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Report by the ESA-ESO Working Group
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The working group membership was es
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3.2.2 The Darwin Ground-Based Precu
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Figure 1: Detection methods for ext
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those with masses between about 0.5
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Figure 2: Detection domains for met
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(c) Astrometric measurements do not
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Table 1: A summary of completed, op
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chemical composition of the primord
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Table 2: A summary of planned or op
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it passes behind the star. They arg
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shapes caused by extra-solar planet
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Table 3: A summary of completed, op
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ground requires simultaneous observ
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0.35 arcsec of the centre, i.e. muc
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ferential phase observations with a
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2.2 Space Observations: 2005-2015 I
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larger number of hot Jupiters would
Page 39 and 40: (Shao): this major SIM survey progr
Page 41 and 42: The planetary lensing events have a
Page 43 and 44: siting extra-solar planets are expe
Page 45 and 46: 2.3 Summary of Prospects 2005-2015
Page 47 and 48: 3 The Period 2015-2025 3.1 Ground O
Page 49 and 50: Table 6: Magnitudes and separations
Page 51 and 52: per star in order to sample the (po
Page 53 and 54: een produced, diffraction effects c
Page 55 and 56: 3.2 Space Observations: 2015-2025 T
Page 57 and 58: Table 8: Detection capabilities: Ea
Page 59 and 60: 3.2.3 Terrestrial Planet Finder (TP
Page 61 and 62: ∼ 5 × 10 5 m, or 1.5 × 10 −4
Page 63 and 64: of Earth-like planets in general, a
Page 66 and 67: 4 The Role of ESO and ESA Facilitie
Page 68 and 69: Figure 7: Links between detection m
Page 70 and 71: 4.2.3 Summary of Follow-Up Faciliti
Page 72 and 73: 4.4 Astrophysical Characterisation
Page 74 and 75: Without any further mission dedicat
Page 76 and 77: and their suitability for supportin
Page 78 and 79: overlap of public and research inte
Page 80 and 81: 2.4. Evaluate observation time for
Page 82 and 83: A Space Precursors: Interferometers
Page 84 and 85: B Beyond 2025: Life Finder and Plan
Page 86 and 87: C ESO 1997 Working Group on Extra-S
Page 88 and 89: Table 10: ESO Working Group 1997: R
Page 92 and 93: Pedretti, E., Labeyrie, A., Arnold,
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