5 days ago · UVES is the high-resolution optical spectrograph of the VLT located at the Nasmyth B focus of UT2. It is a cross-dispersed echelle spectrograph designed to operate with high efficiency from the atmospheric cut-off at 300 nmto the long wavelength limit of the CCD detectors (about 1100 nm).

UVES has provided us with a forest-full of detailed spectroscopic data of an impressive variety of objects — from stars inside our galaxy, the Milky Way, to distant galaxies and gamma-ray bursts.

There are two data sets below. The first is the complete set of velocities (uves_vels.tar). The second is the binned set of data (uves_vels_binned.tar). Often two or more consecutive observations are taken of a star. Faint stars require more than 20 minutes to achieve the necessary signal-to-noise.

UVES (UltraViolet and Visible Echelle Spectrograph) is the high-dispersion spectrograph of the VLT, observing from 300 nm to 1100 nm, with a maximum spectral resolution of 110 000. VISIR (VLT Imager and Spectrometer for mid-Infrared) studies the infrared light from celestial objects.

The Very Large Telescope (VLT) is an astronomical facility operated since 1998 by the European Southern Observatory, located on Cerro Paranal in the Atacama Desert of northern Chile. It consists of four individual telescopes, each equipped with a primary mirror that measures 8.2 metres (27 ft) in diameter.

UVES is a dual beam echelle spectrograph installed at the Nasmyth focus of the UT2 telescope (Kueyen) of the ESO VLT since October 1999. It can reach a resolution of 80000 and 115000 in the blue (300-500nm) and red (420-10050 nm) arm, respectively.

Oct 1, 2017 · High-resolution VLT/UVES spectra of multiple OH bands taken between 2000 and 2015. OH intensities and rotational temperatures show strong solar cycle effects. Good agreement with SABER OH data taken close to the VLT between 2002 and 2015.

Sep 3, 2024 · In 2000, observations by the VLT's UVES instrument of a quasar that we see as it existed 12 billion years ago found that the universe at that time was between 6 and 14 kelvins, which agrees...

Inside UVES, the incoming beam of light is sent to either a blue (UV-to-blue) or a red (visible-to-red) arm — the two branches. Each of these arms goes through two perpendicular gratings, and each grating has a number of grooves which spread out the light by diffraction — the twigs.

3 days ago · A continuous observing window of 4.5 h was obtained through directors discretionary time on the 8.2 m VLT with the UVES. Each exposure lasted for 730 s with a readout time between exposures of 45 ...