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Exoplanet Atmospheres Characterization in the Framework of the MIRI EC GTO

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Exoplanet Atmospheres Characterization in the Framework of the MIRI EC GTO Trappist-1 system Exoplanet Atmospheres Characterization in the framework of the MIRI EC GTO P.-O. Lagage CEA, Paris-Saclay University Image credit: NASA/JPL-Caltech On behalf of the MIRI EC exoplanets team MIRI JWST Copyright: Stephen Kill, Kill, STFC Stephen Copyright: Guaranteed Time Observations 4020 hours ; 8% of nominal 5 years operation of the JWST NIRCam team (900 hours): Marcia Rieke (PI) NIRSpec team (900 hours): Pierre Ferruit (PI) MIRI teams (900 hours): •European MIRI team (450 hours): Gillian Wright (PI) •US MIRI Science Lead (210 hours): George Rieke •US MIRI Science Team members (3×60 hours) : Tom Greene, Margaret Meixner, Mike Ressler •US STScI Scientists (5×12 hours): Christine Chen, Scott Friedman, Karl Gordon, Dean Hines, Alberto Noriega-Crespo FGS/NIRISS team (450 hours): René Doyon (PI) U.S. Telescope Scientist (210 hours): Matt Mountain Interdisciplinary Scientists (6 x 110 hours) : Heidi Hammel, Simon Lilly, Jonathan Lunine, Mark McCaughrean, Massimo Stiavelli, Rogier Windhorst. Most of the time used during cycle 1 25% of the time dedicated to exoplanets (75% transiting, 25% direct imaging) P.-O. Lagage, IAU 22/08/2018 MIRI EC Exoplanet GTO Observing plan MIRI 110 hours (25%) of MIRI European Consortium GTO dedicated to exoplanet/BD observations Motivations 1) To understand the physics and chemistry processes at work in atmospheres of exoplanets not present in the solar system (some may be representative of the earlier planets of the solar system). Step needed for the : 2) Ultimate goal to search for bio-signatures (e.g. O 3) 3) To constrain planet formation (metallicity, C/O ratio, luminosity for young exoplanets) P.-O. Lagage, IAU 22/08/2018 MIRI EC Exoplanet GTO Observing plan MIRI 60 hours for observations of transiting exoplanets 40 hours for observations of exoplanets detected by direct imaging 10 hours for observations of brown dwarfs (making the link with exoplanets) P.-O. Lagage, IAU 22/08/2018 MIRI EC Exoplanet GTO Observing plan MIRI 60 hours for observations of 3 transiting exoplanets Giant planet : Atmosphere physics and chemistry; C/O ratio, metallicity Intermediate mass Giant – Neptune: Earth mass planet: First step towards the study of Earth Like mass and temperature exoplanets 40 hours for observations of 10 exoplanets detected by direct imaging HR 8799 b, c, d GU Psc b GJ504 b 2MASS J2236+4751 b Young; luminosity; HD95086 b WD 0806-661B Formation 2MASSW J1207334-393254 b ROSS 458 AB c HD 106906 b PSO J318.5338-22.8603 10 hours for observations of 7 brown dwarfs (making the link with exoplanets) WISEPC J121756; Eps Ind Ba+Bb; WISEPA J173835.53; WISE J085510.83; WISE J1828; WISE J0458+6434 ; P.-O. Lagage, IAU 22/08/2018 All the MIRI modes will be used P.-O. Lagage, IAU 22/08/2018 All the MIRI modes will be used Transiting exoplanets Giant planet : Slitless LRS; transit + eclipse Intermediate mass Slitless LRS; transit Giant – Neptune: Earth mass planet: Imaging ; eclipse Exoplanets detected by direct imaging HR 8799 b, c, d GU Psc b GJ504 b Corono 2MASS J2236+4751 b HD95086 b WD 0806-661B LRS; imaging HD 106906 b ROSS 458 AB c Poster by C. Danielski 2MASSW J1207334-393254 b MRS PSO J318.5338-22.8603 Brown dwarfs (making the link with exoplanets) MRS P.-O. Lagage, IAU 22/08/2018 GTO Imaging observations of Trappist 1 b Trappist-1 system Imaging Search for thermal emission of Trappist b (400 K) by combining 5 eclipses (25 hours) with the 12.80 filter S/B of 5 expected Image credit: NASA/JPL-Caltech Paving the way to higher number of eclipses Guillon et al. 2017, Nature P.