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 …

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 …

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 …

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 …

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.

Feb 1, 2003 · The uv coverage is shown on the left, and the point spread function (PSF) on the right. The width of the central fringe, i.e. the angular resolution limit, is about 3 by 15 …

In order to test the feasibility of next generation optical interferometers in the context of the VLTI-spectro-imager (VSI), we have embarked on a study of image reconstruction and analysis.

The Very Large Telescope Interferometer (VLTI) is currently the best infrastructure for long-baseline interferometry in particular in terms of sensitivity and accessibility to the general user. …

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 …

At the same time, the preparation for first fringes of the VLT Interferometer (VLTI) is advancing rapidly with the goal of having the first fringes with two siderostats within this year. In this …