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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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slide2

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
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

formation flying interferometer

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

slide8

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

slide12

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

slide14

Kuchner &

Holman 2003

slide15

Optical TPF Advantages:

High Contrast

Accurate Pointing (Boresite)

and Figure

Stability

Optical Wavelengths

slide16

IR TPF Advantages (vs. JWST):

High Contrast

Stability

Angular Resolution

Option for More Instruments

e.g. hi-res spectrograph

slide17

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

slide18

Opportunity to add ~1 instrument:

High Resolution Spectrograph

Wide Field Camera

IFU

Polarimeter

Your 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

Coronagraph

focus

Wide Field Imaging

Ancillary

camera

slide20

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)

slide22

Seyfert 2

Type II Quasars

(narrow line)

Seyfert 1

Type I Quasars

(broad + narrow)

Blazars,

BL Lacs,

Optically Violent

Variables

slide23

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

slide24

TPF Ancillary Science Website:

http://www.astro.princeton.edu/~mkuchner/ancillarysci.html

slide25

TPF Ancillary Science Meeting

Princeton University

April 14-15

Prepare report for presentation

to CAA