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
Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.
Coronagraph: 0.5-0.8 microns
6.5 x 3 m
8 x 7 m
Interferometer: 6.5-13 microns
70-150m baseline, 4x4m
6-fold deployed structure
Ted von Hippel
Jonathan I. Lunine
Kenneth J. Johnston
30-m ground: 20 miilarcseconds, 2 microns
JWST: 100 milliarcseconds, 2-40 microns
TPF: 20 milliarcseconds, 10 microns
ALMA: 30 milliarcseconds, 300+ microns
Accurate Pointing (Boresite)
Option for More Instruments
e.g. hi-res spectrograph
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?
High Resolution Spectrograph
Wide Field Camera
Your Idea Here
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
focusWide Field Imaging
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)
Type II Quasars
Type I Quasars
(broad + narrow)
Near Earth Objects
Supernova Remnants in Virgo
GRB light echoes
Prepare report for presentation