Pulsar Timing at the Very Large Array

Details Pulsar Timing at the Very Large Array Pulsar Timing at the Very Large Array

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.9913t&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #99.13; Bulletin of the American Astronomical Society, Vol. 24, p.1277

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By summing the IF signals from its 27 antennas while taking care to preserve phase coherence, the VLA can be used as the second largest ``single-dish'' telescope in the world at centimeter wavelengths. This makes it ideally suited for observations of faint radio pulsars, especially those outside the Arecibo Observatory declination limits. In August 1990, I installed pulsar timing equipment at the VLA, and, with a number of collaborators, began several projects observing newly discovered binary and millisecond pulsars. In this display, I describe the hardware, which integrates the NRAO HTRP (McKinnon, NMIMT PhD Thesis, 1992) with a Princeton Mark III timing system (Stinebring et al., Rev. Sci. Inst., 63, 3551, 1992). I discuss the performance of the equipment for very high precision millisecond pulsar timing, and describe a number of new results. Of particular interest are several binary systems, including the eclipsing binary pulsar in the globular cluster Terzan 5 (Nice and Thorsett, Ap. J., 397, 249, 1992), which is evaporating its low mass companion, and the binaries PSR B1802-07 and B2303+46, for which measurements of the relativistic advance of the angles of periastron allow the determination of the system masses (Thorsett, Arzoumanian, McKinnon, and Taylor, Ap. J. Lett., submitted). Finally, I present a status report on several other long term projects being done at the VLA, including the monitoring of the orbit of the pulsar PSR B0655+64 as a test of the stability of Newton's constant and as a limit on Brans-Dicke gravity, and the timing of a large group of fast pulsars to limit or detect very long wavelength gravitational waves of cosmological origin.

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