# Presentation: 582454

## 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

## Slide 3

## 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

- Star

- planet

**Notes:**
Achieve core science by (list)
Measurement performed by rotating; phase chopping between the two bracewell pairs maintains the null, moves the rest of the pattern around asymmetrically on the sky, and helps to distinguish the planet from other background sources such as EZ and instrument instabilities
IWA of 43 mas – first peak set a factor of 1.3 inside the IHZ (goes with completeness)
Error budget:  0.1% amplitude control, 1 nm pathlength control, 0.8x10-6 null at 10 um

## 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

**Notes:**
Curt how big are the sunshields – and how might I relate this array size.  Min array size = 3 (sunsh.+ min tip)
= 3*(16+10) = 78m.  What about the root 2 on sunshield?
Launch mass major concern

## TPF Ancillary Science   

## Slide 7

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

- _[tpf-swg-ancillary@s383.jpl.nasa.gov](mailto: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

## Slide 9

## Slide 10

## Slide 11

## 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

## Vega

- arcsec

- 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 Instruments
- e.g. hi-res spectrograph

## Karkoschka 1994

**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?

## 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

- 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)

**Notes:**
Hubble Space Telescope image of the galaxy cluster "Abell 2218" used by Ellis and collaborators in their systematic search for intrinsically faint distant star-forming systems. The image pair (inset) represents the magnified result of a single source gravitationally magnified more than 30 times by Abell 2218 and viewed at a distance of 13.4 billion light years. The intriguing object contains only a few million stars, far fewer than a mature galaxy and Ellis and coworkers believe it is very young. Such young star-forming systems of low mass at early cosmic times are thought to assemble to form the mature galaxies we see today. 

## 100 micro arcsec astrometry

## Blazars,

- BL Lacs,
- Optically Violent
- Variables

- Seyfert 1
- Type I Quasars
- (broad + narrow)

- Seyfert 2
- Type II Quasars
- (narrow line)

## 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

## TPF Ancillary Science Website:

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

## TPF Ancillary Science Meeting

- Princeton University
- April 14-15
- Prepare report for presentation
- to CAA