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Lentati, L; Taylor, S. R; Mingarelli, C. M. F; Sesana, A; Sanidas, S. A; Vecchio, A; Caballero, R. N; Lee, K. J; van Haasteren, R; Babak, S; Bassa, C. G; Brem, P; Burgay, M; Champion, D. J; Cognard, I; Desvignes, G; Gair, J. R; Guillemot, L; Hessels, J. W. T; Janssen, G. H; Karuppusamy, R; Kramer, M; Lassus, A; Lazarus, P; Liu, K; Osłowski, S; Perrodin, D; Petiteau, A; Possenti, A; Purver, M. B; Rosado, P. A; Smits, R; Stappers, B; Theureau, G; Tiburzi, C; Verbiest, J. P. W
Monthly notices of the Royal Astronomical Society, 11/2015, Letnik: 453, Številka: 3Journal Article
We present new limits on an isotropic stochastic gravitational-wave background (GWB) using a six pulsar data set spanning 18 yr of observations from the 2015 European Pulsar Timing Array data release. Performing a Bayesian analysis, we fit simultaneously for the intrinsic noise parameters for each pulsar, along with common correlated signals including clock, and Solar system ephemeris errors, obtaining a robust 95 per cent upper limit on the dimensionless strain amplitude A of the background of A < 3.0 × 10−15 at a reference frequency of 1 yr−1 and a spectral index of 13/3, corresponding to a background from inspiralling supermassive black hole binaries, constraining the GW energy density to Ωgw(f)h 2 < 1.1 × 10−9 at 2.8 nHz. We also present limits on the correlated power spectrum at a series of discrete frequencies, and show that our sensitivity to a fiducial isotropic GWB is highest at a frequency of ∼5 × 10−9 Hz. Finally, we discuss the implications of our analysis for the astrophysics of supermassive black hole binaries, and present 95 per cent upper limits on the string tension, Gμ/c 2, characterizing a background produced by a cosmic string network for a set of possible scenarios, and for a stochastic relic GWB. For a Nambu–Goto field theory cosmic string network, we set a limit Gμ/c 2 < 1.3 × 10−7, identical to that set by the Planck Collaboration, when combining Planck and high-ℓ cosmic microwave background data from other experiments. For a stochastic relic background, we set a limit of $\Omega ^\mathrm{relic}_\mathrm{gw}(f)h^2<1.2 \times 10^{-9}$ , a factor of 9 improvement over the most stringent limits previously set by a pulsar timing array.
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