Project ‘VLTI Tutorial’ Milestones: • Principle of Interferometry: concept of coherence length and spatial coherence, van Cittert-Zernike Theorem • Types of Interferometers: Michelson and Fizeau, Homothetic mapping, measurement of the visibility • Atmospheric turbulence: What does AO do for interferometry,

The result shows an impressive allbeit elongated PSF with a full width at half maximum (F W HM ) of about 4 × 8 milli arcsec for a wavelength of 2.2 µm. As a first step towards this goal, FINITO will provide fringe tracking in the H-band.

In 2005, the dual feed facility PRIMA will extend the capabilities of the VLTI to faint objects (K = 16{19) and will allow for high precision astrometry. Last but not least, a joint ESO/ESA project for GENIE, the DARWIN ground demonstrator planned …

Sep 26, 2002 · VLT Interferometer (VLTI) that will ultimately provide European astronomers with unequalled opportunities for exciting front-line research projects.

NOTT (formerly Hi-5) is a new high-contrast L′band (3.5–4.0 µ m) beam combiner for the VLTI designed with an ambitious aim to be sensitive to young giant exoplanets down to 5 mas separation around nearby stars.

Mar 13, 2023 · NOTT (formerly Hi-5) is a new high-contrast L ′ band (3.5–4.0 µm) beam combiner for the VLTI designed with an ambitious aim to be sensitive to young giant exoplanets down to 5 mas separation around nearby stars.

Temporal power spectrum shows intensity spectrum G(ν) multiplied by the modulus V2 of the spatial coherence (VINCI) • Three beam combination produces sidelobes at each of the three frequencies. Weak or noisy signal eventually shows up in the averaged power spectrum.

Mar 28, 2022 · We have developed the Multi AperTure mid-Infrared SpectroScopic Experiment (MATISSE) to access, for the first time, high resolution imaging in a wide spectral domain.

In terms of imaging capabilities, an optical, six telescope VLTI-type configuration and ∼200 meter baseline will achieve 4 mas spatial resolution, which is comparable to ALMA and almost 50 times better than JWST will achieve at 2.2 microns. Our results show that such an instrument will be capable of imaging, with unprecedented

GRAVITY is an adaptive optics assisted Beam Combiner for the second generation VLTI instrumentation. The instrument will provide high-precision narrow-angle astrometry and phase-referenced interferometric imaging in the astronomical K-band for faint objects.