Upper limits on gravitational wave emission from 78 radio pulsars

By B. Abbott, R. Abbott, Rana X. Adhikari, J. Agresti, P. Ajith, B. Allen, R. Amin, S. Anderson, W. Anderson, M. Arain and 446 more. 2007

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We present upper limits on the gravitational wave emission from 78 radio pulsars based on data from the third and fourth science runs of the LIGO and GEO600 gravitational wave detectors. The data from both runs have been combined coherently to maximise sensitivity. For the first time pulsars within binary (or multiple) systems have been included in the search by taking into account the signal modulation due to their orbits. Our upper limits are therefore the first measured for 56 of these pulsars. For the remaining 22, our results improve on previous upper limits by up to a factor of 10. For example, our tightest upper limit on the gravitational strain is 2.6e-25 for PSRJ1603-7202, and the equatorial ellipticity of PSRJ2124-3358 is less than 10^{-6}. Furthermore, our strain upper limit for the Crab pulsar is only 2.2 times greater than the fiducial spin-down limit.

Subfields: Astronomy and Astrophysics, Geophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/57c3d377cd35d794bd053ef94e2577b69eafe704

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Citations in the corpus

Detecting gravitational wave emission from the known accreting neutron stars (2008, methodology): “Twin kHz 20 Abbott et al. (2007a) use a slightly larger uncertainty on T90 in their searches for gravitational waves from Sco X-1, to account for the time elapsed since the Steeghs & Casares (2002) measurement.”
Modelling magnetically deformed neutron stars (2007, methodology): “To see how this works out in the present case, let us consider the recent upper limits on pulsar signals from the LIGO effort (Abbott et al. 2007).”
LIGO: The laser interferometer gravitational-wave observatory (2006, methodology): “Three techniques that trade off between sensitivity and computation have been implemented: (1) semi-coherent, long duration all-sky searches sensitive only to power and neglecting phase using the entire data set [86]; (2) coherent, short-duration all-sky searches sensitive to amplitude and phase but”