Beating the spin-down limit on gravitational wave emission from the Crab pulsar

We present direct upper limits on gravitational wave emission from the Crab pulsar using data from the first 9 months of the fifth science run of the Laser Interferometer Gravitational-wave Observatory (LIGO). These limits are based on two searches. In the first we assume that the gravitational wave emission follows the observed radio timing, giving an upper limit on gravitational wave emission that beats indirect limits inferred from the spin-down and braking index of the pulsar and the energetics of the nebula. In the second we allow for a small mismatch between the gravitational and radio signal frequencies and interpret our results in the context of two possible gravitational wave emission mechanisms. © 2008. The American Astronomical Society.

Beating the spin-down limit on gravitational wave emission from the Crab pulsar

Abbott B.;Abbott R.;Adhikari R.;Ajith P.;Allen B.;Allen G.;Amin R.;Anderson S. B.;Anderson W. G.;Arain M. A.;Araya M.;Armandula H.;Armor P.;Aso Y.;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.;Bastarrika M.;Bayer K.;Betzwieser J.;Beyersdorf P. T.;Bilenko I. A.;Billingsley G.;Biswas R.;Black E.;Blackburn K.;Blackburn L.;Blair D.;Bland B.;Bodiya T. P.;Bogue L.;Bork R.;Boschi V.;Bose S.;Brady P. R.;Braginsky V. B.;Brau J. E.;Brinkmann M.;Brooks A.;Brown D. A.;Brunet G.;Bullington A.;Buonanno A.;Burmeister O.;Byer R. L.;Cadonati L.;Cagnoli G.;Camp J. B.;Cannizzo J.;Cannon K.;Cao J.;Cardenas L.;Casebolt T.;Castaldi G.;Cepeda C.;Chalkley E.;Charlton P.;Chatterji S.;Chelkowski S.;Chen Y.;Christensen N.;Clark D.;Clark J.;Cokelaer T.;Conte R.;Cook D.;Corbitt T.;Coyne D.;Creighton J. D. E.;Cumming A.;Cunningham L.;Cutler R. M.;Dalrymple J.;Danzmann K.;Davies G.;Debra D.;Degallaix J.;Degree M.;Dergachev V.;Desai S.;Desalvo R.;Dhurandhar S.;Diaz M.;Dickson J.;Dietz A.;Donovan F.;Dooley K. L.;Doomes E. E.;Ver R. W. P. D.;Duke I.;Dumas J. -C.;Dupuis R. J.;Dwyer J. G.;Echols C.;Effler A.;Ehrens P.;Espinoza E.;Etzel T.;Evans T.;Fairhurst S.;Fan Y.;Fazi D.;Fehrmann H.;Fejer M. M.;Finn L. S.;Flasch K.;Fotopoulos N.;Freise A.;Frey R.;Fricke T.;Fritschel P.;Frolov V. V.;Fyffe M.;Garofoli J.;Gholami I.;Giaime J. A.;Giampanis S.;Giardina K. D.;Goda K.;Goetz E.;Goggin L.;Gonzalez G.;Gossler S.;Gouaty R.;Grant A.;Gras S.;Gray C.;Gray M.;Greenhalgh R. J. S.;Gretarsson A. M.;Grimaldi F.;Grosso R.;Grote H.;Grunewald S.;Guenther M.;Gustafson E. K.;Gustafson R.;Hage B.;Hallam J. M.;Hammer D.;Hanna C.;Hanson J.;Harms J.;Harry G.;Harstad E.;Hayama K.;Hayler T.;Heefner J.;Heng I. S.;Hennessy M.;Heptonstall A.;Hewitson M.;Hild S.;Hirose E.;Hoak D.;Hosken D.;Hough J.;Huttner S. H.;Ingram D.;Ito M.;Ivanov A.;Johnson B.;Johnson W. W.;Jones D. I.;Jones G.;Jones R.;Ju L.;Kalmus P.;Kalogera V.;Kamat S.;Kanner J.;Kasprzyk D.;Katsavounidis E.;Kawabe K.;Kawamura S.;Kawazoe F.;Kells W.;Keppel D. G.;Khalili F. Y.;Khan R.;Khazanov E.;Kim C.;King P.;Kissel J. S.;Klimenko S.;Kokeyama K.;Kondrashov V.;Kopparapu R. K.;Kozak D.;Kozhevatov I.;Krishnan B.;Kwee P.;Lam P. K.;Landry M.;Lang M. M.;Lantz B.;Lazzarini A.;Lei M.;Leindecker N.;Leonhardt V.;Leonor I.;Libbrecht K.;Lin H.;Lindquist P.;Lockerbie N. A.;Lodhia D.;Lormand M.;Lu P.;Lubinski M.;Lucianetti A.;Luck H.;Machenschalk B.;Macinnis M.;Mageswaran M.;Mailand