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Analysis of PSR 1641–45 Using Specialized Capabilities of the S2 VLBI Correlator

Published online by Cambridge University Press:  12 April 2016

D.A. Del Rizzo
Affiliation:
University of Calgary/Dominion Radio Astrophysical Observatory, NRC, Box 248, Penticton, B.C.CanadaV2A 6K3
B.R. Carlson
Affiliation:
University of Calgary/Dominion Radio Astrophysical Observatory, NRC, Box 248, Penticton, B.C.CanadaV2A 6K3
W.T. Petrachenko
Affiliation:
NRCan c/o DRAO, NRC, Box 248, Penticton, B.C.CanadaV2A 6K3
J. E. Everett
Affiliation:
University of Calgary/Dominion Radio Astrophysical Observatory, NRC, Box 248, Penticton, B.C.CanadaV2A 6K3
J. M. Cordes
Affiliation:
NRCan c/o DRAO, NRC, Box 248, Penticton, B.C.CanadaV2A 6K3

Abstract

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The pulsar PSR 1641-45 was observed using the S2 VLBI Recording System at 1.6 GHz with radio telescopes at Tidbinbilla and Narrabri in Australia, and at Hartebeesthoek in South Africa. The data were correlated with the Canadian S2 VLBI Correlator using the ‘fast-dumping’ mode in conjunction with two independent pulsar gates. The high time and spectral resolution capabilities of this correlator permit a detailed examination of dispersion and dispersion-removal effects on individual pulses, and a comparison of these effects from pulse to pulse over the duration of the observation. We give a brief summary of the pulsar processing capabilities highlighted by examples from the PSR 1641-45 data.

Type
Part 3. Studies of Radio Emission
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Carlson, B.R. et al. 1999, PASP, 111, 10251047 CrossRefGoogle Scholar