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Mark III VLBI Observation of Pulsars

Published online by Cambridge University Press:  04 August 2017

N. Bartel ,
R. J. Cappallo ,
M. I. Ratner ,
A.E.E. Rogers ,
I. I. Shapiro  and
A. R. Whitney
N. Bartel
Affiliation:
1Harvard-Smithsonian Center for Astrophysics
R. J. Cappallo
Affiliation:
1Harvard-Smithsonian Center for Astrophysics
M. I. Ratner
Affiliation:
1Harvard-Smithsonian Center for Astrophysics
A.E.E. Rogers
Affiliation:
1Harvard-Smithsonian Center for Astrophysics
I. I. Shapiro
Affiliation:
1Harvard-Smithsonian Center for Astrophysics
A. R. Whitney
Affiliation:
1Harvard-Smithsonian Center for Astrophysics 2NEROC Haystock Observatory

Extract

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Mark III VLBI observations of the pulsars PSR 0329+54 and PSR 1133+16 were made at 2.3 GHz using antennas with diameters and locations as follows: 100m, Effelsberg, West Germany (but only for SPR 0329+54); 43m Green Bank, WV, USA; and 40m, Big Pine, CA, USA. The Mark III processor at the Haystack Observatory was “gated” to compute visibility amplitudes and phases as a function of pulsar longitude. This method allowed a) an improvement of the signal to noise ration, by as much as a factor of ten in the case of PSR 1133+16, and b) an interferometric investigation of the pulse structure.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 110: VLBI and Compact Radio Sources , 1984 , pp. 275 - 276
Copyright
Copyright © Reidel 1984