planetary characterization
DESCRIPTION
Planetary Characterization. Giovanna Tinetti University College London. - France Allard (CRAL, radiative transfer, spectral models) - Nicole Allard (GEPI, spectroscopy of atomic species) - Alan Aylward et al. (UCL, 3D upper atm. modeling) - PowerPoint PPT PresentationTRANSCRIPT
Planetary Planetary CharacterizationCharacterization
Giovanna Tinetti
University College London
- France Allard (CRAL, radiative transfer, spectral models)- Nicole Allard (GEPI, spectroscopy of atomic species)- Alan Aylward et al. (UCL, 3D upper atm. modeling)- Bruno Bezard (LESIA, solar system, models/observations)- James Cho (QMUL, atmosphere dynamics)- Athena Coustenis (LESIA, solar system, models/obs.)- Olivier Grasset (Un. Nantes, planetary interior)- John Harries (Imperial College, Earth mod/obs)- Hugh Jones (Un. of Herthfordshire, exoplanet obs.)- Helmut Lammer (IWF/OeAW, upper atm.)- Emmanuel Lellouch (LESIA, solar system, model/obs.)- Enric Palle (IAC, Earth observations/biosig.)- Heike Rauer et al. (DLR, atmos/biosig. modeling)- Jean Schneider (LUTH, exoplanet observations)- Franck Selsis (Un. Bordeaux, planetary models/biosig.)- Daphne Stam (SRON, exoplanet polarization)- Jonathan Tennyson (UCL, spectroscopy of molecules)- Giovanna Tinetti (UCL, exoplanet spectral simulations)- Yuk Yung (Caltech, photochemistry/rad. transfer)
Projects Spectral Bands
Output Type of Planets
High Accuracy RV Visible/NIR Mass, address, statistics Giant and super-Earths
Cold Spitzer
MIR Photometry and low res. spectroscopy of transiting
planets
Nearby Hot Jupiters and Neptunes, Super-Earths
around M stars?
Warm Spitzer
MIR Photometry at 3.6 and 4.5 micron
Nearby Hot Jupiters and Neptunes, Super-Earths
around M stars?
HST (UV) VIS, NIR Low, Medium, (High) res. Spectroscopy for transiting
planets
Nearby Hot Jupiters and Neptunes, Super-Earths
around M-stars?
SPHERE/GPI (2011) NIR
VIS
Photometry & spectra
Photometry, polarization
Young/massiv e nearby giants
Young/massiv e nearby giants
JWST (2013) NIR-MIR Photometry &
High Res. Spectroscopy transiting planets
Down to Super-Earths & favourable Earth-size Planets;
Habitable zone M-stars
SPICA (2018) (NIR)-MIR-FIR
Low & High Res. Spectroscopy transiting
planets
Down to Super-Earths & favourable Earth-size Planets;
Habitable zone M-stars
ELTs (2018-2020) VIS-NIR Spectroscopy, Photometry, Polarization
Mature giants, super-Earths
Small/medium telescope + Coronograph
(SEE-Coast, SPICA-coronograph, Epic, Peco,
Access etc.)
VIS + (NIR)
MIR
Photometry & spectra & degree of polarization
Photometry & Spectra
Mature giants, nearby super-
Earths
Astrometry / RV with ELT
Visible Mass, address, statistics Earth sized planets, habitable zone
TPF-C VIS (NIR) Low-Medium Res. Spectroscopy ~ 100
Down to Earth sized planets in habitable zone
TPF-O VIS (NIR) Medium Res. Spectroscopy 300-1000
Down to Earth sized planets in habitable zone
TPF-I/Darwin MIR Low-Res. Spectroscopy < 40 Down to Earth sized planets in habitable zone
Atmospheric characterisation: priorities for future missions
• Spectroscopy! • Spectral resolution• Signal to noise reachable• Integration time• Wavelength range• Instrument sensitivity• Redundancies to address degeneracy• Variety of planetary types (Gas-giants, Neptunes, Terrestrial Planets, orbiting different types of stars, @ different orbital separation
• Type of targets reachable
20082008Contribution: advanced.
Low res; spectroscopy from space.
