Limits on gravitational-wave emission from selected pulsars using LIGO data

We place direct upper limits on the amplitude of gravitational waves from 28 isolated radio pulsars by a coherent multidetector analysis of the data collected during the second science run of the LIGO interferometric detectors. These are the first direct upper limits for 26 of the 28 pulsars. We use coordinated radio observations for the first time to build radio-guided phase templates for the expected gravitational-wave signals. The unprecedented sensitivity of the detectors allows us to set strain upper limits as low as a few times 10-24. These strain limits translate into limits on the equatorial ellipticities of the pulsars, which are smaller than 10-5 for the four closest pulsars. © 2005 The American Physical Society.

Limits on gravitational-wave emission from selected pulsars using LIGO data

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.;Di Credico A.;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.;Keils 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.;Maclnnis 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.;Oreilly B.;Ottaway D. J.;Ottewill A.;Ouimette D.;Overmier H.;Owen B. J.;Pan Y.;Papa M. A.;Parameshwaraiah V.;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.;Schofleld 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.;Suites 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.;Wooley R.;Worden J.;Wu W.;Yakushin;Yamamoto H.;Yoshida S.;Zaleski K. D.;Zanolin M.;Zawischa I.;Zhang L.;Zhu R.;Zotov N.;Zucker M.;Zweizig J.;Kramer M.;Lyne A. G.

2005

Abstract

We place direct upper limits on the amplitude of gravitational waves from 28 isolated radio pulsars by a coherent multidetector analysis of the data collected during the second science run of the LIGO interferometric detectors. These are the first direct upper limits for 26 of the 28 pulsars. We use coordinated radio observations for the first time to build radio-guided phase templates for the expected gravitational-wave signals. The unprecedented sensitivity of the detectors allows us to set strain upper limits as low as a few times 10-24. These strain limits translate into limits on the equatorial ellipticities of the pulsars, which are smaller than 10-5 for the four closest pulsars. © 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.94.181103
			
	Codice Scopus
	
				2-s2.0-76249123224
			
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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/11577/3578239

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