Giant Planets in the Context of Planetary Systems

1
TPF Ancillary Science 2/04 Marc Kuchner
2
TPF vs. LISA, SPIRIT, SUVO, etc. Interferometer
vs Coronagraph
3
(No Transcript)
4
(No Transcript)
5
(No Transcript)
6
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
7
IRAM Plateau de Bure 1.3 mm
arcsec
Vega
arcsec
8
Optical TPF Advantages High Contrast Accurate
Pointing (Boresite) and Figure Stability Optical
Wavelengths
9
IR TPF Advantages (vs. JWST) High
Contrast Stability Angular Resolution Option
for More Instruments e.g. hi-res spectrograph
10
tpf-swg-ancillary_at_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
11
Bill Danchi Rene Liseau Jonathan I. Lunine
Kenneth J. Johnston Doug Lin Charley
Noecker Kilston, Steve
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
12
Ancillary Science Website http//www.astro.princ
eton.edu/mkuchner/ancillarysci.html
Ancillary Science with TPF Send comments to
Marc Kuchner Base Missions IR 6.5-13
microns, R20 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, R70 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!
13

• 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

14

• 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

15

• III) Modificaions to TPF
• Tony Hull, Charlie Noecker
• Wide-Field Imaging
• David Leisawitz (IR), Thangasamy Velusamy (IR)
• B) High-Resolution Spectroscopy
• Mid IR--R100,000?
• C) Astrometry Ken Johnston
• 100 microarcsec of faint objects--
• Distance to the Hulse-Taylor binary pulsar
• Isolated neutron stars at 24-25 magnitude

16

• Optical
• Tall TPF Grande TPF
• IR
• Tall TPF Grande TPF
• Plain TPF
• Tweaked TPF
• Modified TPF (1 new instrument)

17
HIGHLIGHTS
18
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?
19
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/inclinatio
n/semimajor axis distribution. Orbit
Determination Phase Curves Rings and
moons Polarimetry cloud compositions Correlate
planets and exozodiacal clouds.
20
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?
21
Karkoschka 1994
wavelength (nanometers)
22
Karkoschka 1994
23
OWA 2.5 arcsec, Jupiter zone5-10 L1/2 AU
24
(No Transcript)
25
Tools Study RVSIM 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
26
Planets around A stars, M stars, OB 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?
27
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!
28
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.
29
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.
30
AGN Key Questions How do massive black holes
form and evolve? What is relationship between
galaxies and BHs? IR Mapping of dusty torii to
z7 detailed kinematics of torii
R2000 Optical morphology of quasar host
galaxies, z0.2-2 higher contrast and
resolutionthan JWST polarimetry of host galaxies
emission physics light echoes gives you distances
31
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 ViewAstrometry!
32
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)
33
Wide Field Imaging
Coronagraph focus
Ancillary camera

• 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 gt 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

34
Things we could resolve at K-band with
interferometer (1 millarcseconds) Near Earth
Objects Comet nuclei X-ray binaries Supergiants Pl
anetary Nebulae Supernova Remnants in Virgo GRB
light echoes
35
TPF Ancillary Science Meeting Princeton
University April 14-15 Prepare report for
presentation to CAA
36
Meeting Tomorrow and Friday Space
Telescope The Science Potential of a 10-30m
UV/Optical Space Telescope http//www.stsci.edu/s
tsci/meetings/vlst/
37
Resolution vs. Collecting Area
Log10 (Collecting Area (sq.m))
Long Wavelength Limit (warm telescope)
? 3.2mm
? 1.6mm
Log10 (Angular Resolution())
Spitzer _at_ l 3.5mm
Circular Apertures
? 0.8mm
? 0.4mm
TPF-C base band 0.5-0.8mm
? 0.2mm
JWST _at_ l 2.0mm
HST _at_ l 0.4mm
Short Wavelength Limit (coatings)
8m
4m
16m