K.;Mandic V.;Marka S.;Marka Z.;Markosyan A.;Markowitz J.;Maros E.;Martin I.;Martin R. M.;Marx J. N.;Mason K.;Matichard F.;Matone L.;Matzner R.;Mavalvala N.;Mccarthy R.;Mcclelland D. E.;Mcguire S. C.;Mchugh M.;Mcintyre G.;Mcivor G.;Mckechan D.;Mckenzie K.;Meier T.;Melissinos A.;Mendell G.;Mercer R. A.;Meshkov S.;Messenger C. J.;Meyers D.;Miller J.;Minelli J.;Mitra S.;Mitrofanov V. P.;Mitselmakher G.;Mittleman R.;Miyakawa O.;Moe B.;Mohanty S.;Moreno G.;Mossavi K.;Mowlowry C.;Mueller G.;Mukherjee S.;Mukhopadhyay H.;Muller-Ebhardt H.;Munch J.;Murray P.;Myers E.;Myers J.;Nash T.;Nelson J.;Newton G.;Nishizawa A.;Numata K.;O'dell J.;Ogin G.;O'reilly B.;O'shaughnessy R.;Ottaway D. J.;Ottens R. S.;Overmier H.;Owen B. J.;Pan Y.;Pankow C.;Papa M. A.;Parameshwaraiah V.;Patel P.;Pedraza M.;Penn S.;Perreca A.;Petrie T.;Pinto I. M.;Pitkin M.;Pletsch H. J.;Plissi M. V.;Postiglione F.;Principe M.;Prix R.;Quetschke V.;Raab F.;Rabeling D. S.;Radkins H.;Rainer N.;Rakhmanov M.;Ramsunder M.;Rehbein H.;Reid S.;Reitze D. H.;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.;De La Jordana L. S.;Sandberg V.;Sannibale V.;Saraf S.;Sarin P.;Sathyaprakash B. S.;Sato S.;Saulson P. R.;Savage R.;Savov P.;Schediwy S. W.;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.;Siemens X.;Sigg D.;Sinha S.;Sintes A. M.;Slagmolen B. J. J.;Slutsky J.;Smith J. R.;Smith M. R.;Smith N. D.;Somiya K.;Sorazu B.;Stein L. C.;Stochino A.;Stone R.;Strain K. A.;Strom D. M.;Stuver A.;Summerscales T. Z.;Sun K. -X.;Sung M.;Sutton P. J.;Takahashi H.;Tanner D. B.;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.;Ulmen J.;Urbanek K.;Vahlbruch H.;Van Broeck C. D.;Van Sluys M. D.;Vass S.;Vaulin R.;Vecchio A.;Veitch J.;Veitch P.;Villar A.;Vorvick C.;Vyachanin S. P.;Waldman S. J.;Wallace L.;Ward H.;Ward R.;Weinert M.;Weinstein A.;Weiss R.;Wen S.;Wette K.;Whelan J. T.;Whitcomb S. E.;Whiting B. F.;Wilkinson C.;Willems P. A.;Williams H. R.;Williams L.;Willke B.;Wilmut I.;Winkler W.;Wipf C. C.;Wiseman A. G.;Woan G.;Wooley R.;Worden J.;Wu W.;Yakushin I.;Yamamoto H.;Yan Z.;Yoshida S.;Zanolin M.;Zhang J.;Zhang L.;Zhao C.;Zotov N.;Zucker M.;Zweizig J.;Santostasi G.

2008

Abstract

We present direct upper limits on gravitational wave emission from the Crab pulsar using data from the first 9 months of the fifth science run of the Laser Interferometer Gravitational-wave Observatory (LIGO). These limits are based on two searches. In the first we assume that the gravitational wave emission follows the observed radio timing, giving an upper limit on gravitational wave emission that beats indirect limits inferred from the spin-down and braking index of the pulsar and the energetics of the nebula. In the second we allow for a small mismatch between the gravitational and radio signal frequencies and interpret our results in the context of two possible gravitational wave emission mechanisms. © 2008. The American Astronomical Society.

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	Anno
	
				2008
			
	Rivista su cui è pubblicata l'opera
	
				THE ASTROPHYSICAL JOURNAL
			
	Codice DOI
	
				https://dx.doi.org/10.1086/591526
			
	Codice Scopus
	
				2-s2.0-53349144479
			
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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/11577/3578224

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