F. Asiri
California Institute of Technology
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Physical Review D | 2004
B. Abbott; R. Abbott; R. Adhikari; A. Ageev; B. Allen; R. Amin; S. Anderson; W. G. Anderson; M. C. Araya; H. Armandula; F. Asiri; P. Aufmuth; C. Aulbert; S. Babak; R. Balasubramanian; S. Ballmer; B. Barish; D. Barker; C. Barker-Patton; M. Barnes; B. Barr; M. A. Barton; K. Bayer; R. G. Beausoleil; Krzysztof Belczynski; R. Bennett; S. J. Berukoff; J. Betzwieser; B. Bhawal; I. A. Bilenko
Data collected by the GEO600 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 pulsars gravitational wave emission. A model emission mechanism is used to interpret the limits as a constraint on the pulsars equatorial ellipticity.
