Stellar Angular Diameters of Late-Type Giants and SupergiantsMeasured with the NavyPrototype Optical Interferometer

Tyler E. Nordgren; M. E. Germain; J. A. Benson; D. Mozurkewich; J. J. Sudol; N. M. Elias II; Arsen R. Hajian; N. M. White; D. J. Hutter; K. J. Johnston; F. S. Gauss; J. T. Armstrong; T. A. Pauls; L. J Rickard

doi:10.1086/301114

Stellar Angular Diameters of Late-Type Giants and Supergiants Measured with the Navy Prototype Optical Interferometer

Tyler E. Nordgren¹, M. E. Germain¹, J. A. Benson¹, D. Mozurkewich², J. J. Sudol^3,4, N. M. Elias II¹, Arsen R. Hajian⁵, N. M. White⁶, D. J. Hutter⁵, K. J. Johnston⁵, F. S. Gauss⁵, J. T. Armstrong², T. A. Pauls², and L. J Rickard²

© 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A.
The Astronomical Journal, Volume 118, Number 6 Citation Tyler E. Nordgren et al 1999 AJ 118 3032 DOI 10.1086/301114

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Author affiliations

¹ Astrometry Department, US Naval Observatory, NPOI, P.O. Box 1149, Flagstaff, AZ 86002-1149

² Remote Sensing Division, Naval Research Laboratory, Code 7210, Washington, DC 20375

³ Department of Physics and Astronomy, University of Wyoming, Box 3905, University Station, Laramie, WY 82076

⁴ NASA PASS Grant Fellow, University of Wyoming

⁵ Astrometry Department, US Naval Observatory, 3450 Massachusetts Avenue, NW, Washington, DC 20392

⁶ Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001

Dates

Received 1998 September 4
Accepted 1999 August 18

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Abstract

We have measured the angular diameters of 50 F, G, K, and M giant and supergiant stars using the Navy Prototype Optical Interferometer at wavelengths between 649 and 850 nm and using three baselines with lengths up to 37.5 m. Uniform-disk diameters, obtained from fits to the visibility amplitude, were transformed to limb-darkened diameters through the use of limb-darkening coefficients for plane-parallel stellar atmosphere models. These limb-darkened diameters are compared with those measured with the Mark III optical interferometer and with those computed by the infrared flux method. Sources of random and systematic error in the observations are discussed.

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