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Scientific paper
Nov 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001phdt.........8s&link_type=abstract
Thesis (PhD). CALIFORNIA INSTITUTE OF TECHNOLOGY, Source DAI-B 62/05, p. 2354, Nov 2001, 108 pages.
Other
5
Scientific paper
The science of millisecond pulsar timing can yield the most precise astrometric measurements. This thesis describes the work and results from a precision timing project aimed at monitoring the brightest millisecond pulsar, PSR J0437-4715. The project required the construction and subsequent upgrade of the Fast Pulsar Timing Machine (FPTM) at Parkes observatory, Australia. With a 256 MHz bandwidth and 4 μs time resolution; a few minutes of integration with the 64 m Parkes radio telescope yield times of arrival for PSR J0437-4715 with a precision of 100 nanoseconds. The longer term residuals (3 years) show root-mean-square deviations of 500 nanoseconds. This excess noise has been traced to inaccurate polarization calibration, and a systematic trend of ~5 μs in the times of arrival as a function of baseband frequency. Software simulation has shown the latter effect to arise from the large dynamic range in the baseband spectrum. Despite the systematic errors, the precision in our measurements of the pulsar's astrometric and binary parameters matches the best obtained so far with other millisecond pulsars. We have measured the pulsar's parallax, and the secular change in the binary's projected semi-major axis due to the system's proper motion. The latter measurement restricts the inclination angle of the binary, i < 43°. The parallax, along with the period and orbital period derivatives, enables us to constrain the distance of the pulsar, 162 < d < 205 pc. Stability analysis of the time of arrival residuals demonstrates that this pulsar matches the long term stability of the best studied millisecond pulsars, PSRs B1937+21 and B1855+09, on the time scale of the data available so far. The precision in the pulsar position matches the amplitude of the modulation of position predicted from the pulsar's binary motion. Detection of this effect will require reduction of the systematic errors and further refinements in the timing software. Along with radio interferometric observations of the pulsar and optical detection of the white-dwarf companion, the timing position will provide the best constraints for frame tie between the ecliptic and extragalactic reference frames.
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