AMBER, the near-infrared spectro-interferometric three-telescope VLTI instrument

R. G. Petrov (1, 2) , F. Malbet (3) , G. Weigelt (4) , P. Antonelli (5, 6) , U. Beckmann (4) , Y. Bresson (5, 6, 7) , A. Chelli (3) , M. Dugué (5, 6, 7) , G. Duvert (3) , S. Gennari (8) , L. Glück (3) , P. Kern (3) , S. Lagarde (5, 6, 7) , E. Le Coarer (3) , F. Lisi (8) , F. Millour (1, 3, 4) , K. Perraut (3) , P. Puget (3) , F. Rantakyrö (9) , S. Robbe-Dubois (1, 10) , A. Roussel (5, 7) , P. Salinari (8) , E. Tatulli (3, 8) , G. Zins (3) , M. Accardo (8) , B. Acke (3) , K. Agabi (1) , E. Altariba (1) , B. Arezki (3) , E. Aristidi (1) , C. Baffa (8) , J. Behrend (4) , T. Blöcker (4) , S. Bonhomme (3, 5) , S. Busoni (8) , F. Cassaing (11) , J.-M. Clausse (5) , J. Colin (5, 12) , C. Connot (4) , A. Delboulbé (3) , A. Domiciano de Souza (1, 5, 4) , T. Driebe (4) , P. Feautrier (3) , D. Ferruzzi (8) , T. Forveille (3, 13) , E. Fossat (1) , Renaud Foy (14) , D. Didier Fraix-Burnet (3) , A. Gallardo (3) , E. Giani (8) , C. Gil (3, 15) , A. Glentzlin (5) , M. Heiden (4) , M. Heininger (4) , O. Hernandez Utrera (3) , K.-H. Hofmann (4) , D. Kamm (5, 6) , M. Kiekebusch (9) , S. Kraus (4) , D. Le Contel (5, 6) , J.-M. Le Contel (5) , T. Lesourd , B. Lopez (5, 6) , Morgan Lopez , Y. Magnard (3) , A. Marconi (8) , G. Mars (5, 6) , G. Martinot-Lagarde (5, 16) , P. Mathias (5, 7) , P. Mège (3) , J.-L. Monin (3) , D. Mouillet (3, 17) , D. Mourard (5, 6, 7) , E. Nussbaum (4) , K. Ohnaka (4) , J. Pacheco (5, 7) , C. Perrier (3) , Y. Rabbia (5, 6) , S. Rebattu (5, 6) , François Reynaud (18) , A. Richichi (8, 9) , A. Robini , M. Sacchettini (3) , D. Schertl (4) , M. Schöller (9) , W. Solscheid (4) , A. Spang (5) , P. Stee (1, 5, 7, 12) , P. Stefanini (8) , Michel Tallon (14) , Isabelle Tallon-Bosc (14) , D. Tasso (5) , L. Testi (8) , F. Vakili (1, 12) , O. von Der Lühe , J.-C. Valtier (5) , M. Vannier (1, 9) , N. Ventura (3)

1 LUAN - Laboratoire Universitaire d'Astrophysique de Nice
2 UNS - Université Nice Sophia Antipolis (1965 - 2019)
3 LAOG - Laboratoire d'Astrophysique de Grenoble
4 MPIFR - Max-Planck-Institut für Radioastronomie
5 LG - Laboratoire Gemini
6 FRESNEL - Département Fresnel
7 CASSIOPEE - Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides
8 OAA - INAF - Osservatorio Astrofisico di Arcetri
9 ESO - European Southern Observatory
10 Laboratoire Universitaire d'Astrophysique de Nice
11 ONERA - The French Aerospace Lab [Châtillon]
12 OCA - Observatoire de la Côte d'Azur
13 CFHT - Canada-France-Hawaii Telescope Corporation
14 CRAL - Centre de Recherche Astrophysique de Lyon
15 CEA/DSM/DRFC - Association EURATOM-CEA
16 DTI - Division technique INSU/SDU
17 LATT - Laboratoire Astrophysique de Toulouse-Tarbes
18 PHOTONIQUE

Context: Optical long-baseline interferometry is moving a crucial step forward with the advent of general-user scientific instruments that equip large aperture and hectometric baseline facilities, such as the Very Large Telescope Interferometer (VLTI). Aims: AMBER is one of the VLTI instruments that combines up to three beams with low, moderate and high spectral resolutions in order to provide milli-arcsecond spatial resolution for compact astrophysical sources in the near-infrared wavelength domain. Its main specifications are based on three key programs on young stellar objects, active galactic nuclei central regions, masses, and spectra of hot extra-solar planets. Methods: These key science goals led to scientific specifications, which were used to propose and then validate the instrument concept. AMBER uses single-mode fibers to filter the entrance signal and to reach highly accurate, multiaxial three-beam combination, yielding three baselines and a closure phase, three spectral dispersive elements, and specific self-calibration procedures. Results: The AMBER measurements yield spectrally dispersed calibrated visibilities, color-differential complex visibilities, and a closure phase allows astronomers to contemplate rudimentary imaging and highly accurate visibility and phase differential measurements. AMBER was installed in 2004 at the Paranal Observatory. We describe here the present implementation of the instrument in the configuration with which the astronomical community can access it. Conclusions: .After two years of commissioning tests and preliminary observations, AMBER has produced its first refereed publications, allowing assessment of its scientific potential.

Mots clés: instrumentation: high angular resolution; techniques:; interferometric; techniques: spectroscopic

Domaines: Cosmologie et astrophysique extra-galactique [astro-ph.CO]; Cosmologie et astrophysique extra-galactique [astro-ph.CO]

R. G. Petrov, F. Malbet, G. Weigelt, P. Antonelli, U. Beckmann, et al.. AMBER, the near-infrared spectro-interferometric three-telescope VLTI instrument. Astronomy and Astrophysics - A&A, 2007, 464, pp.1-12. ⟨10.1051/0004-6361:20066496⟩. ⟨hal-00199694⟩