The application of co-integration theory in ensemble pulsar timescale algorithm

Abstract

Employing multiple pulsars and using an appropriate algorithm to establish ensemble pulsar timescale can reduce the influences of various noises on the long-term stability of pulsar timescale, compared to a single pulsar. However, due to the low timing precision and the significant red noises of some pulsars, their participation in the construction of ensemble pulsar timescale is often limited. Inspired by the principle of solving non-stationary sequence modeling using co-integration theory, we puts forward an algorithm based on the co-integration theory to establish ensemble pulsar timescale. It is found that this algorithm can effectively suppress some noise sources if a co-integration relationship between different pulsar data exist. Different from the classical weighted average algorithm, the co-integration method provides the chances of the pulsar with significant red noises to attend the establishment of ensemble pulsar timescale. Based on the data from the North American Nanohertz Observatory for Gravitational Waves, we found that the co-integration algorithm can successfully reduce several timing noises and improve the long-term stability of the ensemble pulsar timescale.

References in corpus (11)

• The Confrontation between General Relativity and Experiment
• PSRCHIVE and PSRFITS An Open Approach to Radio Pulsar Data Storage and Analysis
• The NANOGrav Nine-year Data Set: Observations, Arrival Time Measurements, and Analysis of 37 Millisecond Pulsars
• Timing stability of millisecond pulsars and prospects for gravitational-wave detection
• Development of a pulsar-based timescale
• Pulsar timing analysis in the presence of correlated noise
• Testing Theories of Gravitation Using 21-Year Timing of Pulsar Binary J1713+0747
• Elementary Wideband Timing of Radio Pulsars
• The NANOGrav Nine-Year Data Set: Excess Noise in Millisecond Pulsar Arrival Times
• NANOGrav Constraints on Gravitational Wave Bursts with Memory
• The optimal filters for the construction of the ensemble pulsar time