Very Large Telescope

We have shown that there is a straightforward method for testing off-axis segments of a very large telescope. That is not to say there may be other, perhaps better, methods, but often knowing a solution exists leads to further... 

In conclusion of this section, I think that first it is mandatory to remove the cone effect at very large telescopes, and that second this requires ... 

Important weather details are not only provided by the newest information from the Cassini orbiter the Very Large Telescope in the Atacama desert and the W. M. Keck Observatory on Hawaii are also involved. Near-IR spectra show increased cloudiness in the Titanian troposphere on the morning side, i.e., there are methane clouds at a height of about 30 km and methane drizzle at the surface (Adamkovics et al., 2007). 

Tytler D. (1997) Cosmology with the Very Large Telescope Interferometer using a space-based astrometric reference frame. CERN Document Server astro-ph/9701197. 

VLT Very Large Telescope, the combination of four 8m diameter ground-based telescopes and a set of 1.8 m auxiliary telescopes at Paranal Observatory of the European Southern Observatory. The telescopes can be used individually or as an interferometer (VLTI) providing very high spatial resolution. 

Mirrors measuring 8.2 m in diameter (Fig. 4-13) were produced by the Schott Glaswerke for the Very Large Telescopes (VLT) of the European Southern Observatory (ESO). They are being installed in mirror telescopes at the observatory in La Sila, Chile. 

Zerodur can be supplied in the form of disks, rectangular blocks, prisms, rods, and cut pieces. Thick disks which are self-supporting can be produced with up to more than 4 m in diameter and with volumes of about 8 m (equivalent to 20 metric t). Thin menisci which are not self-supporting can also be produced up to masses of about 20 t the largest sizes produced so far were the 8.2 m menisci for the Very Large Telescope of the European Southern Observatory see Sect. 4.3.1. 

A new record will be achieved by the Very Large Telescope (VLT) of the ESO. In continuation of and using the New Technology , four telescopes of mirror diameters 8.2 m each will be installed on the Cerro Paranal in Chile. Together they will represent a useful mirror surface equating to that of a mirror of diameter 16 m. 

Fig. 4.64. One of four monolithic mirrors of diameter 8.2 m for the the Very Large Telescope of the ESO...

F. Merkle, M. Schneermann Das ESO Very Large Telescope , Sterne und Weltraum 9/86, 460-466, 25. Jahrg. 

ESO/VLT European Southern Observatory/Very Large Telescope SEVIRI Spinning Enhanced Visible and Infra-Red Imager SPOT Solar Patrol Observing Telescope ROSAT Roentgen Satellite... 

Fig. 2.4 The (3 Pictoris system in near infrared light. The faint reflected light radiation from the debris disc is revealed after a very careful subtraction of the much brighter stellar halo. The outer part of the image shows the dust disc, as observed in 1996 with the ADONIS instrument on the ESO 3.6 m telescope the inner part of the image has been obtained with the NACO instrument on the ESO Very Large Telescope. The newly detected source is more than 1,000 times fainter than (3 Pictoris, aligned with the disc, at a projected distance of eight times the Earth-Sun distance. Both parts of the image were obtained on ESO telescopes equipped with adaptive optics [30]...

Very large telescopes with multielement primary optics. Proposed sizes range up to 25 m for ground-based telescopes. Only a few multielement telescopes have actually been built. 

The already mentioned NICMOS instrument on the Hubble Space telescope was used to measure a sample of KBOs (84 objects were selected) photometrically and first results were presented by Noll et al 2005 [250]. Stellar occultations provide another effective means to study these objects (see Roques and Doressoundiram, 2005 [281]). These observations were made with the WHT in La Palma and with the Very Large Telescope of ESO. The influence of a stellar fly-by encounter on the KBOs was investigated by Kobayashi, Ida, and Tanaka, 2005 [187]. 

SIMCO, A SIMULATION SOFTWARE FOR CONICA, the COUDE NIR CAMERA FOR THE VERY LARGE TELESCOPE... 

Claes, P. 1993, The significance for IR-astronomy of ESO s Very Large Telescope In-... 

To equip instruments to be mounted on very large telescopes sudi as the European VLT at ESO, manufacture of new arrays has been undertaken and is currently under way at CEA-LETI-LIR. These new arrays will have a 128x192 format and will present the outstanding essential feature that their storage capacity will be able to be changed according to observation conditions (2 capacities will be implemented in the pixel). 

---