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14 - Modern Optical Interferometers

from Part 1 - Optical Observatories

Published online by Cambridge University Press:  15 December 2016

David Leverington
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Summary

Mount Wilson

Michelson had designed a stellar interferometer for the Mount Wilson Observatory in 1920 that consisted of a 6 m (20 ft) long steel girder and two 15 cm (6 inch) movable mirrors which he mounted across the open end of the 2.5 m (100 inch) telescope.(1) This enabled Michelson and Pease to measure the diameter of a number of red giants. However, little more interferometric work was done on Mount Wilson until 1979 when Michael Shao and David Staelin of the Massachusetts Institute of Technology designed a two telescope, white light, 1.5 m (5 ft) baseline interferometer. It was the first interferometer to compensate for atmospheric turbulence by making continuous phase and amplitude measurements with a 4 ms integration time. The Mark I was succeeded by the 3.1 m Mark II interferometer which was used as a technology testbed for astrometric measurements from 1982 to 1984. It incorporated a high speed, ultra high accuracy, laser controlled optical delay line, and it was also used to develop an operational procedure for rapid switching between stars. The Mark II was, in turn, followed by the Mark III(2) from 1986 to 1993 which had a maximum baseline of 32 m and operated in two spectral bands from about 400 to 600 nm and from about 600 to 900 nm. Like the Mark II, the Mark III was designed to test out new techniques and technologies. Its aim was to be reliable and easy to operate, whilst being capable of extremely accurate astronomical measurements of stellar positions and diameters. Lessons learnt in operating the Mark III were applied to the design of the US Naval Observatory's NPOI (Navy Prototype Optical Interferometer, see Section 14.6) located in the mountains near Flagstaff, Arizona which became operational in 1996.

Berkeley Infrared Spatial Interferometer (ISI)

Instead of using the Michelson homodyne or direct detection system of the above instruments, Charles Townes, Mike Johnson and Al Betz of the University of California (UC) at Berkeley(3) used a heterodyne system in 1974 to produce the first mid-infrared interferometer based on techniques used in radio astronomy.

Type
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Information
Observatories and Telescopes of Modern Times
Ground-Based Optical and Radio Astronomy Facilities since 1945
 , pp. 244 - 253
Publisher: Cambridge University Press
Print publication year: 2016

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References

1. Fehrenbach, Charles, Twentieth-century instrumentation, in Gingerich, Owen, (ed.), Astrophysics and Twentieth-century Astronomy to 1950; Part A, Cambridge University Press, 1984, pp. 182–184.
2. Shao, M., et al., The Mark III Stellar Interferometer, Astronomy and Astrophysics, 193, 1988, pp. 357–371.Google Scholar
3. Johnson, M. A., Betz, A. L., and Townes, C. H., Results from the 5.5 Meter Infrared Stellar Interferometer, Bulletin of the American Astronomical Society, 6, 1974, pp. 450–451.Google Scholar
4. Shao, M., and Colavita, M. M., Long-Baseline Optical and Infrared Stellar Interferometry, Annual Review of Astronomy and Astrophysics, 30, 1992, pp. 457–498.Google Scholar
5. Danchi, W. C., Bester, M., and Townes, C. H., The U. C. Berkeley Infrared Heterodyne Interferometer, ESO Conference Workshop Proceedings No. 29, Part 2, pp. 867–877.
6. Hale, D. D. S., et al., The Berkeley Infrared Spatial Interferometer: A Heterodyne Stellar Interferometer for the Mid-Infrared, Astrophysical Journal, 537, 2000, pp. 998–1012.Google Scholar
7. McCullough, P. R., et al., Bulletin of the American Astronomical Society, 20, 1988, p. 1007.
8. ten Brummelaar, T. A., et al., First Results from the CHARA Array. II. A Description of the Instrument, Astrophysical Journal, 628, 2005, pp. 453–465.Google Scholar
9. Monnier, John D., et al., Imaging the Surface of Altair, Science, 317, 2007, pp. 342–345.Google Scholar
10. Kloppenborg, Brian, et al., Infrared Images of the Transiting Disk in the ε Aurigae System, Nature, 464, 2010, pp. 870–872.Google Scholar
11. Labeyrie, Antoine, Interference Fringes Obtained on Vega with Two Optical Telescopes, Astrophysical Journal, 196, 1975, pp. L71–L75.Google Scholar
12. Blazit, A., et al., The Angular Diameters of Capella A and B from Two-Telescope Interferometry, Astrophysical Journal, 217, 1977, pp. L55–L57.Google Scholar
13. Labeyrie, Antoine, Stellar Interferometry: A Widening Frontier, Sky and Telescope, April 1982, pp. 334–338.Google Scholar
14. Baldwin, J. E., The First Images from the Optical Aperture Synthesis Array: Mapping of Capella with COAST at Two Epochs, Astronomy and Astrophysics, 306, 1996, pp. L13–L16.Google Scholar
15. Millan-Gabet, R., et al., A NICMOS3 Camera for Fringe Detection at the IOTA Interferometer, Publications of the Astronomical Society of the Pacific, 111, 1999, pp. 238–245.Google Scholar
16. Colavita, M. M., The Palomar Testbed Interferometer, Astrophysical Journal, 510, 1999, pp. 505–521.Google Scholar
17. Muterspaugh, Matthew W., et al., Scientific Results from High-precision Astrometry at the Palomar Testbed Interferometer in Monnier, John, D., et al., (eds.), Advances in Stellar Interferometry, Proc. SPIE, 6268, 2006.
18. van Belle, Gerard T., et al., Altair's Oblateness and Rotation Velocity from Long-Baseline Interferometry, Astrophysical Journal, 559, 2001, pp. 1155–1164.Google Scholar
19. Simon, R. S., et al., Imaging Optical Interferometry, in Cornwell, T. J., and Perley, R. A., (eds.), Radio Interferometry: Theory, Techniques and Applications, IAU Coll. 131, ASP Conference Series, 19, 1991, pp. 358–367.Google Scholar
20. Armstrong, J. T., et al., The Navy Prototype Optical Interferometer, Astrophysical Journal, 496, 1998, pp. 550–571.Google Scholar
21. Hutter, D. J., et al., Seeing Tests at Four Sites in Support of the NPOI Project, Astronomical Journal, 114, 1997, pp. 2822–2833.Google Scholar
22. Armstrong, J. T., et al., The Navy Precision Optical Interferometer (NPOI): An Update, Journal of Astronomical Instrumentation, 2, Issue 2, 2013, pp. 1–8.Google Scholar

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