Setting upper limits on the strength of periodic gravitational waves from PSR J1939+2134 using the first science data from the GEO 600 and LIGO detectors
B. Abbott
,
R. Abbott
,
R. Adhikari
,
A. Ageev
,
B. Allen
,
R. Amin
,
S. B. Anderson
,
W. G. Anderson
,
M. Araya
,
H. Armandula
,
F. Asiri
,
P. Aufmuth
,
C. Aulbert
,
S. Babak
,
R. Balasubramanian
,
S. Ballmer
,
B. C. Barish
,
D. Barker
,
C. Barker-Patton
,
M. Barnes
,
B. Barr
,
M. A. Barton
,
K. Bayer
,
R. Beausoleil
,
K. Belczynski
,
R. Bennett
,
S. J. Berukoff
,
J. Betzwieser
,
B. Bhawal
,
I. A. Bilenko
,
G. Billingsley
,
E. Black
,
K. Blackburn
,
B. Bland-Weaver
,
B. Bochner
,
L. Bogue
,
R. Bork
,
S. Bose
,
P. R. Brady
,
V. B. Braginsky
,
J. E. Brau
,
D. A. Brown
,
S. Brozek
,
A. Bullington
,
A. Buonanno
(1)
,
R. Burgess
,
D. Busby
,
W. E. Butler
,
R. L. Byer
,
L. Cadonati
,
G. Cagnoli
,
J. B. Camp
,
C. A. Cantley
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L. Cardenas
,
K. Carter
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M. M. Casey
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J. Castiglione
,
A. Chandler
,
J. Chapsky
,
P. Charlton
,
S. Chatterji
,
Y. Chen
,
V. Chickarmane
,
D. Chin
,
N. Christensen
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D. Churches
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C. Colacino
,
R. Coldwell
,
M. Coles
,
D. Cook
,
T. Corbitt
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D. Coyne
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J. D. Creighton
,
T. D. Creighton
,
D. R. Crooks
,
P. Csatorday
,
B. J. Cusack
,
C. Cutler
,
E. d'Ambrosio
,
K. Danzmann
,
R. Davies
,
E. Daw
,
D. Debra
,
T. Delker
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R. Desalvo
,
S. Dhurandhar
,
M. Díaz
,
H. Ding
,
R. W. Drever
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R. J. Dupuis
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C. Ebeling
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J. Edlund
,
P. Ehrens
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E. J. Elliffe
,
T. Etzel
,
M. Evans
,
T. Evans
,
C. Fallnich
,
D. Farnham
,
M. M. Fejer
,
M. Fine
,
L. S. Finn
,
É. Flanagan
,
A. Freise
,
R. Frey
,
P. Fritschel
,
V. Frolov
,
M. Fyffe
,
K. S. Ganezer
,
J. A. Giaime
,
A. Gillespie
,
K. Goda
,
G. González
,
S. Goßler
,
P. Grandclément
,
A. Grant
,
C. Gray
,
A. M. Gretarsson
,
D. Grimmett
,
H. Grote
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S. Grunewald
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M. Guenther
,
E. Gustafson
,
R. Gustafson
,
W. O. Hamilton
,
M. Hammond
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J. Hanson
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C. Hardham
,
G. Harry
,
A. Hartunian
,
J. Heefner
,
Y. Hefetz
,
G. Heinzel
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I. S. Heng
,
M. Hennessy
,
N. Hepler
,
A. Heptonstall
,
M. Heurs
,
M. Hewitson
,
N. Hindman
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P. Hoang
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J. Hough
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M. Hrynevych
,
W. Hua
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R. Ingley
,
M. Ito
,
Y. Itoh
,
A. Ivanov
,
O. Jennrich
,
W. W. Johnson
,
W. Johnston
,
L. Jones
,
D. Jungwirth
,
V. Kalogera
,
E. Katsavounidis
,
K. Kawabe
,
S. Kawamura
,
W. Kells
,
J. Kern
,
A. Khan
,
S. Killbourn
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C. J. Killow
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C. Kim
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C. King
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P. King
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S. Klimenko
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P. Kloevekorn
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S. Koranda
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K. Kötter
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J. Kovalik
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D. Kozak
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B. Krishnan
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M. Landry
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J. Langdale
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B. Lantz
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R. Lawrence
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A. Lazzarini
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M. Lei
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V. Leonhardt
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I. Leonor
,
K. Libbrecht
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P. Lindquist
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S. Liu
,
J. Logan
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M. Lormand
,
M. Lubiński
,
H. Lück
,
T. T. Lyons
,
B. Machenschalk
,
M. Macinnis
,
M. Mageswaran
,
K. Mailand
,
W. Majid
,
M. Malec
,
F. Mann
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A. Marin
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S. Márka
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E. Maros
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J. Mason
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K. Mason
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O. Matherny
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L. Matone
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N. Mavalvala
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R. Mccarthy
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D. E. Mcclelland
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M. Mchugh
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P. Mcnamara
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G. Mendell
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C. Messenger
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V. P. Mitrofanov
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G. Mitselmakher
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O. Miyakawa
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S. Mohanty
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G. Moreno
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K. Mossavi
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B. Mours
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G. Mueller
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S. Mukherjee
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J. Myers
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S. Nagano
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T. Nash
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H. Naundorf
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R. Nayak
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G. Newton
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F. Nocera
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P. Nutzman
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T. Olson
,
B. O'Reilly
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D. J. Ottaway
,
A. Ottewill
,
D. Ouimette
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H. Overmier
,
B. J. Owen
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M. A. Papa
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C. Parameswariah
,
V. Parameswariah
,
M. Pedraza
,
S. Penn
,
M. Pitkin
,
M. Plissi
,
M. Pratt
,
V. Quetschke
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F. Raab
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H. Radkins
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R. Rahkola
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M. Rakhmanov
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S. R. Rao
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D. Redding
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M. W. Regehr
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T. Regimbau
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K. T. Reilly
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K. Reithmaier
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D. H. Reitze
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S. Richman
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R. Riesen
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K. Riles
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A. Rizzi
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D. I. Robertson
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N. A. Robertson
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L. Robison
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S. Roddy
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J. Rollins
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J. D. Romano
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J. Romie
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H. Rong
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D. Rose
