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

tpf-swg-ancillary@s383.jpl.nasa.gov

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