Phase-Sensitive Light Amplifiers in Stellar Interferometry
The signal-to-noise ratio problems in stellar interferometry are serious in a manner somewhat similar to the case of gravitational wave detection. For instance, Hanbury Brown determined the diameters of 32 stars by his intensity interferometer . Without some new technology development such as the squeezed state technique, there is not much chance for further improvement. As soon as the laser amplifier became available, I was interested in its possible applications to improve the sensitivity of the intensity interferometer. To my great disappointment I learned from Professor Charles Townes  that the (phase-insensitive) laser amplifier cannot improve the S/N but worsens the situation due to the excessive spontaneous emissions.
Unable to display preview. Download preview PDF.
- 1.R. Hanbury Brown,The Intensity Interferometer, Taylor and Francis (1974).Google Scholar
- 2..Charles Townes,Fundamental limitations on use of Maser Amplifications for Image Intensification Institute of Defense Analyses, Technical Note 61–20, August (1961).Google Scholar
- 3..Carlton M. Caves,Phys. Rev., D26, pp. 1817–1839 (1982).Google Scholar
- 5.R.Q. Twiss,Optica Acta, 16, pp. 423–451 (1969).Google Scholar
- 6.H. Gamo, Adv. in Quant. Electronic, Columbia Ubiversity Press, pp. 252–266 (1961).Google Scholar
- 7.H. Gamo,Electromagnetic Waves and Antenna, ed. by EC. Jordan, Part 2, pp. 801–810, Pergamon Press, (1963).Google Scholar
- 10..M. Born and E. Wolf,Principles of Optics, Chap. 10, Pergamon Press.Google Scholar
- 12.C.M. Caves and DD. Crouch,J. Opt.Soc.Am., 4B, pp. 1535–1545 (1987).Google Scholar
- 13.B. Yurke,Phys. Rev., A32, pp. 211–223 (1985).Google Scholar
- 14..Horace P. Yuen,Proceedings of the Sixth Rochester Conference and Quantum Optics.Google Scholar