# Presentation: 188860

## TPF Ancillary Science   2/04

- Marc Kuchner

## TPF vs.  LISA, SPIRIT, SUVO, etc.

- Interferometer vs Coronagraph

## Slide 3

## Slide 4

## Slide 5

## 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

## 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

## 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
- David Spergel
- 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

## Marc Kuchner

- Sara Seager
- David Spergel
- Bill Sparks
- Huub Rottgering
- Tony Hull
- Karl Stapelfeldt
- Sally Heap
- Eric Gaidos
- Ted von Hippel
- David Spergel
- David Leisawitz
- Alan Dressler
- Michael Strauss

- Bill Danchi
- Rene Liseau
- Jonathan I. Lunine
- Kenneth J. Johnston
- Doug Lin
- Charley Noecker
- Kilston, Steve

## Ancillary Science Website:

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

- Ancillary Science with TPF
- Send comments to _Marc Kuchner _
-  	Base Missions
- 	IR: 6.5-13 microns, R=20
- 	Tall
- four apertures,
- 3.2 m diameter each spaced along a 36m array at 0,9, 27, 36 m.
- 	Grande
- four apertures,
- 4.0 m diameter each, unevenly spaced along a 70 m arraym expandable to 150m
- 	Visible: 0.5-0.8 microns, R=70
- 	Tall
- 3.5 by 6.5 m
- 	Grande
- 3.5 by 14m segmented array
-  	References and Links
- "The Future of High Angular Resolution Star and Planet Formation Science in the Optical/Infrared" by Lynne A. Hillenbrand
- _astro-ph/0312188_
- "Hubble's Science Legacy: Future Optical/UV Astronomy from Space" Ken Sembach and Chris Blades, eds.
- _Science Case for AURA GSMT (30 meter ground-based optical telescope)_
-  	Meetings
- Workshop on Science with Very Large Space Telescopes
- Feb 23-24, Space Telescope
- _Register now!_

## I) Planetary Science; Comparative Planetology

- A) Non-inhabitable planets
**Sara Seager, Jonathan Lunine**
- B) Planets around non-FGK stars:
- A stars, M stars, Brown Dwarfs, White Dwarfs
**Ted von Hippel**
- C) Planet Formation/Disk Science
-  Debris Disks, YSO Disks + Jets
**Karl Stapelfeldt, Rene Liseau, MJK**
- D) Solar System Science:
**Johnathan Lunine**

## II)	Non-Planetary Science

- Star formation, pre-main sequence binaries
**Doug Lin**
- B) Cosmology
- Dark Matter, Dark Energy, Galaxy Formation
- and Evolution, First Generation of Stars
**David Spergel, Doug Lin**
- C) AGN, QSOs
**Bill Sparks, Huub Rottergering**
- D) AGBs and massive stars
**Bill Danchi, Steve Kilston**

## III)  Modificaions to TPF

**Tony Hull, Charlie Noecker**
- Wide-Field Imaging
**David Leisawitz (IR), ****Thangasamy Velusamy (IR)**
- B) High-Resolution Spectroscopy
- Mid IR--R=100,000?
- C) Astrometry:  **Ken Johnston**
- 100 microarcsec of faint objects--
- Distance to the Hulse-Taylor binary pulsar
- Isolated neutron stars at 24-25 magnitude

## Optical   

- “Tall” TPF + “Grande” TPF
- IR
- “Tall” TPF + “Grande” TPF
- Plain TPF
- Tweaked TPF
- Modified TPF (1 new instrument)

## HIGHLIGHTS

## Non-Inhabitable Small planets

- Key Questions:
- How do terrestrial planets form?
- What is the origin of water on the Earth?
- What is the relationship between small-body
- belts and terrestrial planet formation?
- How common are big moons and rings?
- What are the compositions of extrasolar
- terrestrial planets?
- What is the origin of terrestrial planet spins?

## Tools:

- The Rest of the Biomarkers!
- CO2, CH4, Rayleigh scattering,
- photosynthetic pigments (visible)
- CO2, CH4, N2O (IR),  sulfur compounds
- Silicate spectroscopy
- Find water planets and dry planets.
**Extended Spectroscopic Capabilities:**
**the bigger the range, the better!**
- Dynamics: Measure eccentricity/inclination/semimajor
- axis distribution.  **Orbit Determination**
- Phase Curves: Rings and moons
- Polarimetry: cloud compositions
- Correlate planets and exozodiacal clouds.

