An algorithm of the ensemble pulsar time based on the optimal Wiener filtration method has been constructed. This algorithm allows the separation of the contributions to the post‐fit pulsar timing residuals of the atomic clock and the pulsar itself. Filters were designed using the cross‐ and auto‐covariance functions of the timing residuals. The method has been applied to the timing data of millisecond pulsars PSR B1855+09 and B1937+21 and allowed the filtering out of the atomic‐scale component from the pulsar data. Direct comparison of the terrestrial time TT(BIPM06) and the ensemble pulsar time PTens revealed that the fractional instability of TT(BIPM06)−PTens is equal to σz= (0.8 ± 1.9) × 10−15. Based on the σz statistics of TT(BIPM06)−PTens, a new limit of the energy density of the gravitational wave background was calculated to be equal to Ωgh2∼ 3 × 10−9.
The results of a search for individual fast radio bursts with the Large Phased Array of the Lebedev Physical Institute at 111 MHz during July 2012 through August 2018 are presented. The signals were distinguished by convolving the data with a template with a fixed form, followed by convolution with test dispersion measures. Areas of sky containing the galaxies M31 and M33 were chosen for the search.Three radio bursts were detected in the vicinity of M33, five in the vicinity of M31, and one in a region offset from the center of M31 by an hour in right ascension. The dispersion measures of the detected bursts range from 203 to 1262 pc · cm −3 .
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