Search for gravitational waves from galactic and extra-galactic binary neutron stars

We use 373 hours (≈15 days) of data from the second science run of the LIGO gravitational-wave detectors to search for signals from binary neutron star coalescences within a maximum distance of about 1.5 Mpc, a volume of space which includes the Andromeda Galaxy and other galaxies of the Local Group of galaxies. This analysis requires a signal to be found in data from detectors at the two LIGO sites, according to a set of coincidence criteria. The background (accidental coincidence rate) is determined from the data and is used to judge the significance of event candidates. No inspiral gravitational-wave events were identified in our search. Using a population model which includes the Local Group, we establish an upper limit of less than 47 inspiral events per year per Milky Way equivalent galaxy with 90% confidence for nonspinning binary neutron star systems with component masses between 1 and 3M. © 2005 The American Physical Society.

Search for gravitational waves from galactic and extra-galactic binary neutron stars

Abbott B.;Abbott R.;Adhikari R.;Ageev A.;Allen B.;Amin R.;Anderson S. B.;Anderson W. G.;Araya M.;Armandula H.;Ashley M.;Asiri F.;Aufmuth P.;Aulbert C.;Babak S.;Balasubramanian R.;Ballmer S.;Barish B. C.;Barker C.;Barker D.;Barnes M.;Barr B.;Barton M. A.;Bayer K.;Beausoleil R.;Belczynski K.;Bennett R.;Berukoff S. J.;Betzwieser J.;Bhawal B.;Bilenko I. A.;Billingsley G.;Black E.;Blackburn K.;Blackburn L.;Bland B.;Bochner B.;Bogue L.;Bork R.;Bose S.;Brady P. R.;Braginsky V. B.;Brau J. E.;Brown D. A.;Bullington A.;Bunkowski A.;Buonanno A.;Burgess R.;Busby D.;Butler W. E.;Byer R. L.;Cadonati L.;Cagnoli G.;Camp J. B.;Cantley C. A.;Cardenas L.;Carter K.;Casey M. M.;Castiglione J.;Chandler A.;Chapsky J.;Charlton P.;Chatterji S.;Chelkowski S.;Chen Y.;Chickarmane V.;Chin D.;Christensen N.;Churches D.;Cokelaer T.;Colacino C.;Coldwell R.;Coles M.;Cook D.;Corbitt T.;Coyne D.;Creighton J. D. E.;Creighton T. D.;Crooks D. R. M.;Csatorday P.;Cusack B. J.;Cutler C.;D'Ambrosio E.;Danzmann K.;Daw E.;Debra D.;Delker T.;Dergachev V.;Desalvo R.;Dhurandhar S.;Credico A. D.;Diaz M.;Ding H.;Drever R. W. P.;Dupuis R. J.;Edlund J. A.;Ehrens P.;Elliffe E. J.;Etzel T.;Evans M.;Evans T.;Fairhurst S.;Fallnich C.;Farnham D.;Fejer M. M.;Findley T.;Fine M.;Finn L. S.;Franzen K. Y.;Freise A.;Frey R.;Fritschel P.;Frolov V. V.;Fyffe M.;Ganezer K. S.;Garofoli J.;Giaime J. A.;Gillespie A.;Goda K.;Gonzalez G.;Gossler S.;Grandclement P.;Grant A.;Gray C.;Gretarsson A. M.;Grimmett D.;Grote H.;Grunewald S.;Guenther M.;Gustafson E.;Gustafson R.;Hamilton W. O.;Hammond M.;Hanson J.;Hardham C.;Harms J.;Harry G.;Hartunian A.;Heefner J.;Hefetz Y.;Heinzel G.;Heng I. S.;Hennessy M.;Hepler N.;Heptonstall A.;Heurs M.;Hewitson M.;Hild S.;Hindman N.;Hoang P.;Hough J.;Hrynevych M.;Hua W.;Ito M.;Itoh Y.;Ivanov A.;Jennrich O.;Johnson B.;Johnson W. W.;Johnston W. R.;Jones D. I.;Jones L.;Jungwirth D.;Kalogera V.;Katsavounidis E.;Kawabe K.;Kawamura S.;Kells W.;Kern J.;Khan A.;Killbourn S.;Killow C. J.;Kim C.;King C.;King P.;Klimenko S.;Koranda S.;Kotter K.;Kovalik J.;Kozak D.;Krishnan B.;Landry M.;Langdale J.;Lantz B.;Lawrence R.;Lazzarini A.;Lei M.;Leonor I.;Libbrecht K.;Libson A.;Lindquist P.;Liu S.;Logan J.;Lormand M.;Lubinski M.;Luck H.;Lyons T. T.;MacHenschalk B.;MacInnis M.;Mageswaran M.;Mailand K.;Majid W.;Malec M.;Mann F.;Marin A.;Marka S.;Maros E.;Mason J.;Mason K.;Matherny O.;Matone L.;Mavalvala N.;McCarthy R.;McClelland