Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...2e...6r&link_type=abstract
On the Present and Future of Pulsar Astronomy, 26th meeting of the IAU, Joint Discussion 2, 16-17 August, 2006, Prague, Czech Re
Astronomy and Astrophysics
Astronomy
Scientific paper
Purpose of this work is to construct an algorithm of a new astronomical time scale based on the rotation of pulsars, which has comparable accuracy with the most precise terrestrial time scale TT. This algorithm is based on the Wiener optimal filtering method and allows separating contributions to the post-fit pulsar timing residuals of the atomic clock used in pulsar timing and spin variations of pulsar itself. The optimal filters are constructed with use of the cross and auto covariance functions (in time domain) or auto and cross power spectra (in frequency domain) of the post-fit timing residuals of pulsars participating in construction of the ensemble time scale.. The algorithm is applied to the timing data of millisecond pulsars PSR B1855+09 and B1937+21 (Kaspi et al. 1994) and allowed to obtain the corrections of UTC scale relative to ensemble pulsar time scale PT[ens]. Comparison of the differences UTC - PT[ens] and UTC - TT displays significant correlation between them at level 0.79. Subsequent analysis of TT - PT[ens] shows that TT coincides with PT[ens] within 0.40+/-0.17 mcs and has fractional stability 10^-15 at 7 years time interval. Relatively close angular distance (15.5 degrees) on the sky between these pulsars gives grounds to expect that there is a correlated signal in the post-fit timing data caused by the stochastic gravitational wave background (GWB). A new limit of the fractional energy density of GWB based on the difference TT - PT[ens] were established to be Omega_g h^2 ~ 2*10^-10. This new value is by one order lower than previously published one owing to application of the new algorithm that separates the proper pulsars spin and local atomic standard variations.
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