Characterising Exoplanet Satellite

Transcription

1 Exoplanet Science Quy Nhơn, Việt Nam 21 April 2014 Characterising Exoplanet Satellite David Ehrenreich s first small-class mission

2 Mass-radius diagram 3 distinct families in the Solar System Planet radius (Earth = 1)! 10! 1! icy moons rocky moons high density [g cm -3 ] low density telluric planets ice giants gas giants 0.1! 0.01! 0.1! 1! 10! 100! 1000! 10000! Planet mass (Earth = 1)! planet bulk densities

3 Mass-radius diagram Apparent continuity of masses for exoplanets Planet radius (Earth = 1)! 10! 1! icy moons high density [g cm -3 ] low density telluric planets K-78b (5.5) K-11f (0.7) K-10b (8.8) ice giants C-7b (6.2) gas giants 55 Cnc e (4.3) rocky moons 0.1! 0.01! 0.1! 1! 10! 100! 1000! 10000! Planet mass (Earth = 1)!

4 What are exoplanets made of? GJ 3470b Corot-7b telluric Léger super-earths? Kepler-11f Lissauer gas dwarfs?? Kepler-78b Pepe+, Howard+ 2013? ocean 55planets? Cnc e Winn+, Demory Léger Bonfils massive core HD b Sato subgiants? GJmini 1214b Charbonneau Neptunes? hydrogen/helium envelope thin atmosphere ice mantle/volatile envelope solid core (rocks+metals) Constraints based on bulk densities

5 How do they evolve? How do they survive under extreme irradiation? GJ 436b Kulow Cancri e Winn Demory KIC b Rappaport+ 2012??? hot & warm Jupiters hot Neptunes? hot super-earths? Kepler-78b Sanchis-Ojeda HD b, HD b, 55 Cancri b Vidal-Madjar+ 2003; Lecavelier+2012; Ehrenreich hydrogen/helium envelope thin atmosphere ice mantle/volatile envelope solid core (rocks+metals)

6 Which planets are the golden targets for atmospheric characterisation? 55 Cnc e HST 3σ detection limit sodium detection on HD b Charbonneau HD b HD b Density matters for atmospheric studies The less dense at given mass, the easier to characterize (Ehrenreich+ 2006)

7 Which planets are the golden targets for atmospheric characterisation? JWST 3σ detection limit water detection on HD b in 1 transit (Deming+ 2013) All transiting planets! Hydrogen-rich atmospheres J magnitude HST Absorption signal of one atmospheric scale height in transmission spectroscopy (ppm)

8 Which planets are the golden targets for atmospheric characterisation? JWST 3σ detection limit water detection on HD b in 1 transit (Deming+ 2013) Transiting super-earths (<10 ME)! Hydrogen-rich atmospheres J magnitude HST Absorption signal of one atmospheric scale height in transmission spectroscopy (ppm)

9 Which planets are the golden targets for atmospheric characterisation? JWST 3σ detection limit water detection on HD b in 1 transit (Deming+ 2013) Transiting super-earths (<10 ME)! Water-rich atmospheres J magnitude HST 10 GJ 1214b Absorption signal of one atmospheric scale height in transmission spectroscopy (ppm)

10 Which planets are the golden targets for atmospheric characterisation? JWST 3σ detection limit water detection on HD b in 1 transit (Deming+ 2013) Transiting super-earths (<10 ME)! Water-rich atmospheres J magnitude HST Flat spectrum clouds! 12 HST transits (Kreidberg+ 2014) 10 GJ 1214b Absorption signal of one atmospheric scale height in transmission spectroscopy (ppm)

11 Targets: bright stars Better knowledge of the stars Better knowledge of the planets TESS 1st S-class mission adopted by ESA (Feb 2014) PLATO

12 CHEOPS main science goals What will do: Perform 1st-step characterization of super-earths & Neptunes Measure accurate radii & bulk densities of super-earths & Neptunes orbiting bright stars Provide golden targets for future atmospheric characterization How CHEOPS will do it: High-precision photometry Achieve a photometric precision similar to Kepler Observing brighter stars anywhere on the sky

13 CHEOPS strategy: Follow-up TESS (2017) Me asu re a ccu rat e li ght Ground-based transit surveys NGTS (2014) cur ves for Ne ptu n es rths er-ea p u s n w t of kno ransi he t Detect t Ground-based RV surveys HARPS, HARPS-N, HIRES, SOPHIE (on going) ESPRESSO (2017) 20% open time (3.5-yr mission) K2 (2014)

14 CHEOPS legacy JWST 2018 E-ELT, GMT, TMT ~2020

15 ESA s first small mission requirements Science Top-rated science in any area of space sciences Cost Total cost < 150 M ESA cost < 50 M (fixed) Schedule Developed and launched within 4 years

16 ESA s first small mission requirements Science 1st mission dedicated to exoplanet follow-up Top-rated science in any area of space sciences Cost ESA cost < 50 M (fixed) Total cost < 150 M Schedule ~100 M Platform Detector Launch Developed and launched within 4 years

17 CHEOPS in Europe CHEOPS consortium Small mission, large organization

18 CHEOPS consortium in Europe Small mission, large organization Switzerland Mission Lead Instrument Team Science Operations Center PI: Prof. Willy Benz, U. Bern

19 CHEOPS consortium in Europe Small mission, large organization Switzerland Mission Lead Instrument Team Science Operations Center Germany Focal Plane Assembly Belgium Baffle Italy Optics Austria Digital Processing Unit Hungary Radiators

