First cross-correlation analysis of interferometric and resonant-bar gravitational-wave data for stochastic backgrounds

Data from the LIGO Livingston interferometer and the ALLEGRO resonant-bar detector, taken during LIGO's fourth science run, were examined for cross correlations indicative of a stochastic gravitational-wave background in the frequency range 850-950 Hz, with most of the sensitivity arising between 905 and 925 Hz. ALLEGRO was operated in three different orientations during the experiment to modulate the relative sign of gravitational-wave and environmental correlations. No statistically significant correlations were seen in any of the orientations, and the results were used to set a Bayesian 90% confidence level upper limit of Ωgw(f)≤1.02, which corresponds to a gravitational-wave strain at 915 Hz of 1.5×10-23Hz-1/2. In the traditional units of h1002Ωgw(f), this is a limit of 0.53, 2 orders of magnitude better than the previous direct limit at these frequencies. The method was also validated with successful extraction of simulated signals injected in hardware and software. © 2007 The American Physical Society.

First cross-correlation analysis of interferometric and resonant-bar gravitational-wave data for stochastic backgrounds

Abbott B.;Abbott R.;Adhikari R.;Agresti J.;Ajith P.;Allen B.;Amin R.;Anderson S. B.;Anderson W. G.;Arain M.;Araya M.;Armandula H.;Ashley M.;Aston S.;Aufmuth P.;Aulbert C.;Babak S.;Ballmer S.;Bantilan H.;Barish B. C.;Barker C.;Barker D.;Barr B.;Barriga P.;Barton M. A.;Bayer K.;Belczynski K.;Betzwieser J.;Beyersdorf P. T.;Bhawal B.;Bilenko I. A.;Billingsley G.;Biswas R.;Black E.;Blackburn K.;Blackburn L.;Blair D.;Bland B.;Bogenstahl J.;Bogue L.;Bork R.;Boschi V.;Bose S.;Brady P. R.;Braginsky V. B.;Brau J. E.;Brinkmann M.;Brooks A.;Brown D. A.;Bullington A.;Bunkowski A.;Buonanno A.;Burgamy M.;Burmeister O.;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.;Castaldi G.;Cepeda C.;Chalkey E.;Charlton P.;Chatterji S.;Chelkowski S.;Chen Y.;Chiadini F.;Chin D.;Chin E.;Chow J.;Christensen N.;Clark J.;Cochrane P.;Cokelaer T.;Colacino C. N.;Coldwell R.;Conte R.;Cook D.;Corbitt T.;Coward D.;Coyne D.;Creighton J. D. E.;Creighton T. D.;Croce R. P.;Crooks D. R. M.;Cruise A. M.;Cumming A.;Dalrymple J.;D'Ambrosio E.;Danzmann K.;Davies G.;DeBra D.;Degallaix J.;Degree M.;Demma T.;Dergachev V.;Desai S.;DeSalvo R.;Dhurandhar S.;Diaz M.;Dickson J.;Di Credico A.;Diederichs G.;Dietz A.;Doomes E. E.;Drever R. W. P.;Dumas J. -C.;Dupuis R. J.;Dwyer J. G.;Ehrens P.;Espinoza E.;Etzel T.;Evans M.;Evans T.;Fairhurst S.;Fan Y.;Fazi D.;Fejer M. M.;Finn L. S.;Fiumara V.;Fotopoulos N.;Franzen A.;Franzen K. Y.;Freise A.;Frey R.;Fricke T.;Fritschel P.;Frolov V. V.;Fyffe M.;Galdi V.;Garofoli J.;Gholami I.;Giaime J. A.;Giampanis S.;Giardina K. D.;Goda K.;Goetz E.;Goggin L.;Gonzalez G.;Gossler S.;Grant A.;Gras S.;Gray C.;Gray M.;Greenhalgh J.;Gretarsson A. M.;Grosso R.;Grote H.;Grunewald S.;Guenther M.;Gustafson R.;Hage B.;Hamilton W. O.;Hammer D.;Hanna C.;Hanson J.;Harms J.;Harry G.;Harstad E.;Hayler T.;Heefner J.;Heng I. S.;Heptonstall A.;Heurs M.;Hewitson M.;Hild S.;Hirose E.;Hoak D.;Hosken D.;Hough J.;Howell E.;Hoyland D.;Huttner S. H.;Ingram D.;Innerhofer E.;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.;Keppel D. G.;Khalili F. Ya.;Kim C.;King P.;Kissel J. S.;Klimenko S.;Kokeyama K.;Kondrashov V.;Kopparapu R. K.;Kozak D.;Krishnan B.;Kwee P.;Lam P. K.;Landry M.;Lantz B.;Lazzarini A.;Lee B.;Lei M.;Leiner J.;Leonhardt V.;Leonor I.;Libbrecht K.;Lindquist P.;Lockerbie N. A.;Longo M.;Lormand M.;Lubinski M.;Luck H.;Machenschalk B.;MacInnis M.;Mageswaran M.;Mailand K.;Malec M.;Mandic V.;Marano S.;Marka S.;Markowitz J.;Maros E.;Martin I.;Marx J. N.;Mason K.;Matone L.;Matta V.;Mavalvala N.;McCarthy R.;McCaulley B. J.;McClelland D. E.;McGuire S. C.;McHugh M.;McKenzie K.;McNabb J. W. C.;McWilliams S.;Meier T.;Melissinos A.;Mendell G.;Mercer R. A.;Meshkov S.;Messaritaki E.;Messenger C. J.;Meyers D.;Mikhailov E.;Miller P.;Mitra S.;Mitrofanov V. P.;Mitselmakher G.;Mittleman R.;Miyakawa O.;Mohanty S.;Moody V.;Moreno G.;Mossavi K.;Mowlowry C.;Moylan A.;Mudge D.;Mueller G.;Mukherjee S.;Muller-Ebhardt H.;Munch J.;Murray P.;Myers E.;Myers J.;Nash T.;Nettles D.;Newton G.;Nishizawa A.;Numata K.;O'Reilly B.;O'Shaughnessy R.;Ottaway D. J.;Overmier H.;Owen B. J.;Paik H. -J.;Pan Y.;Papa M. A.;Parameshwaraiah V.;Patel P.;Pedraza M.;Penn S.;Pierro V.;Pinto I. M.;Pitkin M.;Pletsch H.;Plissi M. V.;Postiglione F.;Prix R.;Quetschke V.;Raab F.;Rabeling D.;Radkins H.;Rahkola R.;Rainer N.;Rakhmanov M.;Ramsunder M.;Rawlins K.;Ray-Majumder S.;Re V.;Rehbein H.;Reid S.;Reitze D. H.;Ribichini L.;Riesen R.;Riles K.;Rivera B.;Robertson N. A.;Robinson C.;Robinson E. L.;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.;Sancho De La Jordana L.;Sandberg V.;Sannibale V.;Saraf S.;Sarin P.;Sathyaprakash B. S.;Sato S.;Saulson P. R.;Savage R.;Savov P.;Schediwy S.;Schilling R.;Schnabel R.;Schofield R.;Schutz B. F.;Schwinberg P.;Scott S. M.;Searle A. C.;Sears B.;Seifert F.;Sellers D.;Sengupta A. S.;Shawhan P.;Shoemaker D. H.;Sibley A.;Sidles J. A.;Siemens X.;Sigg D.;Sinha S.;Sintes A. M.;Slagmolen B. J. J.;Slutsky J.;Smith J. R.;Smith M. R.;Somiya K.;Strain K. A.;Strom D. M.;Stuver A.;Summerscales T. Z.;Sun K. -X.;Sung M.;Sutton P. J.;Takahashi H.;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.;Urbanek K.;Vahlbruch H.;Vallisneri M.;Van Den Broeck C.;Varvella M.;Vass S.;Vecchio A.;Veitch J.;Veitch P.;Villar A.;Vorvick C.;Vyachanin S. P.;Waldman S. J.;Wallace L.;Ward H.;Ward R.;Watts K.;Weaver J.;Webber D.;Weber A.;Weidner A.;Weinert M.;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.;Williams L.;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 J.;Zhang L.;Zhang P.;Zhao C.;Zotov N.;Zucker M.;Zur Muhlen H.;Zweizig J.

