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TPF Ancillary Science 2/04 Marc Kuchner

TPF Ancillary Science 2/04 Marc Kuchner. TPF vs. LISA, SPIRIT, SUVO, etc. Interferometer vs Coronagraph. TPF: 20 milliarcseconds, 0.5 microns 30-m ground: 20 miilarcseconds, 2 microns JWST: 100 milliarcseconds, 2-40 microns TPF: 20 milliarcseconds, 10 microns

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TPF Ancillary Science 2/04 Marc Kuchner

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  1. TPF Ancillary Science 2/04 Marc Kuchner

  2. TPF vs. LISA, SPIRIT, SUVO, etc. Interferometer vs Coronagraph

  3. 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

  4. IRAM Plateau de Bure 1.3 mm arcsec Vega arcsec

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

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

  7. tpf-swg-ancillary@s383.jpl.nasa.gov Marc Kuchner Bill Danchi Sara Seager David Spergel 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

  8. Bill Danchi Rene Liseau Jonathan I. Lunine Kenneth J. Johnston Doug Lin Charley Noecker Kilston, Steve Marc Kuchner Sara Seager David Spergel Bill Sparks Huub Rottgering Tony Hull Karl Stapelfeldt Sally Heap Eric Gaidos Ted von Hippel David Spergel David Leisawitz Alan Dressler Michael Strauss

  9. Ancillary Science Website: http://www.astro.princeton.edu/~mkuchner/ancillarysci.html Ancillary Science with TPF Send comments to Marc Kuchner Base Missions IR: 6.5-13 microns, R=20 Tall four apertures, 3.2 m diameter each spaced along a 36m array at 0,9, 27, 36 m. Grande four apertures, 4.0 m diameter each, unevenly spaced along a 70 m arraym expandable to 150m Visible: 0.5-0.8 microns, R=70 Tall 3.5 by 6.5 m Grande 3.5 by 14m segmented array References and Links "The Future of High Angular Resolution Star and Planet Formation Science in the Optical/Infrared" by Lynne A. Hillenbrand astro-ph/0312188 "Hubble's Science Legacy: Future Optical/UV Astronomy from Space" Ken Sembach and Chris Blades, eds. Science Case for AURA GSMT (30 meter ground-based optical telescope) Meetings Workshop on Science with Very Large Space Telescopes Feb 23-24, Space Telescope Register now!

  10. I) Planetary Science; Comparative Planetology A) Non-inhabitable planets Sara Seager, Jonathan Lunine B) Planets around non-FGK stars: A stars, M stars, Brown Dwarfs, White Dwarfs Ted von Hippel C) Planet Formation/Disk Science Debris Disks, YSO Disks + Jets Karl Stapelfeldt, Rene Liseau, MJK D) Solar System Science: Johnathan Lunine

  11. II) Non-Planetary Science • Star formation, pre-main sequence binaries Doug Lin • B) Cosmology • Dark Matter, Dark Energy, Galaxy Formation • and Evolution, First Generation of Stars • David Spergel, Doug Lin • C) AGN, QSOs • Bill Sparks, Huub Rottergering • D) AGBs and massive stars • Bill Danchi, Steve Kilston

  12. III) Modificaions to TPF Tony Hull, Charlie Noecker Wide-Field Imaging David Leisawitz (IR), Thangasamy Velusamy (IR) B) High-Resolution Spectroscopy Mid IR--R=100,000? C) Astrometry: Ken Johnston 100 microarcsec of faint objects-- Distance to the Hulse-Taylor binary pulsar Isolated neutron stars at 24-25 magnitude

  13. Optical “Tall” TPF + “Grande” TPF IR “Tall” TPF + “Grande” TPF Plain TPF Tweaked TPF Modified TPF (1 new instrument)

  14. HIGHLIGHTS

  15. Non-Inhabitable Small planets Key Questions: How do terrestrial planets form? What is the origin of water on the Earth? What is the relationship between small-body belts and terrestrial planet formation? How common are big moons and rings? What are the compositions of extrasolar terrestrial planets? What is the origin of terrestrial planet spins?

