Characterizing the Radio Frequency Timing Stability of Fast and Millisecond Pulsars

Details Characterizing the Radio Frequency Timing Stability of Fast and Millisecond Pulsars Characterizing the Radio Frequency Timing Stability of Fast and Millisecond Pulsars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21713907k&link_type=abstract

American Astronomical Society, AAS Meeting #217, #139.07; Bulletin of the American Astronomical Society, Vol. 43, 2011

Statistics

Methodology

Scientific paper

We propose measuring the average profile stabilization rate in millisecond pulsars. We consider the correlations between a pulsar's global average profile and subaverage profiles constructed using increasing numbers of pulses, thereby quantifying the number of pulses required to build a stable average profile. We adopt the methodology developed by Helfand, Manchester, and Taylor (Ap. J., 1975) and later employed by Rathnasree & Rankin (Ap. J., 1995) to calculate the stabilization rates of a sample of both fast and millisecond pulsars. A correlation coefficient is obtained by averaging the correlation coefficients of the global average profile with each subaverage profile of n pulses. By plotting how the correlation coefficient increases with n one can observe how the star's profile stabilizes as the number of pulses used to construct it increases. We look for values of n for which the correlation coefficient is statistically significant and interpret this value as the number of pulses required to compute a stable average profile of a given star. We expect n to be smaller for millisecond pulsars, as they typically exhibit very few intrinsic variations. This work considers the stars studied by Rathnasree & Rankin, as well as millisecond pulsars that are of interest to the pulsar timing community and in particular the NANOGrav (North American Nanohertz Observatory for Gravitational Waves) initiative. The authors would like to acknowledge support from the US National Science Foundation.

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