Upper limits on a stochastic background of gravitational waves

The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with much improved sensitivities of all three interferometers. We present an analysis of approximately 200 hours of data acquired during this run, used to search for a stochastic background of gravitational radiation. We place upper bounds on the energy density stored as gravitational radiation for three different spectral power laws. For the flat spectrum, our limit of 0 < 8.4 × 10 -4 in the 69-156 Hz band is ∼10 5 times lower than the previous result in this frequency range. © 2005 The American Physical Society.

Upper limits on a stochastic background of gravitational waves

Abbott B.;Abbott R.;Adhikari R.;Agresti J.;Ajith P.;Allen B.;Allen J.;Amin R.;Anderson S. B.;Anderson W. G.;Araya M.;Armandula H.;Ashley M.;Aulbert C.;Babak S.;Balasubramanian R.;Ballmer S.;Barish B. C.;Barker C.;Barker D.;Barton M. A.;Bayer K.;Belczynski K.;Betzwieser J.;Bhawal B.;Bilenko I. A.;Billingsley G.;Black E.;Blackburn K.;Blackburn L.;Bland B.;Bogue L.;Bork R.;Bose S.;Brady P. R.;Braginsky V. B.;Brau J. E.;Brown D. A.;Buonanno A.;Busby D.;Butler W. E.;Cadonati L.;Cagnoli G.;Camp J. B.;Cannizzo J.;Cannon K.;Cardenas L.;Carter K.;Casey M. M.;Charlton P.;Chatterji S.;Chen Y.;Chin D.;Christensen N.;Cokelaer T.;Colacino C. N.;Coldwell R.;Cook D.;Corbitt T.;Coyne D.;Creighton J. D. E.;Creighton T. D.;Dalrymple J.;D'Ambrosio E.;Danzmann K.;Davies G.;DeBra D.;Dergachev V.;Desai S.;DeSalvo R.;Dhurandar S.;Diaz M.;Di Credico A.;Drever R. W. P.;Dupuis R. J.;Ehrens P.;Etzel T.;Evans M.;Evans T.;Fairhurst S.;Finn L. S.;Franzen K. Y.;Frey R. E.;Fritschel P.;Frolov V. V.;Fyffe M.;Ganezer K. S.;Garofoli J.;Gholami I.;Giaime J. A.;Goda K.;Goggin L.;Gonzalez G.;Gray C.;Gretarsson A. M.;Grimmett D.;Grote H.;Grunewald S.;Guenther M.;Gustafson R.;Hamilton W. O.;Hanna C.;Hanson J.;Hardham C.;Harry G.;Heefner J.;Heng I. S.;Hewitson M.;Hindman N.;Hoang P.;Hough J.;Hua W.;Ito M.;Itoh Y.;Ivanov A.;Johnson B.;Johnson W. W.;Jones D. I.;Jones G.;Jones L.;Kalogera V.;Katsavounidis E.;Kawabe K.;Kawamura S.;Kells W.;Khan A.;Kim C.;King P.;Klimenko S.;Koranda S.;Kozak D.;Krishnan B.;Landry M.;Lantz B.;Lazzarini A.;Lei M.;Leonor I.;Libbrecht K.;Lindquist P.;Liu S.;Lormand M.;Lubinski M.;Luck H.;Luna M.;Machenschalk B.;Maclnnis M.;Mageswaran M.;Mailand K.;Malec M.;Mandic V.;Marka S.;Maros E.;Mason K.;Matone L.;Mavalvala N.;McCarthy R.;McClelland D. E.;McHugh M.;McNabb J. W. C.;Melissinos A.;Mendell G.;Mercer R. A.;Meshkov S.;Messaritaki E.;Messenger C.;Mikhailov E.;Mitra S.;Mitrofanov V. P.;Mitselmakher G.;Mittleman R.;Miyakawa O.;Mohanty S.;Moreno G.;Mossavi K.;Mueller G.;Mukherjee S.;Myers E.;Myers J.;Nash T.;Nocera F.;Noel J. S.;O'Reilly B.;O'Shaughnessy R.;Ottaway D. J.;Overmier H.;Owen B. J.;Pan Y.;Papa M. A.;Parameshwaraiah V.;Parameswariah C.;Pedraza M.;Penn S.;Pitkin M.;Prix R.;Quetschke V.;Raab F.;Radkins H.;Rahkola R.;Rakhmanov M.;Rawlins K.;Ray-Majumder S.;Re V.;Regimbau T.;Reitze D. H.;Riesen R.;Riles K.;Rivera B.;Robertson D. I.;Robertson N. A.;Robinson C.;Roddy S.;Rodriguez A.;Rollins J.;Romano J. D.;Romie J.;Rowan S.;Rudiger A.;Ruet L.;Russell P.;Ryan K.;Sandberg V.;Sanders G. H.;Sannibale V.;Sarin P.;Sathyaprakash B. S.;Saulson P. R.;Savage R.;Sazonov A.;Schilling R.;Schofleld R.;Schutz B. F.;Schwinberg P.;Scott S. M.;Seader S. E.;Searle A. C.;Sears B.;Sellers D.;Sengupta A. S.;Shawhan P.;Shoemaker D. H.;Sibley A.;Siemens X.;Sigg D.;Sintes A. M.;Smith J.;Smith M. R.;Spjeld O.;Strain K. A.;Strom D. M.;Stuver A.;Summerscales T.;Sung M.;Sutton P. J.;Tanner D. B.;Taylor R.;Thorne K. A.;Thorne K. S.;Tokmakov K. V.;Torres C.;Torrie C.;Traylor G.;Tyler W.;Ugolini D.;Ungarelli C.;Vallisneri M.;Van Putten M.;Vass S.;Vecchio A.;Veitch J.;Vorvick C.;Vyachanin S. P.;Wallace L.;Ward H.;Ward R.;Watts K.;Webber D.;Weiland U.;Weinstein A.;Weiss R.;Wen S.;Wette K.;Whelan J. T.;Whitcomb S. E.;Whiting B. F.;Wiley S.;Wilkinson C.;Willems P. A.;Willke B.;Wilson A.;Winkler W.;Wise S.;Wiseman A. G.;Woan G.;Woods D.;Wooley R.;Worden J.;Yakushin I.;Yamamoto H.;Yoshida S.;Zanolin M.;Zhang L.;Zotov N.;Zucker M.;Zweizig J.

2005

Abstract

The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with much improved sensitivities of all three interferometers. We present an analysis of approximately 200 hours of data acquired during this run, used to search for a stochastic background of gravitational radiation. We place upper bounds on the energy density stored as gravitational radiation for three different spectral power laws. For the flat spectrum, our limit of 0 < 8.4 × 10 -4 in the 69-156 Hz band is ∼10 5 times lower than the previous result in this frequency range. © 2005 The American Physical Society.

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	Anno
	
				2005
			
	Rivista su cui è pubblicata l'opera
	
				PHYSICAL REVIEW LETTERS
			
	Codice DOI
	
				https://dx.doi.org/10.1103/PhysRevLett.95.221101
			
	Codice Scopus
	
				2-s2.0-76249096276
			
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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/11577/3578166

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