Consortium

  • LAOG: Laboratoire d’Astrophysique de Grenoble, France (PI institute)
  • OCA: Observatoire de la Côte d’Azur in Nice, France
  • INAF: Instituto Nazionale di Astrofisica  Osservatorio Astrofisico di Arcetri in Firenze, Italy
  • MPIfR: Max-Planck-Institut für Radioastronomie in Bonn, Germany

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The AMBER instrument

AMBER (Astronomical Multi BEam Recombiner) is one of the first-generation ESO VLTI (Very Large Telescope Interferometer) instruments. It provides interferometric beam combination in the near-infrared domain from 1 to 2.4 μm (J, H and K bands). The instrument is built for two or three beams from either the 8-meter VLT unit telescopes (UTs) or the 1.8-meter auxiliary telescopes (ATs). AMBER offers the means to perform high quality interferometric measurements and is able to reconstruct real images using phase closure techniques. With a spectral resolution of up to 10000 and a limiting magnitude of 14, the angular resolution is 2 mas in the K band. The excellent instrument stability allows a visibility accuracy of 103 to 104 for bright objects. The main scientific objectives are the investigation of disks and jets around Young Stellar Objects and Active Galactic Nuclei (AGN) at very high angular resolution.

Overview

object Object classes:
hot exoplanets,
formation and evolution of stars,
extragalactic sources

Atmosphere Atmosphere

Telescopes:
ESO VLTI

Delay Lines Delay Lines
ESO Delay Lines

Optic Optics:
Optics developed by the AMBER consortium
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Spectrograph Spectrograph:
Spectrograph developed by the AMBER consortium
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Image sensor Imaging sensor:
HAWAII-1
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Electronic Electronics:
Readout Electronics developed by our group
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Instrument Control Software:
AMBER Detector Control Software (DCS) developed by our group
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Reduktion Software Data Reduction Software:
AMBER Data Reduction Software (DRS)


 
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