2025/08/12 by S. A. Andrianov, Andrianov, S. A., V. A. Potapov +3
Earth and Planetary Sciences · Physics and Astronomy · #Advanced Frequency and Time Standards #FOS: Physical sciences #Geophysics and Gravity Measurements #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research
paper · pdf · doi:10.48550/arxiv.2508.08711
openalex publication_date 2025/08/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We have performed timing of a number of known slow pulsars with poorly known coordinates and parameters of their intrinsic rotation. We used data from the archive of round-the-clock monitoring observations on the third (stationary) beam pattern of the Large Phased Array radio telescope (LPA LPI) at a frequency of 111 MHz, which has an unsatisfactory connection of the local quartz time standards to the reference scale (UTC). To compensate for the resulting errors, we applied an algorithm previously developed by us, which uses Pulsar Timescale as an intermediate reference scale to compute corrections to the pulses Times of Arrival (TOAs) measured by the local clocks and to switch to UTC. Analyzing a ten-year observational data set we substantially refined the rotational and astrometric parameters of 12 pulsars. The spin frequencies ν and their first derivatives ν were determined with accuracies of 10-10 Hz and 10-19 s-2, respectively, which is 5-6 orders of magnitude better than the values quoted in the catalogue. The coordinates are determined with accuracies ranging from units to tens of arcseconds.