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Narrow-Angle and Wide-Angle Astrometry via Long Baseline Optical/Infrared Interferometers

Pan, Xiaopei and Kulkarni, Shri and Shao, Michael and Colavita, M. Mark (1995) Narrow-Angle and Wide-Angle Astrometry via Long Baseline Optical/Infrared Interferometers. In: Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry. IAU Symposium Proceedings Series. No.166. Kluwer , Dordrecht, pp. 13-18. ISBN 9789401100694. https://resolver.caltech.edu/CaltechAUTHORS:20181211-104525501

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Abstract

Long baseline optical/infrared interferometers, such as the Mark III Stellar Interferometer on Mt. Wilson and the ASEPS-0 Testbed Interferometer on Palomar Mountain, California, have good capabilities for narrow-angle and wide-angle astrometry with very high precision. Using the Mark III Interferometer many spectroscopic binaries became “visual” for the first time. The measurement accuracy of angular separation is 0.2 mas, the smallest separation measured between two components is 2 mas, the maximum magnitude difference is 4 mag, and the smallest semimajor axis is 4 mas. Such high angular resolution and dynamic range have been used to determine stellar masses with precision of 2% and differential stellar luminosities to better than 0.05 mag for separations of less than 0.″2. For some binary stars, not only have the systems been resolved, but also the diameter of the primary component has been determined, yielding direct measurements of stellar effective temperature with high accuracy. For parallax determination, the precision is 1 mas or better and is unaffected by interstellar extinction. For wide-angle astrometry with the Mark III interferometer, the observation results yielded average formal 1σ errors for FK5 stars of about 10 mas. Presently a new infrared interferometer, the ASEPS-0 Testbed Interferometer on Palomar Mountain is under construction, and is being optimized to perform high accuracy narrow-angle astrometry using long baseline observations at 2.2 μm, with phase referencing for increased sensitivity. The goal is to demonstrate differential astrometric accuracies of 0.06–0.1 mas in order to allow for detection of extra-solar planets in the near future.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
https://doi.org/10.1017/S0074180900227769DOIArticle
https://doi.org/10.1007/978-94-011-0069-4_3DOIArticle
https://rdcu.be/b37tgPublisherFree ReadCube access
ORCID:
AuthorORCID
Kulkarni, Shri0000-0001-5390-8563
Additional Information:© 1995 IAU.
Series Name:IAU Symposium Proceedings Series
Issue or Number:166
Record Number:CaltechAUTHORS:20181211-104525501
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20181211-104525501
Official Citation:Pan, X., Kulkarni, S., Shao, M., & Colavita, M. (1995). Narrow-Angle and Wide-Angle Astrometry via Long Baseline Optical/Infrared Interferometers. Symposium - International Astronomical Union, 166, 13-18. doi:10.1017/S0074180900227769
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:91682
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:11 Dec 2018 19:42
Last Modified:12 May 2020 21:06

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