2007

Abstract

Data from the LIGO Livingston interferometer and the ALLEGRO resonant-bar detector, taken during LIGO's fourth science run, were examined for cross correlations indicative of a stochastic gravitational-wave background in the frequency range 850-950 Hz, with most of the sensitivity arising between 905 and 925 Hz. ALLEGRO was operated in three different orientations during the experiment to modulate the relative sign of gravitational-wave and environmental correlations. No statistically significant correlations were seen in any of the orientations, and the results were used to set a Bayesian 90% confidence level upper limit of Ωgw(f)≤1.02, which corresponds to a gravitational-wave strain at 915 Hz of 1.5×10-23Hz-1/2. In the traditional units of h1002Ωgw(f), this is a limit of 0.53, 2 orders of magnitude better than the previous direct limit at these frequencies. The method was also validated with successful extraction of simulated signals injected in hardware and software. © 2007 The American Physical Society.

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Scheda completa

Scheda completa (DC)

	Anno
	
				2007
			
	Rivista su cui è pubblicata l'opera
	
				PHYSICAL REVIEW D, PARTICLES, FIELDS, GRAVITATION, AND COSMOLOGY
			
	Codice DOI
	
				https://dx.doi.org/10.1103/PhysRevD.76.022001
			
	Codice Scopus
	
				2-s2.0-34447268891
			
	Appare nelle tipologie:
	
				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/11577/3578116

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