Pulsar timing sensitivity to very-low-frequency gravitational waves

Pulsar timing sensitivity to very-low-frequency gravitational waves,10.1103/PHYSREVD.83.081301,Physical Review D,Fredrick A. Jenet,J. W. Armstrong,Mas

Pulsar timing sensitivity to very-low-frequency gravitational waves   (Citations: 2)
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We compute the sensitivity, constrained by instrumental, propagation, and other fundamental noises, of pulsar timing to very-low-frequency gravitational waves (GWs). Reaching predicted GW signal strengths will require suppression of time-of-arrival fluctuations caused by interstellar plasma turbulence and a reduction of white rms timing noise to < or approx. 100 ns. Assuming negligible intrinsic pulsar rotational noise, perfect time transfer from time standard to observatory, and stable pulse profiles, the resulting single-pulsar signal-to-noise ratio=1 sensitivity is limited by terrestrial time standards at h{sub rms}2x10¹ [f/ (1 cycle/year)]-1/2 for f<3x10 Hz, where f is the Fourier frequency and a bandwidth of 1 cycle/(10 years) is assumed. Since this sensitivity is comparable to predicted GW signal levels, a reliable detection will require substantial signal-to-noise ratio improvement via pulsar timing array.
Journal: Physical Review D - PHYS REV D , vol. 83, no. 8, pp. 081301-081301, 2011
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