  16. Tools: The Rest of the Biomarkers! CO2, CH4, Rayleigh scattering, photosynthetic pigments (visible) CO2, CH4, N2O (IR), sulfur compounds Silicate spectroscopy Find water planets and dry planets. Extended Spectroscopic Capabilities: the bigger the range, the better! Dynamics: Measure eccentricity/inclination/semimajor axis distribution. Orbit Determination Phase Curves: Rings and moons Polarimetry: cloud compositions Correlate planets and exozodiacal clouds.

  17. Giant Planet Key Questions: What creates the range of metallicities in giant planets? Can giant planets form by gas instability? How do giant planets get their eccentricities? What is the role of planet migration? What is the relationship between giant planets and small body belts? What is origin of giant planet spins? Why is there a brown dwarf desert?

  18. Karkoschka 1994 wavelength (nanometers)

  19. Karkoschka 1994

  20. OWA: 2.5 arcsec, Jupiter zone=5-10 L1/2 AU

  21. Tools: Study RV+SIM Exo-Jupiters Extended Spectroscopic Capabilities: the bigger the range, the better! High Resolution Spectrograph: Transit Observations Follow Up Kepler Discoveries Test mass vs luminosity relations and date systems using SIM Masses

  22. Planets around: A stars, M stars, O+B stars?: more statistics. How does the process of planet formation change with stellar mass? White Dwarfs Much less contrast needed in IR photon noise limited--look in closer (1 AU) than JWST, or more distant objects. Faster photometry---time resolved? What is the future of the solar system? Red Giants: Is is stellar mass loss sudden or adiabatic? Do planets create asymmetries in PN?

  23. Key YSO Questions: Where does the gas go? Do planets open gaps? What is disk temperature and chemistry in the planet-forming region? Do disks become self-shadowed? What forms jets? Find and image new disks. Only 10-20% of sources with IR excess and extended CO emission show disks that HST could see in scattered light. Study disks around brown dwarfs. ALMA takes days to get to 100 zodis!

  24. Study Disk Chemistry Many IR lines not accessible to ALMA. Silicate emission feature 10 microns. H2 emission (IR) 17microns H2O CO CO2 Map dissacociation regions and photoionization regions that generate disk winds that remove the disks. High-resolution IR spectrograph + wide-field imaging. OTHER IDEAS: Resolve closely separated PMS binaries Astrometry of PMS binaries that are too cool or embedded for SIM. IR TPF at 2 microns? Study colimation of jets--X winds? Or disk winds? Very high resolution Optical.

  25. Solar System: Chemistry Comets and in planetary atmospheres: isotopic abundances resolved high-res spectroscopy at Kuiper Belt few x 100 km resolution at Kuiper Belt Hi res IR spectrograph---compare to SOFIA Optical spectroscopy, phase curves, and transit curves of faint objects: KBOs, Comet Cores, NEOs. (few x better resolution than ground-based) Resolve Binary KBOs Follow up LSST and MACHO discoveries.

  26. AGN Key Questions: How do massive black holes form and evolve? What is relationship between galaxies and BHs? IR: Mapping of dusty torii to z=7 detailed kinematics of torii R=2000 Optical: morphology of quasar host galaxies, z=0.2-2 higher contrast and resolutionthan JWST polarimetry of host galaxies: emission physics light echoes gives you distances

  27. Cosmology Key questions: 1) What is Dark Matter? 2) What is Dark Energy? Cluster lensing: Distribution of dark matter Distances: Cepheids (to 3 times farther than HST) Surface brightness fluctuations Measure H0 to 2% = Measurement of w (when combined with WMAP data) Optical: Wide Field of View+Astrometry!

  28. 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)

  29. 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

  30. 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

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

  32. Meeting: Tomorrow and Friday Space Telescope The Science Potential of a 10-30m UV/Optical Space Telescope http://www.stsci.edu/stsci/meetings/vlst/

  33. Resolution vs. Collecting Area Log10 (Collecting Area (sq.m)) Long Wavelength Limit (warm telescope)  3.2mm  1.6mm Log10 (Angular Resolution(”)) Spitzer @ l= 3.5mm Circular Apertures  0.8mm  0.4mm TPF-C base band 0.5-0.8mm  0.2mm JWST @ l= 2.0mm HST @ l= 0.4mm Short Wavelength Limit (coatings) 8m 4m 16m

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