4.7 Article

Applying clock comparison methods to pulsar timing observations

期刊

出版社

OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab742

关键词

gravitational waves; methods: data analysis; pulsars: general

资金

  1. French Agence Nationale de la Recherche (ANR) Programme d'Investissement d'Avenir (PIA) under the FIRST-TF network [ANR-10-LABX-48-01]
  2. Oscillator IMP project [ANR-11-EQPX-0033-OSC-IMP]
  3. EUR EIPHI Graduate School [ANR-17-EURE-00002]
  4. Region Bourgogne Franche Comte
  5. 'Programme National de Cosmologie and Galaxies' (PNCG)
  6. 'Programme NationalHautes Energies' (PNHE) - CNRS/INSUIN2P3-INP, France
  7. 'Programme NationalHautes Energies' (PNHE) - CEA, France
  8. 'Programme NationalHautes Energies' (PNHE) - CNES, France

向作者/读者索取更多资源

Frequency metrology in pulsar research plays a crucial role in understanding cosmological phenomena. Precise measurement of pulsar time of arrival is vital for expanding our knowledge of the universe. This article focuses on the application of modern statistical methods in analyzing pulsar data to detect correlated red noise signals.
Frequency metrology outperforms any other branch of metrology in accuracy (parts in 10(-16)) and small fluctuations (<10(-17)). In turn, among celestial bodies, the rotation speed of millisecond pulsars is by far the most stable (<10(-18)). Therefore, the precise measurement of the time of arrival (TOA) of pulsar signals is expected to disclose information about cosmological phenomena, and to enlarge our astrophysical knowledge. Related to this topic, Pulsar Timing Array projects have been developed and operated for the last decades. The TOAs from a pulsar can be affected by local emission and environmental effects, in the direction of the propagation through the interstellar medium or universally by gravitational waves from super massive black hole binaries. These effects (signals) can manifest as a low-frequency fluctuation over time, phenomenologically similar to a red noise, while the remaining pulsar intrinsic and instrumental background (noise) are white. This article focuses on the frequency metrology of pulsars. From our standpoint, the pulsar is an accurate clock, to be measured simultaneously with several telescopes in order to reject the uncorrelated white noise. We apply the modern statistical methods of time-and-frequency metrology to simulated pulsar data, and we show the detection limit of the correlated red noise signal between telescopes.

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