Self-noise in interferometers - Radio and infrared
- Creators
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Kulkarni, Shrinivas R.
Abstract
A complete theory of noise in a synthesis image is proposed for a source of arbitrary strength. In the limit of faint sources, the standard estimates of noise in a synthesis image are recovered, while in the limit of strong sources, the noise in the synthesis image is found to be dominated by either self noise or by the noise generated by the source signal itself. It is found that the best VLBI maps (with noise approaching the thermal noise) may in fact be limited by self noise, and that there is a negligible bias in the standard definitions of the bispectrum phasor and the closure phase. The results suggest that at the low signal levels which are characteristic of infrared interferometers, it is best to fit the model to all the closure phases and fringe amplitudes.
Additional Information
© 1989 American Astronomical Society. Provided by the NASA Astrophysics Data System. Received 26 January 1989; revised 11 April 1989. I am most grateful to the W. M. Keck foundation for a grant under which all of the work reported here was performed. I thank A. C. S. Readhead for early discussions which led to this work, and S. Myers for a careful reading of the manuscript and for pointing out a fundamental flaw with the previous version of the paper. Discussions with D. Jones, T. Nakajima, and T. Pearson were very useful and resulted in improvement of the paper. I thank them for this.Attached Files
Published - Kulkarni_1989p1112.pdf
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Additional details
- Eprint ID
- 38225
- Resolver ID
- CaltechAUTHORS:20130502-082728815
- W. M. Keck Foundation
- Alfred P. Sloan Foundation
- NSF
- Created
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2013-05-02Created from EPrint's datestamp field
- Updated
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2019-10-03Created from EPrint's last_modified field
- Caltech groups
- Division of Geological and Planetary Sciences (GPS)