First light for GRAVITY: Phase referencing optical interferometry for the Very Large Telescope Interferometer

被引：390

作者：

Abuter, R. ^{[10
]}

Accardo, M. ^{[10
]}

Amorim, A. ^{[6
,7
]}

Anugu, N. ^{[8
,9
]}

Avila, G. ^{[10
]}

Azouaoui, N. ^{[2
]}

Benisty, M. ^{[5
]}

Berger, J. P. ^{[5
]}

Blind, N. ^{[12
]}

Bonnet, H. ^{[10
]}

Bourget, P. ^{[11
]}

Brandner, W. ^{[3
]}

Brast, R. ^{[10
]}

Buron, A. ^{[1
]}

Burtscher, L. ^{[1
,17
]}

Cassaing, F. ^{[13
]}

Chapron, F. ^{[2
]}

Choquet, E. ^{[2
]}

Clenet, Y. ^{[2
]}

Collin, C. ^{[2
]}

du Foresto, V. Coude ^{[2
]}

de Wit, W. ^{[11
]}

de Zeeuw, P. T. ^{[10
,17
]}

Deen, C. ^{[1
]}

Delplancke-Stroebele, F. ^{[10
]}

Dembet, R. ^{[2
]}

Derie, F. ^{[10
]}

Dexter, J. ^{[1
]}

Duvert, G. ^{[5
]}

Ebert, M. ^{[3
]}

Eckart, A. ^{[4
,16
]}

Eisenhauer, F. ^{[1
]}

Esselborn, M. ^{[10
]}

Fedou, P. ^{[2
]}

Finger, G. ^{[10
]}

Garcia, P. ^{[8
,9
]}

Dabo, C. E. Garcia ^{[10
]}

Lopez, R. Garcia ^{[3
]}

Gendron, E. ^{[2
]}

Genzel, R. ^{[1
,18
]}

Gillessen, S. ^{[1
]}

Gonte, F. ^{[10
]}

Gordo, P. ^{[6
,7
]}

Grould, M. ^{[2
]}

Groezinger, U. ^{[3
]}

Guieu, S. ^{[5
,11
]}

Haguenauer, P. ^{[10
]}

Hans, O. ^{[1
]}

Haubois, X. ^{[11
]}

Haug, M. ^{[1
,10
]}

机构：

[1] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[2] Univ Paris Diderot, UPMC Univ Paris 06, LESIA Observ Paris, Sorbonne Univ,PSL Res Univ,CNRS,Sorbonne Paris Ci, F-92195 Meudon, France

[3] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[4] Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany

[5] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[6] CENTRA, P-1749016 Lisbon, Portugal

[7] Univ Lisbon, Fac Ciencias, P-1749016 Lisbon, Portugal

[8] CENTRA, P-4200465 Oporto, Portugal

[9] Univ Porto, Fac Engn, P-4200465 Oporto, Portugal

[10] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[11] European Southern Observ, Casilla 19001, Santiago 19, Chile

[12] Univ Geneva, Observ Geneve, 51 Ch Maillettes, CH-1290 Versoix, Switzerland

[13] Off Natl Etud & Rech Aerosp, French Aerosp Lab, BP 72, F-92322 Chatillon, France

[14] European Space Agcy, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[15] Univ Chile, CNRS, Unidad Mixta Int Franco Chilena Astron, UMI 3386,Dept Astron, Camino Observ 1515, Santiago 1515, Chile

[16] Max Planck Inst Radio Astron, Hugel 69, D-53121 Bonn, Germany

[17] Leiden Univ, Sterrewacht Leiden, Postbus 9513, NL-2300 RA Leiden, Netherlands

[18] Univ Calif Berkeley, Dept Phys, Le Conte Hall, Berkeley, CA 94720 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 602卷

基金：

欧洲研究理事会;

关键词：

instrumentation: interferometers; instrumentation: adaptive optics; Galaxy: center; quasars: emission lines; binaries: symbiotic; stars: pre-main sequence; SUPERMASSIVE BLACK-HOLE; STELLAR WIND; TRACKING ALGORITHMS; INFRARED FLARES; GALACTIC-CENTER; DATA REDUCTION; NARROW-ANGLE; ETA-CARINAE; STAR; SYSTEM;

D O I：

10.1051/0004-6361/201730838

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

GRAVITY is a new instrument to coherently combine the light of the European Southern Observatory Very Large Telescope Interferometer to form a telescope with an equivalent 130m diameter angular resolution and a collecting area of 200 m(2). The instrument comprises fiber fed integrated optics beam combination, high resolution spectroscopy, built-in beam analysis and control, near-infrared wavefront sensing, phase-tracking, dual-beam operation, and laser metrology. GRAVITY opens up to optical/infrared interferometry the techniques of phase referenced imaging and narrow angle astrometry, in many aspects following the concepts of radio interferometry. This article gives an overview of GRAVITY and reports on the performance and the first astronomical observations during commissioning in 2015/16. We demonstrate phase-tracking on stars as faint as m(K) approximate to 10 mag, phase-referenced interferometry of objects fainter than m(K) approximate to 15 mag with a limiting magnitude of m(K) approximate to 17 mag, minute long coherent integrations, a visibility accuracy of better than 0.25%, and spectro-differential phase and closure phase accuracy better than 0.5 degrees, corresponding to a differential astrometric precision of better than ten microarcseconds (as). The dual-beam astrometry, measuring the phase difference of two objects with laser metrology, is still under commissioning. First observations show residuals as low as 50 mu as when following objects over several months. We illustrate the instrument performance with the observations of archetypical objects for the different instrument modes. Examples include the Galactic center supermassive black hole and its fast orbiting star S2 for phase referenced dual-beam observations and infrared wavefront sensing, the high mass X-ray binary BP Cru and the active galactic nucleus of PDS 456 for a few mu as spectro-differential astrometry, the T Tauri star S CrA for a spectro-differential visibility analysis, xi Tel and 24 Cap for high accuracy visibility observations, and eta Car for interferometric imaging with GRAVITY.

引用

页数：23

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