A prototype visible to near-infrared spectrograph for the CHARA Array, a long baseline stellar interferometer

Details A prototype visible to near-infrared spectrograph for the CHARA Array, a long baseline stellar interferometer A prototype visible to near-infrared spectrograph for the CHARA Array, a long baseline stellar interferometer

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005phdt.........5o&link_type=abstract

PhD Thesis, Proquest Dissertations And Theses 2005. Section 0079, Part 0606 548 pages; [Ph.D. dissertation].United States -- Geo

Computer Science

Near-Infrared, Spectrograph, Chara Array, Stellar Interferometer, Interferometers

Scientific paper

This work is a description of the Visible to near Infrared Spectrograph system for the CHARA array. The CHARA Array is a 6-telescope interferometer at the Mount Wilson Observatory in the mountains north of Pasadena, California. It combines the light from the 1-meter telescopes, and measures the visibility of the resulting interference fringes, which gives information about the source intensity distribution on the sky. The resolution of the instrument is proportional to the telescope separation, or baseline, divided by the wavelength. The VIS system operates in the 600-1000 nm wavelength range, a factor of 3 to 4 shorter than the standard operating wavelength at CHARA, 2.13 mm. An introduction to interferometry is given, with a description of the CHARA Array. The effects of diffraction through the system combined with atmospheric turbulence are described, and the results of a computer model given. The VIS system design is described, and results of the first fringe data are presented, including system visibility and throughput estimates.

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