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TPF/Darwin

TPF/Darwin. Terrestrial Planet Finder Coronagraph: 0.5-0.8 microns 6.5 x 3 m 8 x 7 m Interferometer: 6.5-13 microns 36m, 4x3.2m 70-150m baseline, 4x4m. Structurally-Connected Interferometer. Dual-chopped Bracewell 36 m array Four apertures, 3.2 m diameter

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TPF/Darwin

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  1. TPF/Darwin

  2. Terrestrial Planet Finder Coronagraph: 0.5-0.8 microns 6.5 x 3 m 8 x 7 m Interferometer: 6.5-13 microns 36m, 4x3.2m 70-150m baseline, 4x4m

  3. Structurally-Connected Interferometer • Dual-chopped Bracewell • 36 m array • Four apertures, 3.2 m diameter • -18, -9, +9, +18 m positions • +/- 45 degrees sky coverage • Delta IV-Heavy, 22.4 m fairing • L2 Orbit Star planet 3.2m telescopes 6-fold deployed structure Sunshield Spacecraft

  4. Formation-Flying Interferometer • Dual-chopped Bracewell • Array size: 70 to 150 m • Four apertures, 4.0 m diameter • +/- 45 degrees sky coverage • Delta IV-Heavy, 22.4 m fairing • L2 Orbit Four Collectors Combiner 4.0m telescopes 16m sunshield

  5. TPF Ancillary Science

  6. tpf-swg-ancillary@s383.jpl.nasa.gov Marc Kuchner Bill Danchi Sara Seager Bill Sparks Huub Rottgering Ted von Hippel Doug Lin Rene Liseau Jonathan I. Lunine Kenneth J. Johnston Tony Hull Karl Stapelfeldt Charley Noecker Kilston, Steve Sally Heap Eric Gaidos David Spergel David Leisawitz Alan Dressler Michael Strauss Jeff Valenti

  7. TPF: 20 milliarcseconds, 0.5 microns 30-m ground: 20 miilarcseconds, 2 microns JWST: 100 milliarcseconds, 2-40 microns TPF: 20 milliarcseconds, 10 microns ALMA: 30 milliarcseconds, 300+ microns

  8. IRAM Plateau de Bure 1.3 mm arcsec Vega arcsec

  9. Kuchner & Holman 2003

  10. Optical TPF Advantages: High Contrast Accurate Pointing (Boresite) and Figure Stability Optical Wavelengths

  11. IR TPF Advantages (vs. JWST): High Contrast Stability Angular Resolution Option for More Instruments e.g. hi-res spectrograph

  12. Giant Planets Can giant planets form by gas instability? How do giant planets get their eccentricities? What is the role of planet migration? How did the asteroid belt form? What is origin of giant planet spins? Why is there a brown dwarf desert? How do ice giants form? Karkoschka 1994

  13. Opportunity to add ~1 instrument: High Resolution Spectrograph Wide Field Camera IFU Polarimeter Your Idea Here

  14. Ancillary optics for wide field work focal reducer wide field corrector Consider FFOV 0.1 1.4x focal reduction Hypothetical design #2, 0.1 FFOV 16 arrays => 262 Mpixel 0.3 x 0.4 m pick-off mirror 1-2 pixels per Airy disk diameter 4048 x 4048 13.5 micron pixels Coronagraph focus Wide Field Imaging Ancillary camera

  15. The most distant observed object is lensed through Abell 2218. Objects at z = 5.6 have been found, corresponding to 13.4 billion light years (4.1 Gpc)

  16. 100 micro arcsec astrometry

  17. Seyfert 2 Type II Quasars (narrow line) Seyfert 1 Type I Quasars (broad + narrow) Blazars, BL Lacs, Optically Violent Variables

  18. Things we could resolve at K-band with interferometer (1 millarcseconds): Near Earth Objects Comet nuclei X-ray binaries Supergiants Planetary Nebulae Supernova Remnants in Virgo GRB light echoes

  19. TPF Ancillary Science Website: http://www.astro.princeton.edu/~mkuchner/ancillarysci.html

  20. TPF Ancillary Science Meeting Princeton University April 14-15 Prepare report for presentation to CAA

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