## Giant Planet Key Questions:

- What creates the range of metallicities in giant planets?
- Can giant planets form by gas instability?
- How do giant planets get their eccentricities?
- What is the role of planet migration?
- What is the relationship between giant planets and
-   small body belts?
- What is origin of giant planet spins?
- Why is there a brown dwarf desert?

## Karkoschka 1994

- wavelength (nanometers)

## Karkoschka 1994

## OWA: 2.5 arcsec, Jupiter zone=5-10 L1/2  AU

- OWA: 2.5 arcsec, Jupiter zone=5-10 L1/2  AU

## Slide 24

## Tools:

- Study RV+SIM Exo-Jupiters
**Extended Spectroscopic Capabilities: the bigger the range, the better!**
**High Resolution Spectrograph:**
**Transit Observations **
- Follow Up Kepler Discoveries
- Test mass vs luminosity relations and date systems using SIM Masses

## Planets around:

**A stars**, **M stars, O+B stars?**:  more statistics. How does the process of planet formation change with stellar mass?
**White Dwarfs**
- Much less contrast needed in IR
- photon noise limited--look in closer (1 AU)
- than JWST, or more distant objects.
- Faster photometry---time resolved?
- What is the future of the solar system?
**Red Giants**:
- Is is stellar mass loss sudden or adiabatic?
- Do planets create asymmetries in PN?

## Key YSO Questions:

- Where does the gas go?
- Do planets open gaps?
- What is disk temperature and chemistry in
-    the planet-forming region?
- Do disks become self-shadowed?
- What forms jets?
**Find and image new disks.**
- Only 10-20% of sources with IR excess and
- extended CO emission show disks that HST could see
- in scattered light.
- Study disks around brown dwarfs.
- ALMA takes days to get to 100 zodis!

## Study Disk Chemistry

**Study Disk Chemistry**
- Many IR lines not accessible to ALMA.
- Silicate emission feature 10 microns.
- H2 emission (IR) 17microns
- H2O CO CO2
- Map dissacociation regions and photoionization
- regions that generate disk winds that remove the disks.
- High-resolution IR spectrograph + wide-field imaging.
- OTHER IDEAS:
- Resolve closely separated PMS binaries
- Astrometry of PMS binaries that are too cool or
- embedded for SIM.   IR TPF at 2 microns?
- Study colimation of jets--X winds? Or disk winds?
- Very high resolution Optical.

## Solar System:

**Chemistry**
- Comets and in planetary
- atmospheres: isotopic abundances
- resolved high-res spectroscopy at Kuiper Belt
- few x 100 km resolution at Kuiper Belt
**Hi res IR spectrograph**---compare to SOFIA
- Optical spectroscopy, phase curves,
- and transit curves of faint objects:
- KBOs, Comet Cores, NEOs.
- (few x better resolution than ground-based)
- Resolve Binary KBOs
- Follow up LSST and MACHO discoveries.

## AGN

- Key Questions:
- How do massive black holes form and evolve?
- What is relationship between galaxies and BHs?
- IR:
- Mapping of dusty torii to z=7
- detailed kinematics of torii  R=2000
- Optical:
- morphology of quasar host galaxies, z=0.2-2
- higher contrast and resolutionthan JWST
- polarimetry of host galaxies: emission physics
- light echoes gives you distances

## Cosmology

- Key questions:
- 1) What is Dark Matter?
- 2) What is Dark Energy?
**Cluster lensing**:  Distribution of dark matter
**Distances:** Cepheids (to 3 times farther than HST)
- Surface brightness fluctuations
- Measure H0 to 2% =  Measurement of w
- (when combined with WMAP data)
**Optical: Wide Field of View+Astrometry!**

## 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. 

## 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

## 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 Meeting

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

## Meeting:  Tomorrow and Friday

- Space Telescope
**The Science Potential of a**
**10-30m UV/Optical Space Telescope**
- http://www.stsci.edu/stsci/meetings/vlst/

## Resolution vs. Collecting Area

- Log10 (Angular Resolution(”))

- Log10 (Collecting Area (sq.m))

- 4m

- 8m

- 16m

- HST @
- m

-  3.2m

- Spitzer @
- m

- Circular Apertures

- JWST @
- m

- Long Wavelength Limit
- (warm telescope)

-  1.6m

-  0.8m

-  0.4m

-  0.2m

- Short Wavelength Limit
- (coatings)

- TPF-C base band 0.5-0.8m