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High Precision Timing of PSR J0437–4715

Published online by Cambridge University Press:  12 April 2016

M. C. Britton ,
W. van Straten ,
M. Bailes ,
M. Toscano  and
R. N. Manchester
M. C. Britton
Affiliation:
Swinburne Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, Victoria 3122, Australia
W. van Straten
Affiliation:
Swinburne Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, Victoria 3122, Australia
M. Bailes
Affiliation:
Swinburne Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, Victoria 3122, Australia
M. Toscano
Affiliation:
Swinburne Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, Victoria 3122, Australia
R. N. Manchester
Affiliation:
Australia Telescope National Facility, CSIRO, Epping NSW 2121, Australia

Abstract

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Systematic effects currently dominate the timing residuals of the pulsar PSR J0437–4715. These systematics arise from transformations that occur during the propagation and detection of radio waves. The transformation properties of polarized radiation are related to the Lorentz group, and such effects may be represented using Lorentz transformations. These effects may be removed using the techniques of polarimetric self-calibration. Alternatively, an invariant profile may be formed from the polarimetric analogue of the Lorentz invariant I2 – Q2 – U2 – V2 and used for pulsar timing. Observations of PSR J0437–4715 are presented that show the consistency between these two techniques.

Type
Part 2. Timing, General Relativity and Astrometry
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 73 - 76
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

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