...world

It may be useful to note that the VLT is just one case of the extraordinary development of new large astronomical telescopes which is now taking place. At the time of writing this report, there are, beside the VLT, several other ongoing projects:  

• The first Keck 10-m telescope is completed on Hawaii island and in the tuning phase, while a twin telescope is being fabricated.
• The american Gemini project for two identical 8-m telescopes for different sites (Hawaii and Chile)  
• The japanese Subaru 8-m telescope project, also to be located on Hawaii.
• The american privately funded Magellan project for a 6-m telescope in Chile.

Other large telescope projects are still in an earlier planning and development phase, such as the Columbus project for a telescope with a twin "binocular" mount with two 8-m mirrors, and several national projects in Germany, Spain and Great Britain.

...observation

105#105 is often called airmass in the astronomical jargon.

...GEMINI

See footnote at page .

...contributions

Including the total seeing contribution.

...designs

The 2.2-m building includes a cooled floor while the 3.6-m now has an active air cooling system in the dome.

...base

The data base is freely available on the Internet World Wide Web at the address http://lw10.ls.eso.org/lasilla/seeing2/seeingmain.html .

...SuperIMAQ

The SuperIMAQ program [ESO] was written by Ph. Diericks of ESO to compute the PSF and all image quality parameters of a telescope mirror, accounting for all diffraction effects, surface wavefront errors and seeing by the method described in [Diericks].

...seeing

Mirror seeing will be treated extensively in section .

...mirror

The wavefront of light is reflected by the primary mirror toward the secondary mirror and then again downwards to an instrument focus (see fig. at page ).

...monitor

The DIMM was introduced at page .

...telescope

see footnote at page .

...DIMM

In that case the DIMM was located 2 meters above the ground, 40 m south (downwind) of the NTT.

...twice

See fig.

...textbook

See for instance [Incoprera], p. 506.

...performance

We recall that seeing contributions along the line of sight add up with the power 5/3, while all other contributions add quadratically to the total seeing (see equations () and ()).

...conditions:

The scaling of the B factor takes account of the lower atmospheric pressure of an astronomical mountain site: here 770 mb with respect to 1000 mb for the wind tunnel.

...scale

One may recall that turbulence frequencies are increased inversely to the geometrical scale: as a comparison the velocity spectra are generally measured up to 200 Hz.

...seeing

This is the case at the Paranal site of the VLT ([Sarazin 90]).

...temperature

The mirror cooling system should ideally allow the mirror to remain always slightly colder than ambient air, a limit being given by the need to avoid water condensation. During the observations, the mirror can only be cooled from the back side and, because of its thermal inertia, there will be inevitably instances when the air temperature will drop during the night to a lower temperature than the front surface.

...noise

The measurements 115, 116 and 117 have been done in the closed inflatable dome. Therefore, they measured the noise of the pressure sensors.

Lorenzo Zago, zago@elgc.epfl.ch, Mon Nov 6 23:33:14 GMT+0100 1995