Searching for a stochastic background of gravitational waves with the laser interferometer gravitational-wave observatory

The Laser Interferometer Gravitational-Wave Observatory (LIGO) has performed the fourth science run, S4, with significantly improved interferometer sensitivities with respect to previous runs. Using data acquired during this science run, we place a limit on the amplitude of a stochastic background of gravitational waves. For a frequency independent spectrum, the new Bayesian 90% upper limit is ΩGW × [H0/(12 km s-1 Mpc-1)]2 < 6.5 × 10-5. This is currently the most sensitive result in the frequency range 51-150 Hz, with a factor of 13 improvement over the previous LIGO result. We discuss the complementarity of the new result with other constraints on a stochastic background of gravitational waves, and we investigate implications of the new result for different models of this background. © 2007. The American Astronumical Society. All rights reserved.

Searching for a stochastic background of gravitational waves with the laser interferometer gravitational-wave observatory

Abbott B.;Abbott R.;Adhikari R.;Agresti J.;Ajith P.;Allen B.;Amin R.;Anderson S. B.;Anderson W. G.;Araya M.;Armandula H.;Ashley M.;Aston S.;Aulbert C.;Babak S.;Ballmer S.;Barish B. C.;Barker C.;Barker D.;Barr B.;Barriga P.;Barton M. A.;Bayer K.;Belczynski K.;Betzwieser J.;Beyersdorf P.;Bhawal B.;Bilenko I. A.;Billingsley G.;Black E.;Blackburn K.;Blackburn L.;Blair D.;Bland B.;Bogue L.;Bork R.;Bose S.;Brady P. R.;Braginsky V. B.;Brau J. E.;Brooks A.;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.;Cannon K.;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.;Christensen N.;Cokelaer T.;Colacino C. N.;Coldwell R.;Cook D.;Corbitt T.;Coward D.;Coyne D.;Creighton J. D. E.;Creighton T. D.;Crooks D. R. M.;Cruise A. M.;Cumming A.;Cutler C.;Dalrymple J.;D'Ambrosio E.;Danzmann K.;Davies G.;De Vine G.;DeBra D.;Degallaix J.;Dergachev V.;Desai S.;DeSalvo R.;Dhurandar S.;Di Credico A.;Diaz M.;Dickson J.;Diederichs G.;Dietz A.;Doomes E. E.;Drever R. W. P.;Dumas J. -C.;Dupuis R. J.;Ehrens P.;Elliffe E.;Etzel T.;Evans M.;Evans T.;Fairhurst S.;Fan Y.;Fejer M. M.;Finn L. S.;Fotopoulos N.;Franzen A.;Franzen K. Y.;Frey R. E.;Fricke T.;Fritschel P.;Frolov V. V.;Fyffe M.;Garofoli J.;Gholami I.;Giaime J. A.;Giampanis S.;Goda K.;Goetz E.;Goggin L.;Gonzalez G.;Gossler S.;Grant A.;Gras S.;Gray C.;Gray M.;Greenhalgh J.;Gretarsson A. M.;Grimmett D.;Grosso R.;Grote H.;Grunewald S.;Guenther M.;Gustafson R.;Hage B.;Hanna C.;Hanson J.;Hardham C.;Harms J.;Harry G.;Harstad E.;Hayler T.;Heefner J.;Heng I. S.;Heptonstall A.;Heurs M.;Hewitson M.;Hild S.;Hindman N.;Hirose E.;Hoak D.;Hoang P.;Hosken D.;Hough J.;Howell E.;Hoyland D.;Hua W.;Huttner S.;Ingram D.;Ito M.;Itoh Y.;Ivanov A.;Jackrel D.;Johnson B.;Johnson W. W.;Jones D. I.;Jones G.;Jones R.;Ju L.;Kalmus P.;Kalogera V.;Kasprzyk D.;Katsavounidis E.;Kawabe K.;Kawamura S.;Kawazoe F.;Kells W.;Khalili F. Ya.;Khan A.;Kim C.;King P.;Kumenko S.;Kokeyama K.;Kondrashov V.;Koranda S.;Kozak D.;Krishnan B.;Kwee P.;Lam P. K.;Landry M.;Lantz B.;Lazzarini A.;Lee B.;Lei M.;Leonhardt V.;Leonor I.;Libbrecht K.;Lindquist P.;Lockerbie N. A.;Lormand M.;Lubinski M.;Luck H.;Machenschalk B.;MacInnis M.;Mageswaran M.;Mailand K.;Malec M.;Mandic V.;Marka S.;Markowitz J.;Maros E.;Martin I.;Marx J. N.;Mason K.;Matone L.;Mavalvala N.;McCarthy R.;McClelland