Searching for a Stochastic Background of Gravitational Waves with the Laser Interferometer Gravitational-Wave Observatory

Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Agresti, J.; Ajith, P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Araya, M. C.; Armandula, H.; Ashley, M. C. B.; Aston, S. M.; Aulbert, C.; Babak, S.; Ballmer, S. W.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer, K.; Belczyński, Krzysztof; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Black, E.; Blackburn, K.; Blackburn, L.; Blair, David; Bland, B.; Bogue, L.; Bork, R.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brooks, A. F.; Brown, D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.; Burman, R.; Busby, D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J. K.; Cannon, K. C.; Cantley, C. A.; Cao, J.; Cardenas, L.; Casey, M. M.; Cepeda, C.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chin, D.; Chin, E.; Chow, J. H.; Christensen, N.; Cokelaer, Thomas; Colacino, C. N.; Coldwell, R. L.; Cook, D.; Corbitt, T. R.; Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.; Cutler, Curt; Dalrymple, James; D’Ambrosio, E.; Danzmann, K.; Davies, G. S.; Vine, Glen de; DeBra, D.; Degallaix, J.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandar, S.; Credico, A. Di; Díaz, M. C.; Dickson, J.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. C.; Dupuis, R. J.; Ehrens, P.; Elliffe, E. J.; Etzel, T.; Evans, M.; Evans, T. M.; Fairhurst, S.; Fan, Y.; Fejer, M. M.; Finn, L. S.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.; Frey, R.; Fricke, T. T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Goda, Keisuke; Goetz, E.; Goggin, L. M.; González, Gabriela; Goßler, S.; Grant, A.; Gras, S.; Gray, C.; Gray, Malcolm B.; Greenhalgh, J.; Gretarsson, A. M.; Grimmett, D.; Grosso, R.; Grote, H.; Grünewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hanna, C.; Hanson, J.; Hardham, C.; Harms, J.; Harry, G. M.; Harstad, E. D.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson, M.; Hild, S.; Hindman, Neil; Hirose, E.; Hoak, D.; Hoang, P.; Hosken, D. J.; Hough, J.; Howell, E. J.; Hoyland, D.; Hua, W.; Huttner, S. H.; Ingram, D. R.; Ito, Masahiro; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.; Jones, D. I.; Jones, Gareth; Jones, R.; Li, Ju; Kalmus, P.; Kalogera, V.; Kasprzyk, Dimitri; Katsavounidis, E.; Kawabe, K.; Kawamura, Seiji; Kawazoe, F.; Kells, W.; Khalili, F. Y.; Khan, A.; Kim, C.; King, P. J.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Koranda, S.; Kozak, D. B.; Krishnan, B.; Kwee, P.; Lam, Ping Koy; Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leonhardt, V.; Leonor, I.; Libbrecht, K. G.; Lindquist, P.; Lockerbie, N. A.; Lormand, M.; Łubiński, M.; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Márka, S.; Markowitz, J.; Maros, E.; Martin, Ian; Marx, J. N.; Mason, K.; Matone, L.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie, Kirk; McNabb, J. W.; Meier, T.; Melissinos, A. C.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger, C.; Meyers, D.; Михайлов, Е. Е.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, Soumya D.; Moreno, G.; Mossavi, K.; Mow–Lowry, C. M.; Moylan, A.; Mudge, D.; Mueller, G.; Müller‐Ebhardt, H.; Mukherjee, Soma; Münch, J.; Murray, P. G.; Myers, E.; Myers, J.; Newton, G.; Numata, Kenji; O’Reilly, B.; O’Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Pedraza, M.; Penn, S.; Pitkin, M.; Plissi, M. V.; Prix, R.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Rahkola, R.; Rakhmanov, M.; Rawlins, K.; Ray‐Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, Rolf; Riles, K.; Rivera, B.; Robertson, D. I.; Robertson, N. A.; Robinson, C.; Roddy, S.; Rodríguez, A.; Rogan, A. M.; Rollins, J. G.; Romano, Joseph D.; Romie, J. H.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, Laurent; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.; Jordana, L. Sancho De La; Sandberg, V.; Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.; Schediwy, Sascha; Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Seader, Shawn; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan, P.; Sheard, Ben; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Sneddon, P.; Somiya, K.; Speake, C. C.; Spjeld, O.; Strain, K. A.; Strom, D.; Stuver, A. L.; Summerscales, T. Z.; Sun, K. X.; Sung, M.; Sutton, P. J.; Tanner, D. B.; Tarallo, M.; Taylor, Robert W.; Thacker, John G.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres, C. V.; Torrie, C. I.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Vahlbruch, H.; Vallisneri, Michele; Varvella, M.; Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P. J.; Vigeland, Sarah J.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R. L.; Watts, K.; Webber, David; Weidner, A.; Weinstein, A. J.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Willke, B.; Wilmut, Ian; Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, Alan; Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, Nicolás; Zanolin, M.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Mühlen, Heribert; Zweizig, J.

doi:10.1086/511329

Cited by 133 publications

(157 citation statements)

