TPF Ancillary Science 2/04 Marc Kuchner. TPF vs. LISA, SPIRIT, SUVO, etc. Interferometer vs...

TPF Ancillary Science 2/04Marc Kuchner

TPF vs. LISA, SPIRIT, SUVO, etc.

Interferometer vs Coronagraph

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

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

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

Marc KuchnerBill Danchi Sara SeagerDavid Spergel 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 Strauss

Marc KuchnerSara SeagerDavid Spergel Bill Sparks Huub Rottgering Tony Hull Karl Stapelfeldt Sally HeapEric GaidosTed von Hippel David SpergelDavid LeisawitzAlan DresslerMichael Strauss

Bill DanchiRene Liseau Jonathan I. Lunine Kenneth J. JohnstonDoug LinCharley NoeckerKilston, 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

Tallfour apertures,3.2 m diameter each spaced along a 36m array at 0,9, 27, 36 m.

Grandefour apertures,4.0 m diameter each, unevenly spaced along a 70 m arraym expandable to 150m

Visible: 0.5-0.8 microns, R=70

Tall3.5 by 6.5 m

Grande3.5 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. Hillenbrandastro-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 TelescopeRegister now!

I) Planetary Science; Comparative Planetology

A) Non-inhabitable planetsSara Seager, Jonathan Lunine

B) Planets around non-FGK stars:A stars, M stars, Brown Dwarfs, White DwarfsTed 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

A) Star formation, pre-main sequence binariesDoug Lin

B) CosmologyDark Matter, Dark Energy, Galaxy Formationand Evolution, First Generation of StarsDavid Spergel, Doug Lin

C) AGN, QSOsBill Sparks, Huub Rottergering

D) AGBs and massive starsBill Danchi, Steve Kilston

III) Modificaions to TPFTony Hull, Charlie Noecker

A) Wide-Field ImagingDavid Leisawitz (IR), Thangasamy Velusamy (IR)

B) High-Resolution SpectroscopyMid IR--R=100,000?

C) Astrometry: Ken Johnston100 microarcsec of faint objects--Distance to the Hulse-Taylor binary pulsarIsolated neutron stars at 24-25 magnitude

Optical “Tall” TPF + “Grande” TPF

IR“Tall” TPF + “Grande” TPF

1) Plain TPF2) Tweaked TPF3) 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-bodybelts and terrestrial planet formation?How common are big moons and rings?What are the compositions of extrasolarterrestrial 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 compoundsSilicate spectroscopyFind water planets and dry planets.Extended Spectroscopic Capabilities:the bigger the range, the better!

Dynamics: Measure eccentricity/inclination/semimajoraxis distribution. Orbit DeterminationPhase Curves: Rings and moonsPolarimetry: 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

Tools:

Study RV+SIM Exo-JupitersExtended 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 DwarfsMuch less contrast needed in IRphoton 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 andextended CO emission show disks that HST could seein scattered light.Study disks around brown dwarfs.ALMA takes days to get to 100 zodis!

Study Disk ChemistryMany IR lines not accessible to ALMA. Silicate emission feature 10 microns.H2 emission (IR) 17micronsH2O CO CO2

Map dissacociation regions and photoionizationregions that generate disk winds that remove the disks.High-resolution IR spectrograph + wide-field imaging.

OTHER IDEAS:

Resolve closely separated PMS binariesAstrometry of PMS binaries that are too cool orembedded for SIM. IR TPF at 2 microns?Study colimation of jets--X winds? Or disk winds? Very high resolution Optical.

Solar System:

ChemistryComets and in planetaryatmospheres: isotopic abundancesresolved high-res spectroscopy at Kuiper Beltfew x 100 km resolution at Kuiper BeltHi 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=7detailed kinematics of torii R=2000

Optical:morphology of quasar host galaxies, z=0.2-2higher contrast and resolutionthan JWSTpolarimetry of host galaxies: emission physicslight 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 fluctuationsMeasure 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)

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

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 Meeting

Princeton UniversityApril 14-15

Prepare report for presentationto CAA

Meeting: Tomorrow and FridaySpace Telescope

The Science Potential of a10-30m UV/Optical Space Telescope

http://www.stsci.edu/stsci/meetings/vlst/

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