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Geodetic VLBI Experiment at 22 GHz Band Between Japan and Italy

Published online by Cambridge University Press:  07 August 2017

Y. Takahashi ,
H. Kiuchi ,
N. Kurihara ,
G. Grueff  and
R. Ambrosini
Y. Takahashi
Affiliation:
Kashima Space Research Center, Communications Research Laboratory 893-1 Hirai, Kashima, Ibaraki, Japan 314
H. Kiuchi
Affiliation:
Kashima Space Research Center, Communications Research Laboratory 893-1 Hirai, Kashima, Ibaraki, Japan 314
N. Kurihara
Affiliation:
Kashima Space Research Center, Communications Research Laboratory 893-1 Hirai, Kashima, Ibaraki, Japan 314
G. Grueff
Affiliation:
Astronomy Department, Bologna University, Bologna, Italy
R. Ambrosini
Affiliation:
Institute of Radioastronomy, National Council of Research Irnerio 46 40126 Bologna, Italy

Abstract

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Geodetic VLBI experiments are usually conducted at S/X dual bands. Some advantages can be gained at some higher frequency band and in particular at 22 GHz band (K band). We organized a geodetic VLBI experiment on the 16th of February 1991 between Kashima 34m antenna of the Communication Research Laboratory (CRL), in Japan and Medicina 32 m telescope of the Institute of antenna(IRA), in Italy. The phase calibrator was developed using a new “up-conversion” scheme for K band. Data relative to 212 observations of 40 sources were correlated and for 152 scans we obtained correlated amplitudes, delays and delay rates. The r.m.s. residuals have been found to be 100 ps for delays, and 74 fs/s for delay rates. The coherence loss of correlation amplitude becomes large at higher frequency band than 22GHz due to the atmospheric scintillation. The estimated method of the coherence loss was presented. The correlated flux densities at K band evaluated from them were found to be smaller than the ones at X band in general.

Type
Very Long Baseline Interferometry (VLBI)
Information
Symposium - International Astronomical Union , Volume 156: Developments in Astrometry and their Impacts on Astrophysics , 1993 , pp. 185 - 190
Copyright
Copyright © Kluwer 

References

Ambrosini, R., Roma, M., Internal Report IRA 134/90/ June 1990.Google Scholar
Hitosi, Kiuchi, Journal of the Communications Research Laboratory, Vol. 38, No. 3 1991.Google Scholar
Ma, C., Ryan, J.W., Caprette, D.S., NASA Technical Memorandum 104552/ March 1992.Google Scholar
Takahashi, Y., Journal of the Communications Research Laboratory, Vol. 38, No. 3 1991.Google Scholar