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• Solar neighborhood is sparsely populated – Fraction of stars with Earths (in habitable zone) unknown – Unknown how far we need to look to ensure success – Surveying substantial number of stars means looking to ~15 pc Sensitivity (relatively easy) • Detection in hours spectroscopy in days. – Integration time ∝ (distance/diameter) 4 – Need 12 m 2 of collecting area (>4 m) for star at ~10 pc • Angular resolution (hard) – 100 mas is enough to see ~25 stars, but requires >4 m coronagraph or >20 m interferometer – Baseline/aperture ∝ distance • Starlight suppression (hard to very hard) – 10 -6 in the mid-IR – 10 -9 in the visible/near-IR Four Hard Things About TPF >10 9 >10 6
The Challenge of Angular Resolution • Coronagraphs at >3λ/D • Interferometers at > 1 λ/B Cost ($$), Launch Date + 10 µm, 28 m Coronagraph
Page 1 and 2: The Search for (Habitable) Planets
Page 3 and 4: Organic Chemistry Ubiquitous: Comet
Page 5 and 6: …and distant galaxies • Polycyc
Page 7 and 8: Earth’s Gases With And Without Li
Page 9 and 10: Star Formation & Protoplanetary Dis
Page 11 and 12: SIRTF Observations of Disks •NASA
Page 13 and 14: • Observations at 24, 70, 160 µm
Page 15 and 16: Transit Determines Planet’s Prope
Page 17 and 18: • Make astrometric census of plan
Page 19: Search for Planets Around Young Sta
Page 23 and 24: TPF Science Requirements-I • Dete
Page 25 and 26: TPF Candidate Architectures • Vis
Page 27 and 28: Visible Light Planet Detection •
Page 29 and 30: IR Interferometer Goal Earth at 10
Page 31 and 32: Selection of Final Architecture Jun
Page 33: Collaboration on TPF/Darwin • Str

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