The VLT Interferometer - ESO

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2 CHAPTER 1. INTRODUCTION
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Figure 1.1: The VLT in context of the Development of Optical Astronomical
Telescopes since their Invention by Lippershey (German-Dutch) and first Use
by Galileo (Italian)
for the very high angular resolution (milliarcsec and better) combined with the
high sensitivity which results from interferometric arrays using very large 8
meter telescopes. In doing so ESO follows in the footsteps of radio astronomy
which chose image synthesis techniques done with interferometric arrays three
decades ago as the means of obtaining very high angular resolution imaging. By
capitalizing on the refined image synthesis techniques developed since then in
radio astronomy, and by using the technical experience gained with the successful
implementation of optical interferometric arrays in recent years, ESO is now
well poised to go aggressively ahead with the definition, design and deployment
of the VLT Interferometer (VLTI). This is the goal which forms the basis of
this study. In achieving it, together with its high sensitivity, the VLT will place
European astronomy on the forefront of optical technological achievement and
scientific capability as optical astronomy enters the 21st century regaining the
lead which it held since the invention of the telescope but which it lost at the
beginning of this century. Figure 1.1 puts the VLT in this historical perspective.
The dominant emphasis in this report is on the definition and implelllelltntion
plan of the VLTI and not on its scientific utility, which was well covered
in earlier studies (eg VLT Report No.49, ESO 1986 Venice vvorkshop, VLT
Proposal). Chapters 2, 3 and 4 will describe the scientific, opto-mechanical
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