20 CHEOPS consortium in Europe Small mission, large organization Switzerland Mission Lead Instrument Team Science Operations Center Sweden Data simulator Germany Focal Plane Assembly UK Mission Operations Center France Data Reduction Software Portugal Mission Planning, Archive, & Data Reduction Software Belgium Baffle Italy Optics Austria Digital Processing Unit Hungary Radiators

21 CHEOPS in Europe CHEOPS consortium Small mission, large organization Switzerland Austria Belgium France Germany Hungary Italy Portugal Sweden UK University of Bern (project lead)! University of Geneva! Swiss Space Center (EPFL)! ETH Zürich Institut für Weltraumforschung, Graz Centre Spatial de Liège! Université de Liège Laboratoire d astrophysique de Marseille DLR Institute for Planetary Research Konkoly Observatory Osservatorio Astrofisico di Catania INAF! Osservatorio Astronomico di Padova INAF! Università di Padova Centro de Astrofisica da Universidade do Porto! Deimos Engenharia Onsala Space Observatory, Chalmers University! University of Stockholm University of Warwick

22 CHEOPS spacecraft telescope cover radiators instrument baffle star tracker Total weight: 250 kg Total length: 1.3 m platform Two competing platform concepts

23 CHEOPS instrument system radiator radiator isostatic mount optical bench radiator support and optics hood structure tube CCD & FPA BEO with folding mirror secondary mirror primary mirror Telescope : 32 cm Total weight: 60 kg

24 CHEOPS observations Frame-transfer CCD telescope FoV: 20 1k 1k subarray image pixels (4 arcmin2) On-board data stacking Measurement cadence: 1 min-1 30 pixels (30 ) CHEOPSim defocused PSF CHEOPS photometric precision Pointing stability: 8 (rms) jitter p-flat precision: 0.1% pixel-to-pixel

25 CHEOPS science requirements Measuring highly accurate signals 20 ppm accuracy over 6 hours for G-type stars with V < 9 mag 85 ppm accuracy over 3 hours for K-type stars with V < 12 mag

26 CHEOPS science requirements Measuring highly accurate signals 20 ppm accuracy over 6 hours for G-type stars with V < 9 mag 85 ppm accuracy over 3 hours for K-type stars with V < 12 mag Pointing at any location over more than 50% of the sky Can choose the best targets for transit search Can confirm transiting planets on longer orbits (e.g., for TESS) Can search for additional planets

27 orbit km OBSERVATIONS Sun

28 CHEOPS sky

29 Summary CHEOPS is Europe s next exoplanet mission (2017) is a follow-up machine, CHEOPS Knowing when to look at a star makes CHEOPS extremely efficient Provides a first-step characterization of low-mass exoplanets Collects the golden targets for future in-depth characterization Allows 20% open time for high-precision photometry science Next milestones More information in: Choice of the platform Preliminary Design Review (May-June) ESA CHEOPS Definition Study Report

30 Summary CHEOPS is Europe s next exoplanet mission (2017) is a follow-up machine, CHEOPS Knowing when to look at a star makes CHEOPS extremely efficient Provides a first-step characterization of low-mass exoplanets Collects the golden targets for future in-depth characterization Allows 20% open time for high-precision photometry science Next milestones More information in: Choice of the platform Preliminary Design Review (May-June) ESA CHEOPS Definition Study Report Thank you Cảm ơn

31 CHEOPS prescreening for JWST What TESS can do for CHEOPS: Provide targets for CHEOPS follow-up What CHEOPS can do for TESS: Maximize science impact of JWST transit observations Validate TESS long-period candidates Precise radii & densities for TESS planets: thick atmospheres? Planet parameters vs. cloud correlation? Obtain long-baseline TTVs for TESS planets

32 CHEOPS in Europe Science Team Board Yann Alibert Universität Bern Tamás Bárczy Admatis François Bouchy Alexis Brandeker Christopher Broeg Juan Cabrera David Ehrenreich Anders Erikson Andrea Fortier Michaël Gillon Manuel Güdel Kevin Heng Laboratoire d'astrophysique de Marseille Stockholms Universitet Universität Bern DLR Institut für Planetenforschung Université de Genève DLR Institut für Planetenforschung Universität Bern Université de Liège Universität Wien Universität Bern Wolfgang Baumjohann Willy Benz Magali Deleuil Michaël Gillon Antonio Gutiérrez Peña László Kiss Alain Lecavelier René Liseau Göran Olofsson Institut für Weltraumforschung Universität Bern Laboratoire d'astrophysique de Marseille Université de Liège Deimos Konkoly Obszervatórium Institut d'astrophysique de Paris Chalmers Tekniska Högskola Stockholms Universitet Gyula Szabó Konkoly Obszervatórium Giampaolo Piotto Università degli Studi di Padova Helmut Lammer Christophe Lovis Michael R. Meyer Isabella Pagano Giampaolo Piotto Didier Queloz Roberto Ragazzoni Sérgio Sousa Institut für Weltraumforschung Université de Genève Eidgenössische Technische Hochschule Zürich INAF Osservatorio Astrofisico di Catania Università degli Studi di Padova Université de Genève INAF Osservatorio Astronomico di Padova Centro de Astrofísica da Universidade do Porto Roberto Ragazzoni Étienne Renotte Nuno C. Santos Tilman Spohn Manfred Steller Nicolas Thomas Stéphane Udry INAF Osservatorio Astronomico di Padova Université de Liège Centro de Astrofísica da Universidade do Porto DLR Institut für Planetenforschung Institut für Weltraumforschung Universität Bern Université de Genève Tilman Spohn DLR Institut für Planetenforschung Valérie Van Grootel Université de Liège