tpf/darwin. terrestrial planet finder coronagraph: 0.5-0.8 microns 6.5 x 3 m 8 x 7 m interferometer:...
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TPF/Darwin
Terrestrial Planet Finder
Coronagraph: 0.5-0.8 microns6.5 x 3 m 8 x 7 m
Interferometer: 6.5-13 microns36m, 4x3.2m70-150m baseline, 4x4m
Structurally-Connected Interferometer
Sunshield
• 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
6-fold deployed structure
Spacecraft
3.2m telescopes
Starplanet
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
4.0mtelescopes
16msunshield
TPF Ancillary Science
Marc KuchnerBill 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 NoeckerKilston, SteveSally HeapEric Gaidos
David SpergelDavid LeisawitzAlan DresslerMichael StraussJeff Valenti
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
Vegaarcsec
arcsec
IRAM Plateau de Bure 1.3 mm
Kuchner &Holman 2003
Optical TPF Advantages:
High Contrast
Accurate Pointing (Boresite)and Figure
Stability
Optical Wavelengths
IR TPF Advantages (vs. JWST):
High Contrast
Stability
Angular Resolution
Option for More Instrumentse.g. hi-res spectrograph
Karkoschka 1994
Giant PlanetsCan 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?
Opportunity to add ~1 instrument:
High Resolution SpectrographWide Field CameraIFUPolarimeterYour Idea Here
Wide Field Imaging
• 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
Coronagraphfocus
Ancillary camera
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)
100 micro arcsec astrometry
Blazars,BL Lacs,Optically ViolentVariables
Seyfert 1Type I Quasars(broad + narrow)
Seyfert 2Type II Quasars(narrow line)
Things we could resolve at K-band with interferometer(1 millarcseconds):
Near Earth ObjectsComet nucleiX-ray binariesSupergiantsPlanetary NebulaeSupernova Remnants in VirgoGRB light echoes
TPF Ancillary Science Website:
http://www.astro.princeton.edu/~mkuchner/ancillarysci.html
TPF Ancillary Science Meeting
Princeton UniversityApril 14-15
Prepare report for presentationto CAA