D. E.;McGuire S. C.;McHugh M.;McKenzie K.;McNabb J. W. C.;Meier T.;Melissinos A.;Mendell G.;Mercer R. A.;Meshkov S.;Messaritaki E.;Messenger C. J.;Meyers D.;Mikhailov E.;Mitra S.;Mitrofanov V. P.;Mitselmakher G.;Mittleman R.;Miyakawa O.;Mohanty S.;Moreno G.;Mossavi K.;MowLowry C.;Moylan A.;Mudge D.;Mueller G.;Muller-Ebhardt H.;Mukherjee S.;Munch J.;Murray P.;Myers E.;Myers J.;Newton G.;Numata K.;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.;Rabeling D.;Radkins H.;Rahkola R.;Rakhmanov M.;Rawlins K.;Ray-Majumder S.;Re V.;Rehbein H.;Reid S.;Reitze D. H.;Ribichini L.;Riesen R.;Riles K.;Rivera B.;Robertson D. I.;Robertson N. A.;Robinson C.;Roddy S.;Rodriguez A.;Rogan A. M.;Rollins J.;Romano J. D.;Romie J.;Route R.;Rowan S.;Rudiger A.;Ruet L.;Russell P.;Ryan K.;Sakata S.;Samidi M.;De La Jordana L. S.;Sandberg V.;Sannibale V.;Saraf S.;Sarin P.;Sathyaprakash B. S.;Sato S.;Saulson P. R.;Savage R.;Schediwy S.;Schilling R.;Schnabel R.;Schofield R.;Schutz B. F.;Schwinberg P.;Scott S. M.;Seader S. E.;Searle A. C.;Sears B.;Seifert F.;Sellers D.;Sengupta A. S.;Shawhan P.;Sheard B.;Shoemaker D. H.;Sibley A.;Siemens X.;Sigg D.;Sintes A. M.;Slagmolen B.;Slutsky J.;Smith J.;Smith M. R.;Sneddon P.;Somiya K.;Speake C.;Spjeld O.;Strain K. A.;Strom D. M.;Stuver A.;Summerscales T.;Sun K.;Sung M.;Sutton P. J.;Tanner D. B.;Tarallo M.;Taylor R.;Taylor R.;Thacker J.;Thorne K. A.;Thorne K. S.;Thuring A.;Tokmakov K. V.;Torres C.;Torrie C.;Traylor G.;Trias M.;Tyler W.;Ugolini D.;Ungarelli C.;Vahlbruch H.;Vallisneri M.;Varvella M.;Vass S.;Vecchio A.;Veitch J.;Veitch P.;Vigeland S.;Villar A.;Vorvick C.;Vyachanin S. P.;Waldman S. J.;Wallace L.;Ward H.;Ward R.;Watts K.;Webber D.;Weidner A.;Weinstein A.;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 I.;Winkler W.;Wipf C. C.;Wise S.;Wiseman A. G.;Woan G.;Woods D.;Wooley R.;Worden J.;Wu W.;Yakushin I.;Yamamoto H.;Yan Z.;Yoshida S.;Yunes N.;Zanolin M.;Zhang L.;Zhao C.;Zotov N.;Zucker M.;Zur Muhlen H.;Zweizig J.

2007

Abstract

The Laser Interferometer Gravitational-Wave Observatory (LIGO) has performed the fourth science run, S4, with significantly improved interferometer sensitivities with respect to previous runs. Using data acquired during this science run, we place a limit on the amplitude of a stochastic background of gravitational waves. For a frequency independent spectrum, the new Bayesian 90% upper limit is ΩGW × [H0/(12 km s-1 Mpc-1)]2 < 6.5 × 10-5. This is currently the most sensitive result in the frequency range 51-150 Hz, with a factor of 13 improvement over the previous LIGO result. We discuss the complementarity of the new result with other constraints on a stochastic background of gravitational waves, and we investigate implications of the new result for different models of this background. © 2007. The American Astronumical Society. All rights reserved.

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Scheda completa

Scheda completa (DC)

	Anno
	
				2007
			
	Rivista su cui è pubblicata l'opera
	
				THE ASTROPHYSICAL JOURNAL
			
	Codice DOI
	
				https://dx.doi.org/10.1086/511329
			
	Codice Scopus
	
				2-s2.0-34248341844
			
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				01.01 - Articolo in rivista

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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11577/3578168

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