Europe's Quest for the Universe - Laboratoires de Recherche

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ESO, La Silla, the 3.6 m Telescope 33 To detect the faint extraterrestrial sources, rapid switching techniques are needed in which the source is compared repeatedly with the “empty” sky. Because the atmosphere is rather variable, the switching between source and background has to be done dozens of times per second. Moreover, to reduce the background due to the infrared instrument itself, the detector and the critical optical elements have to be cooled to temperatures of a few K above absolute zero. Under the leadership of Alan Moorwood some infrared photometers were constructed for the 3.6-m telescope, followed in 1985 by an advanced cryogenic infrared spectrograph based on a small solid state detector array. As a result of the new instrumentation, the ESO 3.6-m / CAT combination was changed from a late-comer of the previous era into a fully up-todate combination. Instead of having to adapt photographic instruments to the new world, the instruments were designed from the beginning for the new detectors. Of course, the CAT remained a small telescope (1.4-m) and only relatively bright stars could be observed. Later, when efficient optical fibers became available, the coudé échelle spectrograph was coupled directly to the 3.6-m telescope and the CAT was closed down. Later additional instrumentation for the 3.6-m telescope would also include a multiple object spectrograph, allowing numerous objects to be observed at the same time, an adaptive optics imager (chapter VII) and a very precise radial velocity meter for planet detection (chapter XV). The La Silla Telescope Park and its cost At the end of 1971, construction of the 3.6-m telescope was still to begin, but at La Silla smaller telescopes had been springing up like mushrooms: a 1.5-m for spectroscopy, a 1-m for photometry, four 40–60 cm telescopes (partly in cooperation with institutes in the ESO countries) and a 1-m Schmidt telescope for photographing the whole southern sky. While these telescopes could certainly be justified scientifically and politically, the multiplicity of efforts may well have been detrimental for the progress of the main project, the 3.6-m telescope. Instrumentation for these telescopes also represented much effort. Although this was supposed to create valuable experience for the instrumentation of the 3.6-m telescope, hardly anything had been built for the latter when it was completed. Later a 2.2-m and a 1.5-m telescope were also added (Figure II, 3). All these activities came at a considerable cost. Blaauw 7) estimates that when the 3.6-m telescope became operational, the (3.6-m) Telescope Project Division had been responsible for only 28% of the cumulative ESO expenditure. While to this should be added the part of the infrastructure needed for the 3.6-m at La Silla, it shows that the cost of the smaller telescopes was far from negligible. Later in the 1986 ESO Annual Report, I presented an
34 Europe’s quest for the Universe analysis of the operational cost of the various telescopes at La Silla. Costs incurred in Garching were appropriately apportioned, including those for instrumental development, Visiting Astronomers and administrative overhead. During 1986 the cost for the 3.6-m telescope came to 4.6 M€ Figure II, 3. La Silla in 2003. In the lower part are offices and dormitories. Then come some small telescopes, followed by the 1.5-m, the GPO, the 1-m, the 1.5-m DK, the 2.2-m and the 1-m Schmidt. Higher up are the NTT and the 3.6-m/CAT and to the right the 15-m SEST. Near the bottom is the 15-m inflatable dome for VLT experiments.
Page 1 and 2: Europe's Quest for the Universe Lod
Page 3 and 4: Cover: THE VLT Array on the Paranal
Page 6 and 7: Preface What a magnificent title,
Page 8: Acknowledgements First of all I wou
Page 11 and 12: 8 Europe’s quest for the Universe
Page 13 and 14: 10 Europe’s quest for the Univers
Page 28 and 29: II. ESO, La Silla, the 3.6-m Telesc
Page 30 and 31: ESO, La Silla, the 3.6 m Telescope
Page 46 and 47: III. Origin of the VLT Project; The
Page 48 and 49: Origin of the VLT Project; The NTT
Page 62 and 63: IV. Technological, Financial and Sc
Page 64 and 65: Technological, Financial and Scient
Page 72 and 73: V. Construction of the VLT Could we
Page 74 and 75: Construction of the VLT 71 contract
Page 76 and 77: Construction of the VLT 73 of the p
Page 78 and 79: Construction of the VLT 75 Figure V
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Construction of the VLT 83 telescop
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Construction of the VLT 85 Supporte
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88 Europe’s quest for the Univers
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Figure VI, 3. Map of northern Chile
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100 Europe’s quest for the Univer
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VII. The VLT Observatory: Adaptive
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The VLT Observatory 111 effects. Ho
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The VLT Observatory 113 member coun
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The VLT Observatory 115 Table VII,
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The VLT Observatory 117 the NTT and
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Interferometry The VLT Observatory
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The VLT Observatory 121 Figure VII,
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VIII. Ground and Space Based Optica
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Ground and Space Based Optical Tele
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HST and VLT Ground and Space Based
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HST and VLT are complementary. Beca
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seeing conditions prevail; the latt
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IX. Radio Astronomy; ALMA and SKA A
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Radio Astronomy; ALMA and SKA 141 a
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Radio Astronomy; ALMA and SKA 143 w
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at Jodrell Bank. Baselines range up
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science remains compelling. We stil
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Radio Astronomy; ALMA and SKA 149 A
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Radio Astronomy; ALMA and SKA 151 w
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ALMA Radio Astronomy; ALMA and SKA
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Radio Astronomy; ALMA and SKA 155 F
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Radio Astronomy; ALMA and SKA 157 S
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Radio Astronomy; ALMA and SKA 159 o
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CLUSTER DOUBLE STAR 1 9 9 0 2 0 0 0
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XIII. European Space Missions: The
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European Space Missions: The Sun an
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XIV. Astroparticles and Gravitation
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Log +5 F (>E) 0 -5 -10 -15 Astropar
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Astroparticles and Gravitational Wa
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XV. Looking for Planets and Life in
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Looking for Planets and Life in the
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XIX. Epilogue …entre européens d
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Introduction 1) ESO, Garching, 1991
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Chapter V; Most notes refer to docu
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27) E. Carrasco, R. Avila, A. Carra
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NASA (-1/2 “research”) ESA × 1
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Missions”. An excellent review on
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Acronyms and Concepts - A - A Austr
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CDS 1. Coronal Diagnostic Spectrome
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EGRET Energetic Gamma-Ray Experimen
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HALCA Japanese satellite with radio
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La Palma island of the Canary Islan
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O2 O3 - O - Odin molecular oxygen o
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SN supernova SNO Sudbury Neutrino O
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- W - Wetzel site in Germany WFPC W
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Photo credits p. 10 ESO I 1 ESO 2 J
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