Abstract <p>A method for pulsar timing based on monitoring data from the 3-th beam of the Large Phase Array (LPA LPI) radio telescope is proposed. In our observations, recorders with quartz clock generators were used as local clocks. Such recorders initially had an accuracy and hardware reference to the UTC time scale insufficient for pulsar timing. We have developed a method for referencing such clocks to the UTC based on observations of known pulsars used as intermediate reference clocks. This allowed us to improve dramatically the accuracy of determining the Time of Arrivals (TOAs) of pulsars’ pulses. We applied this method to the results of our observations of 24 second period pulsars over a time interval of 10 years. It was shown that the accuracy of the pulsar period, its first derivative (<InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(P\)</EquationSource>  </InlineEquation> and <InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(\dot {P}\)</EquationSource>  </InlineEquation>) and their coordinates in right ascension and declination (<InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(\alpha \)</EquationSource>  </InlineEquation>, <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(\delta \)</EquationSource>  </InlineEquation>) allow us to predict the pulsar phase within <InlineEquation ID="IEq5"> <EquationSource Format="TEX">\( \pm 0.5{\kern 1pt} P\)</EquationSource>  </InlineEquation> during several years. The accuracy of determining the coordinates by right ascension and declination was typically better than <InlineEquation ID="IEq6"> <EquationSource Format="TEX">\(10'' \)</EquationSource>  </InlineEquation> with an angular resolution of the radio telescope of about <InlineEquation ID="IEq7"> <EquationSource Format="TEX">\(30' \)</EquationSource>  </InlineEquation>. That makes it possible to use these parameters for timing using radio telescopes with narrow beam patterns. The accuracy of the calculated period was typically better than <InlineEquation ID="IEq8"> <EquationSource Format="TEX">\({{10}^{{ - 8}}}\)</EquationSource>  </InlineEquation> s.</p>

The Pushchino Multibeam Pulsar Search. VI. Method for Pulsar Timing Using Poorly Timed Data

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发表日期：

2025年11月1日

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S. A. Andrianov,
V. A. Potapov,
S. A. Tyul’bashev,
S. V. Logvinenko,
V. V. Oreshko

摘要

Abstract

A method for pulsar timing based on monitoring data from the 3-th beam of the Large Phase Array (LPA LPI) radio telescope is proposed. In our observations, recorders with quartz clock generators were used as local clocks. Such recorders initially had an accuracy and hardware reference to the UTC time scale insufficient for pulsar timing. We have developed a method for referencing such clocks to the UTC based on observations of known pulsars used as intermediate reference clocks. This allowed us to improve dramatically the accuracy of determining the Time of Arrivals (TOAs) of pulsars’ pulses. We applied this method to the results of our observations of 24 second period pulsars over a time interval of 10 years. It was shown that the accuracy of the pulsar period, its first derivative ( \(P\) and \(\dot {P}\) ) and their coordinates in right ascension and declination ( \(\alpha \) , \(\delta \) ) allow us to predict the pulsar phase within \( \pm 0.5{\kern 1pt} P\) during several years. The accuracy of determining the coordinates by right ascension and declination was typically better than \(10'' \) with an angular resolution of the radio telescope of about \(30' \) . That makes it possible to use these parameters for timing using radio telescopes with narrow beam patterns. The accuracy of the calculated period was typically better than \({{10}^{{ - 8}}}\) s.