D. E.;McHugh M.;McNabb J. W. C.;Mendell G.;Mercer R. A.;Meshkov S.;Messaritaki E.;Messenger C.;Mitrofanov V. P.;Mitselmakher G.;Mittleman R.;Miyakawa O.;Miyoki S.;Mohanty S.;Moreno G.;Mossavi K.;Mueller G.;Mukherjee S.;Murray P.;Myers J.;Nagano S.;Nash T.;Nayak R.;Newton G.;Nocera F.;Noel J. S.;Nutzman P.;Olson T.;O'Reilly B.;Ottaway D. J.;Ottewill A.;Ouimette D.;Overmier H.;Owen B. J.;Pan Y.;Papa M. A.;Parameshwaraiah V.;Parameswaran A.;Parameswariah C.;Pedraza M.;Penn S.;Pitkin M.;Plissi M.;Prix R.;Quetschke V.;Raab F.;Radkins H.;Rahkola R.;Rakhmanov M.;Rao S. R.;Rawlins K.;Ray-Majumder S.;Re V.;Redding D.;Regehr M. W.;Regimbau T.;Reid S.;Reilly K. T.;Reithmaier K.;Reitze D. H.;Richman S.;Riesen R.;Riles K.;Rivera B.;Rizzi A.;Robertson D. I.;Robertson N. A.;Robison L.;Roddy S.;Rollins J.;Romano J. D.;Romie J.;Rong H.;Rose D.;Rotthoff E.;Rowan S.;Rudiger A.;Russell P.;Ryan K.;Salzman I.;Sandberg V.;Sanders G. H.;Sannibale V.;Sathyaprakash B.;Saulson P. R.;Savage R.;Sazonov A.;Schilling R.;Schlaufman K.;Schmidt V.;Schnabel R.;Schofield R.;Schutz B. F.;Schwinberg P.;Scott S. M.;Seader S. E.;Searle A. C.;Sears B.;Seel S.;Seifert F.;Sengupta A. S.;Shapiro C. A.;Shawhan P.;Shoemaker D. H.;Shu Q. Z.;Sibley A.;Siemens X.;Sievers L.;Sigg D.;Sintes A. M.;Smith J. R.;Smith M.;Smith M. R.;Sneddon P. H.;Spero R.;Stapfer G.;Steussy D.;Strain K. A.;Strom D.;Stuver A.;Summerscales T.;Sumner M. C.;Sutton P. J.;Sylvestre J.;Takamori A.;Tanner D. B.;Tariq H.;Taylor I.;Taylor R.;Taylor R.;Thorne K. A.;Thorne K. S.;Tibbits M.;Tilav S.;Tinto M.;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.;Walther H.;Ward H.;Ware B.;Watts K.;Webber D.;Weidner A.;Weiland U.;Weinstein A.;Weiss R.;Welling H.;Wen L.;Wen S.;Whelan J. T.;Whitcomb S. E.;Whiting B. F.;Wiley S.;Wilkinson C.;Willems P. A.;Williams P. R.;Williams R.;Willke B.;Wilson A.;Winjum B. J.;Winkler W.;Wise S.;Wiseman A. G.;Woan G.;Woods D.;Wooley R.;Worden J.;Wu W.;Yakushin I.;Yamamoto H.;Yoshida S.;Zaleski K. D.;Zanolin M.;Zawischa I.;Zhang L.;Zhu R.;Zotov N.;Zucker M.;Zweizig J.

2005

Abstract

We use 373 hours (≈15 days) of data from the second science run of the LIGO gravitational-wave detectors to search for signals from binary neutron star coalescences within a maximum distance of about 1.5 Mpc, a volume of space which includes the Andromeda Galaxy and other galaxies of the Local Group of galaxies. This analysis requires a signal to be found in data from detectors at the two LIGO sites, according to a set of coincidence criteria. The background (accidental coincidence rate) is determined from the data and is used to judge the significance of event candidates. No inspiral gravitational-wave events were identified in our search. Using a population model which includes the Local Group, we establish an upper limit of less than 47 inspiral events per year per Milky Way equivalent galaxy with 90% confidence for nonspinning binary neutron star systems with component masses between 1 and 3M. © 2005 The American Physical Society.

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Scheda completa

Scheda completa (DC)

	Anno
	
				2005
			
	Rivista su cui è pubblicata l'opera
	
				PHYSICAL REVIEW D, PARTICLES, FIELDS, GRAVITATION, AND COSMOLOGY
			
	Codice DOI
	
				https://dx.doi.org/10.1103/PhysRevD.72.082001
			
	Codice Scopus
	
				2-s2.0-29744435495
			
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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/11577/3578118

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