Titlebook: Infrared Space Interferometry: Astrophysics & the Study of Earth-Like Planets; Proceedings of a Wor C. Eiroa,A. Alberdi,C. J. Schalinski Co

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Molecular Gas Production in the , Pictoris DiskModel calculations suggest the SiO production rate due to grain-grain collisions to be higher by orders of magnitude. However, because of insufficient angular resolution the predicted SiO line emission escaped detection. A new generation of interferometers is required to test the Keplerian disk hypo

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Planets in CM Draconis: A Multi-Site Photometric Searchy companions with more than ～3 Earth radii should produce detectable occultations at the accuracy of our measurements. The observations started in spring 1994 and are still going on. Eight observatories have participated so far: Haute Provence (France), Lick (USA), La Palma (Spain), Rochester (USA),

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Epicurus was Right: Other Worlds Exist! the discovery of 51 Peg B, five planetary companions have been detected by radial velocity techniques. The unexpected orbital elements of most of these jovian planets give a first evidence of the diversity of planetary systems which is still far to be fully understood.

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Array Configurations to Detect and Characterize Extrasolar Planets with a Space Infrared Interferomearacterize extrasolar planets. Three main constrains can be identified: the interferometer must provide a very strong suppression of the starlight, a good spectral coverage (from 7 to 18 microns) with a fixed baseline, and be able to clearly distinguish planets from local dust disc emission. We revi

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Ground-Based Optical/IR Long Baseline Interferometryometry is briefly reviewed with emphasis on the scientific objectives that can be expected to be reached in the near future with this technique. It is shown that, if everything goes according to plan, extensive capabilities in this field will be available to the astronomical community by ～ 2005. In

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Infrared Interferometry with the VLTIen to the European community at the beginning of the next century. The baseline plan for the VLTI (see the reports by the ESO VLT Interferometer Panel, 1989 and 1992) includes combination of the four 8 m telescopes and a number of 2 m class auxiliary telescopes providing better coverage of the . pla

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Infrared Interferometry of Active Galaxiestheir host galaxies. When these devices become operational, they will tell us how quasars generate infrared light and will clarify the relationships between the powerful black-hole engines at the centers of galaxies and the surrounding bursts of star formation.

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