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 Molecules Molecules Key Observables: Key 16 The science of EChO – ROPACS 16/11/12 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! Help us planning the best possible mission! http://www.echo2013.net/ .