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High Resolution & High Sensitivity Spectral-Line Imaging with Multiple Arrays

Published online by Cambridge University Press:  19 July 2016

V. Migenes ,
J.A. Yates ,
R.J. Cohen ,
M.C. Shepherd  and
P.F. Bowers
V. Migenes
Affiliation:
CSIRO/ATNF, P.O. Box 76, Epping, NSW 2121 Australia
J.A. Yates
Affiliation:
NRAL/Jodrell Bank, Macclesfield. Cheshire SK11-9DL, UK
R.J. Cohen
Affiliation:
NRAL/Jodrell Bank, Macclesfield. Cheshire SK11-9DL, UK
M.C. Shepherd
Affiliation:
NRAL/Jodrell Bank, Macclesfield. Cheshire SK11-9DL, UK
P.F. Bowers
Affiliation:
E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC 20735, USA

Extract

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At present there are several radio interferometer arrays ranging from the low-resolution (0.1–1″) high-sensitivity arrays such as the Very Large Array (VLA) to the high-resolution (0.0005–0.1″) low-sensitivity arrays such as MERLIN (though MERLIN, in the UK, is really in between this broad category), EVN, VLBA and SHEVE. Combining high sensitvity and high resolution is prohibitively expensive, because to have the u–v sampling of small arrays would require more and larger antenna elements. Hence high- resolution arrays have poor u–v coverage, decreasing the sensitivity of the instrument. This has a serious effect on spectral-line work, where sensitivity has already been sacrificed in the pursuit of spectral resolution.

Type
Aperture Distributions
Information
Symposium - International Astronomical Union , Volume 158: Very High Angular Resolution Imaging , 1994 , pp. 334 - 336
Copyright
Copyright © Kluwer 1994 

References

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