References 35 publications

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“…The nearest binaries are expected to produce loud chirp-like signals that could be individually detected by the upcoming detectors. However, such loud transients are typically explicitly excluded from the searches for GWB [30][31][32][33]. We have verified that the nearest (and loudest) binaries contribute little to Ω GW : Figure 2 shows the gravitationalwave spectrum Ω GW (f ) computed for the BNS case with…”

Section: Calculation Of the Energy Spectrummentioning

confidence: 72%

“…The LIGO and Virgo collaborations have developed techniques for searching for GWB by cross-correlating data from pairs of gravitational wave detectors [30]. Such searches have also been performed using LIGO and Virgo data [31][32][33], and have produced competitive upper limits on the energy density carried by gravitational waves. The goal of this paper is to perform a detailed study of the accessibility of the GWB produced by the binary coalescences to the second and third generation gravitational-wave detectors.…”

Section: Introductionmentioning

confidence: 99%

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Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

2012

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International audienceCompact binary coalescences, such as binary neutron stars or black holes, are among the most promising candidate sources for the current and future terrestrial gravitational-wave detectors. While such sources are best searched using matched template techniques and chirp template banks, integrating chirp signals from binaries over the entire universe also leads to a gravitational-wave background (GWB). In this paper we systematically scan the parameter space for the binary coalescence GWB models, taking into account uncertainties in the star formation rate and in the delay time between the formation and coalescence of the binary, and we compare the computed GWB to the expected sensitivities of the second and third generation gravitational-wave detector networks. We find that second generation detectors are likely to detect the binary coalescence GWB, while the third generation detectors will probe most of the available parameter space. The binary coalescence GWB will, in fact, be a foreground for the third generation detectors, potentially masking the GWB background due to cosmological sources. Accessing the cosmological GWB with third generation detectors will therefore require identification and subtraction of all inspiral signals from all binaries in the detectors’ frequency band

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Section: Calculation Of the Energy Spectrummentioning

confidence: 72%

Section: Introductionmentioning

confidence: 99%

Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

2012

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“…One of the ground-based experiments, LIGO [24], is in operation and it is sensitive to the frequency between O(10) Hz and 10 4 Hz. The latest upper bound is Ω gw h 2 < 6.5 × 10 −5 around 100 Hz [25], and an upgrade of the experiment, Advanced LIGO, would reach sensitivities of O(10 −9 ). The sensitivity of LCGT would be more or less similar to that of Advanced LIGO.…”

Section: Gravitational Wavesmentioning

confidence: 99%

Gravitational waves as a probe of the gravitino mass

2008

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If gaugino condensations occur in the early universe, domain walls are produced as a result of the spontaneous breaking of a discrete R symmetry. Those domain walls eventually annihilate with one another, producing the gravitational waves. We show that the gravitational waves can be a probe for measuring the gravitino mass, if the constant term in the superpotential is the relevant source of the discrete R symmetry breaking.

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“…Summing up the contributions to the cross-correlation in the frequency band 41.5-169.25 Hz, which contains 99% of the sensitivity, leads to the final point estimate for the frequency independent gravitational-wave spectrum (a 5 0): V 0 5 (2.1 6 2.7) 3 10 26 , where the quoted error is statistical. We calculate the Bayesian 95% confidence upper limit for V 0 , using the previous LIGO result (S4 run 22 ) as a prior for V 0 and averaging over the interferometer calibration uncertainty. This procedure yields the 95% confidence upper limit V 0 , 6.9 3 10 26 .…”

mentioning

confidence: 99%

An upper limit on the stochastic gravitational-wave background of cosmological origin

Abbott¹,

Abbott²,

Acernese³

et al. 2009

Nature

313

154

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A stochastic background of gravitational waves is expected to arise from a superposition of a large number of unresolved gravitational-wave sources of astrophysical and cosmological origin. It should carry unique signatures from the earliest epochs in the evolution of the Universe, inaccessible to standard astrophysical observations(1). Direct measurements of the amplitude of this background are therefore of fundamental importance for understanding the evolution of the Universe when it was younger than one minute. Here we report limits on the amplitude of the stochastic gravitational-wave background using the data from a two-year science run of the Laser Interferometer Gravitational-wave Observatory(2) (LIGO). Our result constrains the energy density of the stochastic gravitational-wave background normalized by the critical energy density of the Universe, in the frequency band around 100 Hz, to be <6.9 X 10(-6) at 95% confidence. The data rule out models of early Universe evolution with relatively large equation-of-state parameter(3), as well as cosmic (super) string models with relatively small string tension(4) that are favoured in some string theory models(5). This search for the stochastic background improves on the indirect limits from Big Bang nucleosynthesis(1,6) and cosmic microwave background(7) at 100Hz

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Searching for a Stochastic Background of Gravitational Waves with the Laser Interferometer Gravitational-Wave Observatory

Cited by 133 publications

References 35 publications

Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

Gravitational waves as a probe of the gravitino mass

An upper limit on the stochastic gravitational-wave background of cosmological origin

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