H.; Pankow, C.; Pannarale, F.; Pant, B. C.; Papa, M. A.; Paris, H. R.; Parker, W.; Pascucci, D.; Patrick, Z.; Pearlstone, B. L.; Pedraza, M.; Pekowsky, L.; Pele, A.; Penn, S.; Perreca, A.; Perri, L. M.; Phelps, M.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Poe, M.; Post, A.; Powell, J.; Prasad, J.; Predoi, V.; Prestegard, T.; Price, Larry R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prokhorov, L.; Puncken, O.; Pürrer, M.; Qi, H.; Qin, J.; Qiu, S.; Quetschke, V.; Quintero, E. A.; Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Raja, S.; Rajan, C.; Rakhmanov, M.; Raymond, V.; Read, J.; Reed, C. M.; Reid, S.; Reitze, D. H.; Rew, H.; Reyes, S. D.; Riles, K.; Rizzo, Maria L.; Robertson, N. A.; Robie, R.; Rollins, J. G.; Roma, V. J.; Romanov, G.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadeghian, L.; Sakellariadou, Mairi; Saleem, M.; Salemi, F.; Samajdar, A.; Sammut, L.; Sanchez, E. J.; Sandberg, V.; Sandeen, B.; Sanders, J. R.; Sathyaprakash, B. S.; Saulson, P. R.; Sauter, O.; Savage, R. L.; Sawadsky, A.; Schale, P.; Schilling, R.; Schmidt, J.; Schmidt, P.; Schnabel, R.; Schofield, R. M. 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V.; Toland, K.; Tomlinson, C.; Tornasi, Z.; Torres, C. V.; Torrie, C. I.; Töyrä, D.; Traylor, G.; Trifirò, D.; Tse, M.; Tuyenbayev, D.; Ugolini, D.; Unnikrishnan, C. S.; Urban, A. L.; Usman, S. A.; Vahlbruch, H.; Vajente, G.; Valdes, G.; Vander-Hyde, D. C.; Veggel, A. A. van; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P. J.; Venkateswara, K.; Vinciguerra, S.; Vine, D. J.; Vitale, Salvatore; Vo, T.; Vorvick, C.; Voss, D. V.; Vousden, W. D.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade, M.; Walker, M.; Wallace, L.; Walsh, S.; Wang, H.; Wang, M.; Wang, X.; Wang, Y.; Ward, R. L.; Warner, J.; Weaver, B.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Weßels, P.; Westphal, T.; Wette, K.; Whelan, J. T.; Williams, R. D.; Williamson, A. R.; Willis, J. L.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wipf, C. C.; Wittel, H.; Woan, G.; Woehler, J.; Worden, J.; Wright, J. L.; Wu, D. S.; Wu, G.; Yablon, J.; Yam, W.; Yamamoto, H.; Yancey, C. C.; Yu, Hang; Zanolin, M.; Zevin, M.; Zhang, L.; Zhang, M.; Zhang, Y.; Zhao, C.; Zhou, M.; Zhou, Z.; Zhu, X. J.; Zucker, M. E.; Zuraw, S. E.; Zweizig, J.; Harms, J.

doi:10.1088/1361-6382/aa51f4

Cited by 1,032 publications

(767 citation statements)

References 94 publications

(129 reference statements)

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“…Cosmic Explorer: There is also a proposal for a Cosmic Explorer detector [61,65], which would be around a factor of 3 more sensitive than ET. The design and technology used is similar to ET but with arm length that can stretch out to between 40 to 50 km.…”

Section: Future Detectors and Networkmentioning

confidence: 99%

“…1 we show the sensitivities of the proposed future detectors [65], as well as the advanced LIGO design sensitivity. We show the ET xylophone configuration, called ET-D. Also included for comparison is ET-B, which is an alternative ET configuration where every interferometer is optimized for best overall sensitivity, but at the expense of some low frequency sensitivity.…”

Section: Future Detectors and Networkmentioning

confidence: 99%

“…Additionally, entirely new detectors have been proposed. The Einstein Telescope is a next-generation European gravitational wave observatory [62][63][64], and Cosmic Explorer [65] is a proposed US-based future detector, both of which improve on the advanced detector sensitivity by a factor of 10 or more. As well as revealing new sources of gravitational waves, these detectors will allow us to observe BBH mergers throughout most of the history of the Universe [66] and BNS to cosmological distances [67][68][69][70].…”

