Publications of the MPIfR
Optical & Infrared
Interferometry Group
R.G. Petrov, F. Malbet, G. Weigelt,
P. Antonelli, U. Beckmann, Y. Bresson, A. Chelli, M. Dugué,
G. Duvert, S. Gennari, L. Glück, P. Kern, S. Lagarde, E. Le
Coarer, F. Lisi, F. Millour,
K. Perraut, P. Puget, F. Rantakyrö, S. Robbe-Dubois, A. Roussel,
P. Salinari, E. Tatulli, G. Zins,
M. Accardo, B. Acke, K. Agabi, E. Altariba, B. Arezki, E. Aristidi, C.
Baffa, J.
Behrend,
T. Blöcker, S. Bonhomme, S. Busoni, F. Cassaing, J.-M. Clausse,
J. Colin, C. Connot,
A. Delboulbé, A. Domiciano de Souza, T. Driebe, P. Feautrier, D.
Ferruzzi, T. Forveille, E. Fossat,
R. Foy, D. Fraix-Burnet, A. Gallardo, E. Giani, C. Gil, A. Glentzlin,
M. Heiden, M. Heininger,
O. Hernandez Utrera, K.-H. Hofmann, D. Kamm, M. Kiekebusch, S.
Kraus, D. Le Contel, J.-M. Le
Contel, T. Lesourd, B. Lopez, M. Lopez, Y. Magnard, A. Marconi,
G. Mars,
G. Martinot-Lagarde, P. Mathias, P. Mège, J.-L. Monin, D. Mouillet, D.
Mourard,
E. Nussbaum, K. Ohnaka, J. Pacheco, C. Perrier, Y. Rabbia, S.
Rebattu, F. Reynaud,
A. Richichi, A. Robini, M. Sacchettini, D. Schertl, M. Schöller,
W. Solscheid, A. Spang, P. Stee,
P. Stefanini, M. Tallon, I. Tallon-Bosc, D. Tasso, L. Testi, F.
Vakili, O. von der Lühe,
J.-C. Valtier, M. Vannier, and N. Ventura
AMBER, the near-infrared
spectro-interferometric three-telescope VLTI instrument
Astronomy & Astrophysics, vol.464, pg.1-12
(2007)
Abstract
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.
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