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E. Rotthoff
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S. Rowan
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A. Rüdiger
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P. Russell
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K. Ryan
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I. Salzman
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G. H. Sanders
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V. Sannibale
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B. Sathyaprakash
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P. R. Saulson
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R. Savage
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A. Sazonov
,
R. Schilling
,
K. Schlaufman
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V. Schmidt
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R. Schofield
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M. Schrempel
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B. F. Schutz
,
P. Schwinberg
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S. M. Scott
,
A. C. Searle
,
B. Sears
,
S. Seel
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A. S. Sengupta
,
C. A. Shapiro
,
P. Shawhan
,
D. H. Shoemaker
,
Q. Z. Shu
,
A. Sibley
,
X. Siemens
,
L. Sievers
,
D. Sigg
,
A. M. Sintes
,
K. Skeldon
,
J. R. Smith
,
M. Smith
,
M. R. Smith
,
P. Sneddon
,
R. Spero
,
G. Stapfer
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K. A. Strain
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D. Strom
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A. Stuver
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T. Summerscales
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M. C. Sumner
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P. J. Sutton
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J. Sylvestre
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A. Takamori
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D. B. Tanner
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H. Tariq
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I. Taylor
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R. Taylor
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K. S. Thorne
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M. Tibbits
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S. Tilav
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M. Tinto
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K. V. Tokmakov
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C. Torres
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C. Torrie
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S. Traeger
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G. Traylor
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W. Tyler
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D. Ugolini
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M. Vallisneri
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M. van Putten
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S. Vass
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A. Vecchio
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C. Vorvick
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S. P. Vyachanin
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L. Wallace
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H. Walther
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H. Ward
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B. Ware
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K. Watts
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D. Webber
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A. Weidner
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U. Weiland
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A. Weinstein
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R. Weiss
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H. Welling
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L. Wen
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S. Wen
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J. T. Whelan
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S. E. Whitcomb
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B. F. Whiting
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P. A. Willems
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P. R. Williams
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R. Williams
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B. Willke
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A. Wilson
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B. J. Winjum
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W. Winkler
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S. Wise
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A. G. Wiseman
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G. Woan
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R. Wooley
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H. Yamamoto
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S. Yoshida
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I. Zawischa
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L. Zhang
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N. Zotov
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M. Zucker
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J. Zweizig
B. Abbott
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R. Abbott
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R. Adhikari
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A. Ageev
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B. Allen
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R. Amin
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S. B. Anderson
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W. G. Anderson
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M. Araya
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H. Armandula
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F. Asiri
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P. Aufmuth
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C. Aulbert
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S. Babak
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M. Barnes
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B. Barr
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M. A. Barton
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K. Bayer
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R. Beausoleil
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K. Belczynski
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R. Bennett
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S. J. Berukoff
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J. Betzwieser
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B. Bhawal
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I. A. Bilenko
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G. Billingsley
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E. Black
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K. Blackburn
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B. Bland-Weaver
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B. Bochner
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L. Bogue
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R. Bork
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M. Smith
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M. R. Smith
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R. Spero
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A. Stuver
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- Function : Author
A. Wilson
- Function : Author
B. J. Winjum
- Function : Author
W. Winkler
- Function : Author
S. Wise
- Function : Author
A. G. Wiseman
- Function : Author
G. Woan
- Function : Author
R. Wooley
- Function : Author
J. Worden
- Function : Author
I. Yakushin
- Function : Author
H. Yamamoto
- Function : Author
S. Yoshida
- Function : Author
I. Zawischa
- Function : Author
L. Zhang
- Function : Author
N. Zotov
- Function : Author
M. Zucker
- Function : Author
J. Zweizig
- Function : Author
Abstract
Data collected by the GEO 600 and LIGO interferometric gravitational wave detectors during their first observational science run were searched for continuous gravitational waves from the pulsar J1939+2134 at twice its rotation frequency. Two independent analysis methods were used and are demonstrated in this paper: a frequency domain method and a time domain method. Both achieve consistent null results, placing new upper limits on the strength of the pulsar’s gravitational wave emission. A model emission mechanism is used to interpret the limits as a constraint on the pulsar’s equatorial ellipticity.
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