The science of EChO Exoplanet Characterisation Observatory
Giovanna Tinetti & EChO consortium
UK, France, Italy, Spain, MPS Germany, Poland, Denmark, Ireland,Un. Liege, Portugal, Hungary, US ~850 Exoplanets!
Radial velocity, Transit Surveys Microlensing, Direct detec.
ESA-GAIA -> 104 new planets!
1 The science of EChO – ROPACS ~250 Exoplanets (+x000 candidates) Radius, Mass & Orbit
2 The science of EChO – ROPACS 16/11/12 Exoplanets for which we have spectra: < 20
H2O, CO, CH 4, CO2, Na etc. identified, but data are sparse, degeneracy of interpretation
Swain et al., 2009 3 The science of EChO – ROPACS 16/11/12 EPSC-DPS 2011
TESS PLATO E-ELT HUBBLE CoRoT VLT Finesse Early years The present The golden future 2000 2005 2010 2020 EChO Spitzer GAIA JWST Kepler Cheops SPICA
4 Big picture?
5 The science of EChO – ROPACS
EChO Exoplanet Characterisation Observatory
ESA M3 mission candidate – March 2011
ESA Science Team ESA EChO Study Team
ØG. Tinetti ØK. Isaak ØP. Drossart ØL.Puig ØO. Krause ØM. Linder ØC. Lovis ØG. Micela ØM. Ollivier ØI. Ribas ØI. Snellen ØB. Swinyard Gaseous planets formed elsewhere and migrated
Planet formation Energy budget C/O ratio Albedo/thermal emission
Planet-star interaction Photochemistry+ Weather Day/night variation Temporal variability/ T-P profile
Planet evolution + Escape/H3
8 The science of EChO – ROPACS 16/11/12
Terrestrial planets formed in situ? Or remnant of gaseous planets’ core?
Primary or secondary atmosphere? Does the planet have H2 retained or not an atmosphere? Energy budget Spectral observations Albedo/thermal emission
Habitable conditions? Main atmospheric component Temperature? H2O? Primary transit observations
Planet-star interaction Photochemistry
9 The science of EChO – ROPACS 16/11/12
Planets considered by EChO Jupiter Neptune Super Earth Radius
‘Hot’ (850-1500K)
‘War m’ (500-800K) Temperature Temperature
‘Temperate’ (250-350K)
F, G, K, M G, K, M M (G, K) EChO view from L2
EChO instantaneous field of view (L2)
11 The science of EChO – ROPACS 16/11/12 EChO candidates: Number known transiting hot-Jupiters 118 109 100 91 82 73 64 55 46 37 28 19 10 Mag K 1 5.5 6.5 7.5 8.5 9.5 10.5
12 The science of EChO – ROPACS 16/11/12
Method: Transit
This is a zoom in!
13 EChO Payload Consortium - Mid Term Review 16/11/12 Primary transit spectra
EChO Payload Consortium - Mid Term Review The science14 of EChO – ROPACS 16/11/12 Phase lightcurves
HAT-P7b observed by Kepler (Borucki et al, 2010)
15 The science of EChO – ROPACS 16/11/12 16 16 The science of EChO – ROPACS The science
16/11/12 Key Observables: Molecules Energy budget
Stratopause
Emission Absorber
Tropopause Absorption 0 20 25 30 0 0 0 Need for both VIS and IR to understand the planetary energy budget.
17 The science of EChO – ROPACS 16/11/12 Spectral coverage
Given the range of T considered, need to extend to the Mid-IR
18 The science of EChO – ROPACS 16/11/12 Key Science requirements/goals
ESA- SciRD 19 The science of EChO – ROPACS 16/11/12 EChO-SIM
ï4 x 10 2.5
2 0.017
0.0165
1.5 /F p
F 0.016 2 )
1 /R p 0.0155 0.006 (R 0.015 0.5 0.005 0.0145 0 1 10 100.004 Wavelength (!m) 0.014 0 1 0.003 10 10 Wavelength (!m) Contrast ratio 0.002
0.001
0 2 4 6 8 10 12 14 16 Wavelength (µm)
20 The science of EChO – ROPACS 16/11/12 SNR for molecular detectability
Warm-Neptune GJ436b Warm-Neptune Tessenyi et al.,2012; The science of EChO – ROPACS 21 Tessenyi et al. submitted. 16/11/12 Spectral retrieval T-P profile/molecular abundances
Lee, Fletcher, Irwin, 2011 Barstow et al., submitted 22 The science of EChO – ROPACS 16/11/12 Stellar activity
Temporal variability Temporal
Basri et al, 2010 23 The science of EChO – ROPACS 16/11/12 Work done on stellar activity
Spectral variability Spectral
Ballerini, Micela et al, 2012 To be matched with observations at multiple wl (Ribas et al.) 24 The science of EChO – ROPACS 16/11/12 Work done to remove stellar activity
Kepler photometry of an active star Use of statistical techniques statistical of Use Ballerini et al, 2012 Waldmann, 2012 25 The science of EChO – ROPACS 16/11/12 Transit-RV surveys Expected to provide additional targets for EChO
HARPS North HAT-NET Super-WASP Carmenes M-Earth NGTS APACHI Spirou MASCARA CHEOPS
26 The science of EChO – ROPACS 16/11/12 Science return for EChO
Photochemical models Photochemical
Moses et al., 2011; Venot, Selsis et al., 2012 EChO for return Science
27 The science of EChO – ROPACS 16/11/12 Science return for EChO
Science return for EChO EChO for return Science Thermal stability and escape and Thermal stability Koskinen et al., 2008, 2010 28 The science of EChO – ROPACS 16/11/12 Science return for EChO
Gaseous planets planets Gaseous Climate simulations Climate
Cho et al., 2003
29 The science of EChO – ROPACS 16/11/12 Science return for EChO
Climate simulations Climate Terrestrial planets: GJ581d GJ581d planets: Terrestrial
30 The science of EChO – ROPACS Wordsworth , Forget et al Join EChO!
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