Higher res. from ground?Hot planets orbiting very close
in, Targets down to Super-Earth
UV-IR
~2015-2018~2015-2018JWST, SPICA:
High spectral res. from space, down to ~Earth-size,
planets orbiting close-in,Habitable zone M-stars?
IR
Further into the future:Further into the future:Improved resolution,
sensitivity, broader spectral window etc.
20082008Contribution: study phase.
2010: VLT-Sphere first light (warm Jupiters, large separation)
~2015-2018~2015-2018Small size space-based missions?
E-ELT-EPICS (ground) Low spectral res. ~ 65,
planets with larger separation,down to Super-Earth size,
Habitable zoneVIS-NIR-MIR
Further into the future:Further into the future:Large space-based missions,Planets down to Earth-size,
Habitable zoneHigher spect. resolution
dnvkav
Transiting planets
The present (Hubble, Spitzer, ground)
Planets orbiting VERY close in +
Photometry/low spectral resolution from space, very high spect. res from ground?
Hot Jupiters, hot Neptunes, hot-Super Earths?
Radial velocity / Occultation
Period = 3.524738 Period = 3.524738 daysdays
Mass = 0.69 ±0.05 Mass = 0.69 ±0.05 MMJupiterJupiter
Radius = 1.35 ±0.04 Radius = 1.35 ±0.04 RRJupiter Jupiter
Density = 0.35 ±0.05 Density = 0.35 ±0.05 g/cmg/cm33
HD 209458bHD 209458b
Sotin, Grasset & Mocquet;
Kuchner & Seager;
Radius/mass ratio
Ice
Silicate
Carbon
Charbonneau et al., 2002
0.0232±0.0057%
First atmospheric component: NaFirst atmospheric component: Na
Sensitive to overall temperature, main atmospheric component, planetary mass
Harrington et al., Science, 2006
υ Andromeda light-curve @ 24
μm
contribution from the planet:
~0.1%
Light curves of a non-transtiting Light curves of a non-transtiting exoplanetexoplanet
VIS-MIR transit VIS-MIR transit spectroscopy spectroscopy
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Swain, Vasisht, Tinetti, Bouwman, Deming, Nature, submitted
Swain et al., 2008aSwain et al., 2008a +Grillmair, 2007
Charbonneau et al., 2008
Knutson et al., 2008
Deming et al., 2007
Knutson et al., 2008
Beaulieu et al., 2008Swain et al., 2008
Pont et al., 2007
d
H2O, CH4, CO + other C-N bearing molecules
The short term future (JWST, SPICA?)
Planets orbiting VERY close in +
High spectral resolution from space
Hot Jupiters, hot Neptunes, hot-Super Earths,hot Earth-size?
Warm Earth-size (Mstar)
Cavarroc, Cornia, Tinetti, Boccaletti, 2008
James Webb Space Telescope James Webb Space Telescope performances (MIRI)performances (MIRI)
Earth-size Planets @ 10, 20, 30 parsec
SPICA
• Japanese (ISAS/JAXA) proposal for successor mission to Spitzer, Akari and Herschel
• Telescope: 3.5m, <5 K
– Herschel: 3.5m, 80K
– JWST: ~6m, ~45K
• Core λ: 5-200 μm
– Δθ=0.35”-14”
• Orbit: Sun-Earth L2 Halo
• Warm Launch, Cooling in Orbit
– No Cryogen → 3.2 t
– Long Lifetime
• Launch: 2017
Primary and secondary transit
photometry/spectroscpy have been shown to be very powerful diagnostic
techniques to probe the atmospheres of extrasolar
planets.
But for planets with larger separation from the Star…
Direct detectionDirect detection
Stellar light reflected by the planet
(UV/visible)
Multiple scattering of reflected photons:Rayleigh scattering/clouds/surface typesMolecules with electronic transitions
Molecules/clouds/surface types
Photons emitted by the planet, Molecules (roto-vibrational modes),
thermal structure, clouds
Photons emitted by the planet
(IR)
Molecules/thermal structure
O3
200 300250
Tropopause
Stratopause
Water Vapor
Ozone Absorption
Absorption
0
10
20
30
40
50
60Net
Emission
In the visible, sunlight is reflected and scattered back to the observer, and is absorbed by materials on the planet’s surface and in its atmosphere.