Section: Introductionmentioning

confidence: 99%

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Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Mills¹,

Tiwari²,

Fairhurst³

2018

Phys. Rev. D

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The observation of gravitational wave signals from binary black hole and binary neutron star mergers has established the field of gravitational wave astronomy. It is expected that future networks of gravitational wave detectors will possess great potential in probing various aspects of astronomy. An important consideration for successive improvement of current detectors or establishment on new sites is knowledge of the minimum number of detectors required to perform precision astronomy. We attempt to answer this question by assessing the ability of future detector networks to detect and localize binary neutron stars mergers on the sky. Good localization ability is crucial for many of the scientific goals of gravitational wave astronomy, such as electromagnetic follow-up, measuring the properties of compact binaries throughout cosmic history, and cosmology. We find that although two detectors at improved sensitivity are sufficient to get a substantial increase in the number of observed signals, at least three detectors of comparable sensitivity are required to localize majority of the signals, typically to within around 10 deg 2 -adequate for follow-up with most wide field of view optical telescopes.

show abstract

Section: Future Detectors and Networkmentioning

confidence: 99%

Section: Future Detectors and Networkmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Mills¹,

Tiwari²,

Fairhurst³

2018

Phys. Rev. D

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“…3. Curves presented in [8] assume sources nearly, but not exactly, overhead the detectors. We only show the directional dependence for CE because all other detectors are short enough that the effects are small.…”

Section: Fig 4 Amplitude Spectralmentioning

confidence: 99%

“…However, planning for 3rd generation detectors, such as Cosmic Explorer (CE) [8] and the Einstein Telescope (ET) [9] has already begun. Among other technological improvements, 3rd generation detectors will have longer arms than the current detectors, with ET proposing a 10 km triangular design [10] and CE a 40 km L-shaped detector, an order of magnitude longer than the current LIGO detectors.…”

Section: Introductionmentioning

confidence: 99%

Frequency-dependent responses in third generation gravitational-wave detectors

2017

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Interferometric gravitational-wave detectors are dynamic instruments. Changing gravitational-wave strains influence the trajectories of null geodesics and therefore modify the interferometric response. These effects will be important when the associated frequencies are comparable to the round-trip light travel time down the detector arms. The arms of advanced detectors currently in operation are short enough that the strain can be approximated as static, but planned 3rd generation detectors, with arms an order of magnitude longer, will need to account for these effects. We investigate the impact of neglecting the frequencydependent detector response for compact binary coalescences and show that it can introduce large systematic biases in localization, larger than the statistical uncertainty for 1.4-1.4 M ⊙ neutron star coalescences at z ≲ 1.7. Analysis of 3rd generation detectors therefore must account for these effects.

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Forecasting Gamma‐Ray Bursts Using Gravitational Waves

Akçay

2018

Annalen der Physik

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The intriguing possibility of employing future ground-based gravitational-wave interferometers to forecast short gamma-ray bursts (GRBs) is explored. The forecasting prospect is quantified in terms of an advance-warning time: the binary-neutron star (BNS) inspiral time (to merger) from when the interferometer network accumulates a signal-to-noise ratio of 15. As sources for the Advanced LIGO-Virgo (ALV) network of 2020, BNS systems at luminosity distances of D ≤ 200 Mpc are considered, and similarly, BNS systems at D ≤ 1000 Mpc for Einstein Telescope. It is shown that the ALV network will provide a few minutes of warning time, thus will not forecast GRBs in the 2020s. On the other hand, Einstein Telescope will provide advance-warning times of more than 5 hours for D ≤ 100 Mpc. Taking 1 hour as a benchmark advance-warning time, a corresponding BNS range of roughly 600 Mpc is obtained for Einstein Telescope. Using current BNS event rates, it is shown that Einstein Telescope will forecast O(10 2 ) GRBs in the 2030s. This warning-time computation is reapplied to black hole-neutron star inspirals and it is found that one to three tidal disruption events are expected to be forecast by the same detector.

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Exploring the sensitivity of next generation gravitational wave detectors

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Cited by 1,032 publications

References 94 publications

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Frequency-dependent responses in third generation gravitational-wave detectors

Forecasting Gamma‐Ray Bursts Using Gravitational Waves

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