The data-reduction software for micro-arcsecond astrometry with PRIMA at the VLTI

被引：0

作者：

Koehler, Rainer ^{[1
,2
]}

Stilz, Ingo ^{[1
,2
]}

Quirrenbach, Andreas ^{[1
]}

Kaminski, Adrian ^{[1
]}

Schulze-Hartung, Tim ^{[2
]}

Launhardt, Ralf ^{[2
]}

Elias, Nicholas M., II ^{[3
]}

Henning, Thomas ^{[2
]}

Queloz, Didier ^{[4
]}

机构：

[1] Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany

[2] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[3] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA

[4] Univ Geneva, Observ Astron, CH-1290 Versoix, Switzerland

来源：

OPTICAL AND INFRARED INTERFEROMETRY II | 2010年 / 7734卷

关键词：

exoplanet detection; parallax; proper motion; PRIMA; VLTI; narrow-angle astrometry; optical interferometry; data-reduction software;

D O I：

10.1117/12.857276

中图分类号：

TM [电工技术]; TN [电子技术、通信技术];

学科分类号：

0808 ; 0809 ;

摘要：

PRIMA (Phase-Referenced Imaging and Microarcsecond Astrometry) is an ESO/VLTI instrument designed for phase-referenced imaging and narrow-angle astrometry, dedicated to exoplanet detection. The astrometric data-reduction software (ADRS) is a key component of the system, calculating very precise (similar to 10 mu as) differential angular separations projected on the sky. For an interferometer with a baseline of 100 m, this separation corresponds to measuring the (differential) optical path difference with a precision of 5 - 15 nanometers. This precision can only be achieved with careful calibration of the instrument, including effects that are irrelevant for almost any other scientific application. PRIMA is currently being commissioned on Paranal, and we expect to obtain the first astrometric data in September 2010. These data will provide a new insight into the operation and calibration of the instrument.

引用

页数：7

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