The planet is warm and gives off its own infrared radiation. As this radiation escapes to space, materials in the atmosphere absorb it and produce spectral features.
VIS - Near VIS - Near IRIR
Molecules in 0.4-2.5 microns
Molecule
Absorption bands (μm)
H2O 0.51, 0.57, 0.61, 0.65, 0.72, 0.82, 0.94, 1.13, 1.41, 1.88, 2.6
CH4 0.48, 0.54, 0.57. 0.6, 0.67, 0.7, 0.79, 0.84, 0.86, 0.73, 0.89, 1.69, 2.3
CO2 1.21, 1.57, 1.6. 2.03
NH3 0.55, 0.65, 0.93, 1.5, 2, 2.3
O3 0.45-0.75 (the Chappuis band)
O2 0.58, 0.69, 0.76, 1.27
CO 1.2, 1.7, 2.4
H2S
VIS: AlbedoVIS: Albedo
Karkoschka, Icarus, 1998
H2O, CH4, NH3, C2H6, CO, H2S, CO2
…
Terrestrial Planet Spectra Vary Widely in Solar System
O2
Iron oxides
CO2
H2O H2O
CO2
EARTH-CIRRUS
VENUSX 0.60
MARS
EARTH-OCEAN
H2O H2O
H2O ice
?
O3O2
VIS-Near-IR signatures for terrestrial planetsVIS-Near-IR signatures for terrestrial planetsin our Solar System in our Solar System
Polarization: a huge help to distinguish
clouds
Polarization variations 10%-40%(Stam et al 2004)
=> Starlight is NOT polarized
Polarization: sensitivity to phase
Polarization variations 10%-40%(Stam et al 2004)
=> Starlight is NOT polarized
IRIR
H2O, CO2, CH4, Hydrocarbons, HCN, H2S, SO2, CO, N2O, NH3 ….
Molecules in the Mid-IR
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Terrestrial Planet Spectra Vary Widely in Solar System
MIR signatures for terrestrial planetsMIR signatures for terrestrial planetsin our Solar System in our Solar System
Knutson et al., Nature, 2007; ApJ, 2008
IR: Thermal structure, IR: Thermal structure, dynamicsdynamics
ESO Extremely Large Telescope-ESO Extremely Large Telescope-EPICSEPICS
EPICS is an instrument project for the direct imaging and characterization of extra-solar planets with the European ELT
• The eXtremeAdaptive Optics(XAO) system - The Diffraction Suppression System(or coronagraph) - The Speckle Suppression System
• The Scientific Instrument(s) - Integral Field Spectroscopy - Differential Polarimetry - A speckle coherence-based instrument
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Missions concepts Missions concepts consideredconsidered
for studies (US)for studies (US)
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Access: coronagraphs for exoplanet missions (John Trauger)
Davinci, Dilute Aperture VIsible Nulling Coron. Imager(Michael Shao)
EPIC: directly imaging exoplanets orbiting nearby stars (Mark Clampin)
PECO: refining a Phase Induced Amplitude Apodization Coronograph (Olivier Guyon)
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M-mission from space or first generation from ground
NWO is a large-class Exoplanet mission that employs two spacecrafts: a “starshade” to suppress starlight before it enters the telescope and a conventional telescope to detect and characterize exo-planets.
Cash, Nature, 2006
The New World Observer
Spectroscopy
O2
H2O
CH4
NH3
S. Seager
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Coronagraph on SPICA
• Assumed observation mode - imaging and low res. spectroscopy - because of limit of sensitivity• Distance/number of target - a few hundred of target in 10pc - a few x 10 seems too small - a few x 1000 is difficult to complete
survey• Wavelength - 3.5-27um rather than 5-27um to detect
excess in spectral, and advantage on IWA.• IWA - limited by coronagraph method. - 3.3 lambda/D (binary mask mode,
baseline of SPICA coronagrah) - 1.2-1.5 lambda/D (PIAA mode)• Contrast - finally 10^-7. To obtain it, 10^-6 for
raw contrast. (~10 is assumed as gain of
subtraction)
Enya et al., Enya et al., 20082008
Direct Detection of Earth-size Planets IR