Upper limits on the strength of periodic gravitational waves from PSR J1939+2134

The first science run of the LIGO and GEO gravitational wave detectors presented the opportunity to test methods of searching for gravitational waves from known pulsars. Here we present new direct upper limits on the strength of waves from the pulsar PSR J1939+2134 using two independent analysis methods, one in the frequency domain using frequentist statistics and one in the time domain using Bayesian inference. Both methods show that the strain amplitude at Earth from this pulsar is less than a few times 10-22.

Upper limits on the strength of periodic gravitational waves from PSR J1939+2134

Allen B.;Woan G.;Abbott B.;Abbott R.;Adhikari R.;Allen B.;Amin R.;Anderson S. B.;Anderson W. G.;Araya M.;Armandula H.;Asiri F.;Aufmuth P.;Aulbert C.;Babak S.;Balasubramanian R.;Ballmer S.;Barish B. C.;Barker D.;Barker-Patton C.;Barnes M.;Barr B.;Barton M. A.;Bayer K.;Beausoleil R.;Belczynski K.;Bennett R.;Berukoff S. J.;Betzwieser J.;Bhawal B.;Billingsley G.;Black E.;Blackburn K.;Bland-Weaver B.;Bochner B.;Bogue L.;Bork R.;Bose S.;Brady P. R.;Brau J. E.;Brown D. A.;Brozek S.;Bullington 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.;Chen Y.;Chickarmane V.;Chin D.;Christensen N.;Churches D.;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.;Davies R.;Daw E.;de Bra D.;Delker T.;de Salvo R.;Dhurandar S.;Diaz M.;Ding H.;Drever R. W. P.;Dupuis R. J.;Ebeling C.;Edlund J.;Ehrens P.;Elliffe E. J.;Etzel T.;Evans M.;Evans T.;Fallnich C.;Farnham D.;Fejer M. M.;Fine M.;Finn L. S.;Flanagan E.;Freise A.;Frey R.;Fritschel P.;Frolov V.;Fyffe M.;Ganezer K. S.;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.;Harry G.;Hartunian A.;Heefner J.;Hefetz Y.;Heinzel G.;Heng I. S.;Hennessy M.;Hepler N.;Heptonstall A.;Heurs M.;Hewitson M.;Hindman N.;Hoang P.;Hough J.;Hrynevych M.;Hua W.;Ingley R.;Ito M.;Itoh Y.;Ivanov A.;Jennrich O.;Johnson W. W.;Johnston W.;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.;Kloevekorn P.;Koranda S.;Kotter K.;Kovalik J.;Kozak D.;Krishnan B.;Landry M.;Langdale J.;Lantz B.;Lawrence R.;Lazzarini A.;Lei M.;Leonhardt V.;Leonor I.;Libbrecht K.;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.;McNamara P.;Mendell G.;Meshkov S.;Messenger C.;Mitselmakher G.;Mittleman R.;Miyakawa O.;Miyoki S.;Mohanty S.;Moreno G.;Mossavi K.;Mours B.;Mueller G.;Mukherjee S.;Myers J.;Nagano S.;Nash T.;Naundorf H.;Nayak R.;Newton G.;Nocera F.;Nutzman P.;Olson T.;O'Reilly B.;Ottaway D. J.;Ottewill A.;Ouimette D.;Overmier H.;Owen B. J.;Papa M. A.;Parameswariah C.;Parameswariah V.;Pedraza M.;Penn S.;Pitkin M.;Plissi M.;Pratt M.;Quetschke V.;Raab F.;Radkins H.;Rahkola R.;Rakhmanov M.;Rao S. R.;Redding D.;Regehr M. W.;Regimbau T.;Reilly K. T.;Reithmaier K.;Reitze D. H.;Richman S.;Riesen R.;Riles K.;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.;Sanders G. H.;Sannibale V.;Sathyaprakash B.;Saulson P. R.;Savage R.;Sazonov A.;Schilling R.;Schlaufman K.;Schmidt V.;Schofield R.;Schrempel M.;Schutz B. F.;Schwinberg P.;Scott S. M.;Searle A. C.;Sears B.;Seel S.;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.;Skeldon K.;Smith J. R.;Smith M.;Smith M. R.;Sneddon P.;Spero R.;Stapfer G.;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.;Thorne K. S.;Tibbits M.;Tilav S.;Tinto M.;Torres C.;Torrie C.;Traeger S.;Traylor G.;Tyler W.;Ugolini D.;Vallisneri M.;van Putten M.;Vass S.;Vecchio A.;Vorvick C.;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.;Willems P. A.;Williams P. R.;Williams R.;Willke B.;Wilson A.;Winjum B. J.;Winkler W.;Wise S.;Wiseman A. G.;Wooley R.;Worden J.;Yakushin I.;Yamamoto H.;Yoshida S.;Zawischa I.;Zhang L.;Zotov N.;Zucker M.;Zweizig J.

2004

Abstract

The first science run of the LIGO and GEO gravitational wave detectors presented the opportunity to test methods of searching for gravitational waves from known pulsars. Here we present new direct upper limits on the strength of waves from the pulsar PSR J1939+2134 using two independent analysis methods, one in the frequency domain using frequentist statistics and one in the time domain using Bayesian inference. Both methods show that the strain amplitude at Earth from this pulsar is less than a few times 10-22.

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Scheda completa (DC)

	Anno
	
				2004
			
	Rivista su cui è pubblicata l'opera
	
				CLASSICAL AND QUANTUM GRAVITY
			
	Codice DOI
	
				https://dx.doi.org/10.1088/0264-9381/21/5/042
			
	Codice Scopus
	
				2-s2.0-1642377296
			
	Appare nelle tipologie:
	
				04.01 - Contributo in atti di convegno

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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11577/3578079

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