-O. Lagage, IAU 22/08/2018 Ozone search Trappist b, c, d How to recognize a bio-signature? Collaboration with other GTO teams Main molecules have bands in the IR from near IR to mid-IR NIRSPEC, MIRI NIRCAM, From G. Tinetti et al. AAR 2013 NIRISS The broad wavelength coverage from visible to mid IR : a great advantage probing different regions in the atmosphere 11 P.O. Lagage; SF2A, June 2015 Collaboration with other GTO teams Transiting exoplanets collaboration with Tom Greene (MIRI GTO + NIRCAM GTO) WASP107b, (NIRCAM obs) Trappist 1 b (filter at 15 microns) Deming et et al. Deming2009 Exoplanets detected by direct imaging Coronography MIRI with G. Serabyne (20 h MIRI JPL GTO) (HR8799 e, 51-Eri b) NIRCAM (C. Beichman et al.) Spectroscopy : NIRCAM (K. Hodapp et al.); 1 source (2M1207b) with NIRSPEC (S. Birkmann et al.) Brown dwarfs With NIRCAM (T. Roelling et al.) One source (WISE J085510.83) NIRSPEC, NIRCAM, NIRISS (C. Alves de Oliveira) P.-O. Lagage, IAU 22/08/2018 MIRI EC Exoplanet GTO Observing plan MIRI 60 hours for observations of transiting exoplanets Giant planet : Atmosphere physics and chemistry; C/O ratio, metallicity Intermediate mass Giant – Neptune: Earth mass planet: First step towards the study of Earth Like mass and temperature exoplanets 40 hours for observations of exoplanets detected by direct imaging HR 8799 b, c, d GU Psc b GJ504 b 2MASS J2236+4751 b Young; luminosity; HD95086 b WD 0806-661B Formation 2MASSW J1207334-393254 b ROSS 458 AB c HD 106906 b PSO J318.5338-22.8603 10 hours for observations of 7 brown dwarfs (making the link with exoplanets) WISEPC J121756; Eps Ind Ba+Bb; WISEPA J173835.53; WISE J085510.83; WISE J1828; WISE J0458+6434 P.-O. Lagage, IAU 22/08/2018 Data reduction, analysis and interpretation Several challenges to face given the high S/N or wavelength coverage provided by JWST observations Terrific S/N > 100 for exoplanets detected by direct imaging Baudino et al. 2017 P.-O. Lagage, IAU 22/08/2018 Data reduction Spitzer/IRAC observations at 3.6 µm of GJ436b Raw lightcurves Detrended lightcurves + models ICA e.g. Morello et al. 2015 Developping MIRI transit simulations importance of various effects; testing various spectra extraction… (PhD Marine Martin–Lagarde) P.-O. Lagage, IAU 22/08/2018 Modelling Benchmarking activity : Comparing three 1D models: ATMO, Exo_REM, petitCODE Has been beneficial to each model, which has been improved; Better knowledge of the limitation of current models (Alkalin) PH3 opacities have to be taken into account J.-L. Baudino et al. 2017 P.-O. Lagage, IAU 22/08/2018 In parallel : retrieval activity Given the high precision of JWST observations over a large wavelength range simplified models, such as those assuming isothermal temperature, to retrieve transmissio spectra are no longer valid information on the P-T atmospheric profile can be retrieved from transmission spectra 3D effect are also to be taken into account (in progress; I. Waldmann) P.-O. Lagage, IAU 22/08/2018 Since January 2018, the activity is funded in the framework of an European Commission Grant (1.5 M€ in total for 3 years) : ExoplANETS-A See presentation by J. Pye tomorrow Symposium 345 Consortium of 7 European institutes: CEA-Saclay (Paris, France), INTA (Madrid, Spain), MPIA (Heidelberg, Germany), University College London (U.K.), University of Leicester (U.K.), SRON (Utrecht, NL), Universitat Wien (Austria); P.-O. Lagage, IAU 22/08/2018 ProJect also well connected to the ARIEL mission, selected as the M5 mission of the ESA cosmic-vision 2015 - 2025 PI: G. Tinetti Mission dedicated to the Study of exoplanet atmospheres with a statistical approach : 1000 atmospheres to be probed To be Launched in 2028 Image Credit: ESA/STFC RALSpace/UCL/Europlanet-Science Office 19 P.-O. Lagage, IAU 22/08/2018 So very exciting perspectives for the Characterisation of the atmosphere of exoplanets P.-O. Lagage, IAU 22/08/2018 END P.-O. Lagage, IAU 22/08/2018.
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