Wide-angle astrometry with the Mark III stellar interferometer

Shao, Michael; Colavita, M. M.; Hines, Braden E.; Hershey, J. L.; Hughes, J. A.; Hutter, D. J.; Kaplan, G. H.; Johnston, K. J.; Mozurkewich, David; Simon, R. S.; Pan, Xiaopei

doi:10.1086/115630

Cited by 49 publications

(35 citation statements)

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“…The internal delay that is necessary to observe interference therefore contains information on the star's position, hence a series of delay measurements can be used for the determination of accurate stellar positions (e.g. Shao et al 1990;Hummel et al 1994). The relation between the optical delay w and the stellar position defined by the unit vector s in direction of the star is…”

Section: Principles Of Narrow-angle Astrometrymentioning

confidence: 99%

“…(14) allows for the non-degenerate solution for the three components of B Wide (e.g. Shao et al 1990;Buscher 2012). The pivot point of an ideal telescope is defined as the intersection between the altitude and azimuth axes and remains at a fixed position in the horizontal coordinate system at all times.…”

Section: Wide-angle Astrometric Baselinementioning

confidence: 99%

“…Construction of optical interferometers was in part motivated by their capability of performing precise (a few mas) global astrometry (Shao et al 1990) and very precise (∼10 µas) narrow-angle relative astrometry (Shao & Colavita 1992). The latter requires a dual feed configuration to observe two stars simultaneously, which was demonstrated at the Palomar Testbed Interferometer (PTI; Lane & Colavita 2003).…”

Section: Introductionmentioning

confidence: 99%

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The ESPRI project: astrometric exoplanet search with PRIMA

Launhardt

Queloz²,

Henning

et al. 2008

SPIE Proceedings

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Context. The ESPRI project relies on the astrometric capabilities offered by the PRIMA facility of the Very Large Telescope Interferometer for discovering and studying planetary systems. Our survey consists of obtaining high-precision astrometry for a large sample of stars over several years to detect their barycentric motions due to orbiting planets. We present the operation's principle, the instrument's implementation, and the results of a first series of test observations. Aims. We give a comprehensive overview of the instrument infrastructure and present the observation strategy for dual-field relative astrometry in the infrared K-band. We describe the differential delay lines, a key component of the PRIMA facility that was delivered by the ESPRI consortium, and discuss their performance within the facility. This paper serves as reference for future ESPRI publications and for the users of the PRIMA facility. Methods. Observations of bright visual binaries were used to test the observation procedures and to establish the instrument's astrometric precision and accuracy. The data reduction strategy for the astrometry and the necessary corrections to the raw data are presented. Adaptive optics observations with NACO were used as an independent verification of PRIMA astrometric observations. Results. The PRIMA facility was used to carry out tests of astrometric observations. The astrometric performance in terms of precision is limited by the atmospheric turbulence at a level close to the theoretical expectations and a precision of 30 µas was achieved. In contrast, the astrometric accuracy is insufficient for the goals of the ESPRI project and is currently limited by systematic errors that originate in the part of the interferometer beamtrain that is not monitored by the internal metrology system. Conclusions. Our observations led to defining corrective actions required to make the facility ready for carrying out the ESPRI search for extrasolar planets.

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Section: Principles Of Narrow-angle Astrometrymentioning

confidence: 99%

Section: Wide-angle Astrometric Baselinementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The ESPRI project: astrometric exoplanet search with PRIMA

Launhardt

Queloz²,

Henning

et al. 2008

SPIE Proceedings

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“…The interferometer concept shown is the result of a systems design performed at MIT for NASA's Jet Propulsion Laboratory interferometry group [50,51].…”

Section: Interferometrymentioning

confidence: 99%

Evolutionary Design of Controlled Structures

Masters

Crawley

1999

Journal of Aircraft

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“…The astrometric baselines of this instrument are ~ 12 m long (Mozurkewich et al 1988). Astrometric observations with the Mklll have resulted in corrections tb twelve FK5 star positions with ~ 10 mas errors (Shao et al .1990;Hummel 1993). There are, however, small systematic effects present in these positions, the most important being the mechanical and thermal motions within the instrument.…”

Section: Introductionmentioning

confidence: 99%

The Baseline Metrology System of the USNO Astrometric Interferometer

Elias

Hutter

1994

Symp. - Int. Astron. Union

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Abstract. The USNO Astrometric Interferometer (USNOAI; a subarray of the Navy Prototype Optical Interferometer at Lowell Observatory) is presently under construction and expected to begin limited operations within a year. The main goal of the USNOAI observations is to provide a northern hemisphere catalog of several thousand stars with positions known to a few mas. In order to meet this requirement, a baseline laser metrology system must be employed to measure the three-dimensional motions of the baselines with an accuracy better than ~ 0.1 μτη. The metrology scheme, as presently conceived, represents the largest and most complex high-resolution laser metrology system ever attempted.

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Wide-angle astrometry with the Mark III stellar interferometer

Cited by 49 publications

References 0 publications

The ESPRI project: astrometric exoplanet search with PRIMA

The ESPRI project: astrometric exoplanet search with PRIMA

Evolutionary Design of Controlled Structures

The Baseline Metrology System of the USNO Astrometric Interferometer

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