And now, Molecules Jean Schneider

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And now, MoleculesJean Schneider Paris
Observatory

• Why
• Where
• How

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And now, Molecules

• Why molecules
• After mass, orbit, radius,  adresses  and
  statistics
• molecules gives the real characterization of
  exoplanets.
• Only part of more general approach spectra,
  images
• Atmosphere , Ground surface
• Whole planetary system
• Where (which type of planets)
• How
• Multiple approaches
• Reflected light vs/ thermal emission
• Polarization
• Time variation
•  Inverse problem 
• Implementation

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Molecules where do we stand?

•  Business as usual 
• Plenty of known molecules
• Na, CO, CO2, H20, CH4, HCN, H, O, TiO, VO
• Gradients
• Orbital evolution
• Secondary transits (Knutson)
• Beyond standard situations rings, artefacts,
  degeneracies....

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Why

• Why molecules
• After
• Mass and orbit and statistics (from RV
  astrometry 10-100 times more expensive)
• Radius from transits
• Radius disentangle atmosphere and solid core
• M-R-atmosphere correlation (Elkins-Tanton)
  insight on atmosphere origin degassing /vs
  accretion
• Starting from spectra, disentangle molecules from
  
• Haze
• Clouds
• Surface (Continents/oceans)

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Why

• After RVs, other approaches to investigate
  planets
• Transits first molecules (Charbonneau), but
• Only 1 10 of planets
• Only brief snapshot along the orbit (0.1 -
  0.5)
• Astrometry
• No information on the physics of planets

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Where

• Plenty of candidate super-Earths (Mayor et al
  2008)

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Some non standard situations

• Oxygen on icy bodies (Farmer et al. 2007)
• --gt abiotic oxygen on icy satellites of planet
  with liquid water ?
• Rings significant contribution to spectra (ice,
  CH4) but very different temperature
• 
  3 M_Earth 3 M_Jup
• 
  Ice Rock Ice Rock
• 
  ------------------------------------------
  --
• R_Ring
  2.5 3 R_Earth 3 4 R_Jup
• Hyper-Ios (Briot 2008)

Keywords openmindedness anticipation of
surprises
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Some non standard situations

• Rings
• --gt Contribution of
• ice bands in spectra
• Planet cooler in the ring's shadow
• (Bézard et al 1984) tiny distortion
• in thermal spectra

Temp.
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Some non standard situationsartefacts

• Band at 9.6 micron ozone or Diopside ?

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Some non standard situations

• Previous surprises
• Orbits
• Very close to parent star
• Eccentricity
• Too large radius of HD 209458 b
• Why HD 209458 b and HD 189733 b so different?
• Mass-temperature anomaly for 2M 053-054 BD binary
• The more massive has the lowest temperature
  (Stassun et al 2007)
• Fomalhaut b (Clampin this Meeting)
• Unexplained photometric variability
• Unexpectedly large flux
•  There is nothing like an average planet  (G.
  Laughlin)
• gt  planeto-diversity 

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How

• By-products of molecules by direct imaging
• Mass of planets
• From measuring orbital inclination RV
• From gap sculpturing in disks (Fomalhaut Chiang
  et al 2008)
• Removing degeneracies from RV or astrometry
  orbital solutions
• Trojan planets
• 12 resoances /vs eccentric orbits
•  exchange orbits  (2 planets on quasi-identical
  orbits)
• Doppler shift relative to star gt improve
  detection, planet mass (Riaud et al 2007)
• Benefits of continuous monitoring
• Rings
• Moons
• Planet rotation (Palle et al 2008)

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How

• One single approach not sufficient to remove
  degeneracies in extracting planet models from
  observables
•  Inverse problem  from observable to planet
  model
• gt necessity to accumulate observations in
  time, in wavelength range
• But no reason to wait for readiness of all
  approaches, start with the easiestgt step by
  step progression

Galileo
Today
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How

• Implementation a plan we can believe in
• Mono (-pupil -spacecraft) / Multi (-aperture
  -spacecraft)
• After RV, transits, continue step by step
  approach

• Mono pupil and spacecraft
• coronagraph VIS
• ELTs. Problems
• - share with cosmology, RV, etc .
• - not possible of continuous monitoring
• gt only few snapshot spectra
• 1.5 2 m dedicated space telescope

• Multi-aperture precursor ?
• Nulling interferometer IR

Large (4m) monopupil space corono.
Multi spacecraft
Multi-aperture - Nulling
interferometer - Hypertelescope

coronagraph IR 4-5 S/C
VIS gt 30 S/C
Mono -pupil - External occulter - Fresnel
array UV, VIS 2 S/C
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How
1993-4 TOPS (NASA) 1996 ExNPS (NASA) 1997 ESO
WG on Exoplanets Origins Roadmap
(NASA) 2005 Cosmic Vision (ESA)
ESA-ESO Report on Exopl. 2007 ExoPTF
(NASA/NSF) 2008 JPL  Community Report  2009
EPRAT (ESA) EXOPAG (NASA)
Decadal Survey (US Acad Sci) ... ad vitam
aeternam ?
51 Peg

• Implementation
• Mono (-pupil -spacecraft) / Multi (-aperture
  -spacecraft)
• After RV, transits, continue step by step
  approach

• Mono pupil and spacecraft
• coronagraph
• ELTs. Problems
• - share with cosmology, RV, etc .
• - not possible of continuous monitoring
• gt only few snapshot spectra
• 1.5 2 m dedicated space telescope

HD 209458 transit
CoRoT launch
Large (4m) monopupil space corono.
Multi spacecraft

• Multi-aperture
• Nulling interferometer
• Hypertelescope coronagraph

• Mono -pupil
• External occulter
• Fresnel array

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How

• Implementation
• Mono (-pupil -spacecraft) / Multi (-aperture
  -spacecraft)
• After RV, transits, continue step by step
  approach

• 1st step Mono pupil and spacecraft
• coronagraph
• ELTs. Problems
• - share with cosmology, RV, etc .
• - not possible of continuous monitoring
• gt only few snapshot spectra
• 1.5 2 m dedicated space telescope

Action!
Large (4m) monopupil corono.
2nd step Multi spacecraft
World-wide coordination needed

• Multi-aperture
• Nulling interferometer
• Hypertelescope coronagraph

• Mono -pupil
• External occulter
• Fresnel array