Exoplanets at the E-ELT era
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- Maximillian May
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1 Towards Other Earths II: The Star Planet Connection, Porto, September th, 2014 Exoplanets at the E-ELT era Gaël Chauvin - IPAG/CNRS - Institute of Planetology & Astrophysics of Grenoble/France ESO-Project Science Team, and E-ELT CAM, IFU, MIDIR, MOS, HIRES & PCS consortia
2 Outline Exoplanets at the E-ELT era I- The E-ELT project Telescope & context Instrumentation road map II- Exoplanetary science 2.1 Study of planet-forming regions 2.2 Exoplanetary system characterization (Architecture, Formation, Atmosphere)
3 The E-ELT Project The Telescope 39-m class telescope: largest opticalinfrared telescope in the world. (GMT = 25m; TMT = 30m) Novel 5 mirrors design Segmented-primary (M1) 800 segments, 1.4m size Adaptive assisted telescope M4 adaptive mirror, 5000 actuators Diffraction limited performance: 12mas@K-band; 7 arcmin patrol FoV Mid-latitude site (Amazones/Chile). Fast instrument changes.
4 The E-ELT Project E-ELT & other competitive projects Discoveries by opening a new parameter space Increased Sensitivity Spatial resolution (10 mas scale) 50m2 400m2 600m2 1200m2 (JWST: 25m2) 2 µm 50mas 18mas 14mas 10mas (JWST: 68mas)
5 The E-ELT Project Timeline: current/future missions Ground: Harps N/S, SOPHIE, NaCo, VISIR, CRIRES, WASP, Spirou, Carmenes Space: Spitzer, Herschel, Kepler, CoRoT - VLT & VLTI 2 nd & 3 rd generation K-MOS, SPHERE, MUSE, CRIRES+, ESPRESSO, GRAVITY, MATISSE - ALMA (ACA) - GAIA - Cheops - TESS - SKA - JWST - PLATO - WFIRST - TMT - GMT - E-ELT
6 The E-ELT Project Instrument Roadmap Instruments - First Light E-CAM 2024 E-IFU 2024 AO Mode λ (µm) Resolution FoV / Sampling Add. Mode SCAO, MCAO SCAO, LTAO - IMG - MRS BB, NB IFU / 3 mas Astrometry 40µas / 4mas / 40mas E-MIDIR 2025 SCAO LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Polarimetry E-HIRES /2028 SCAO - HRS Polarimetry E-MOS /2028 MOAO Slits IFUs IFUs / / / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS /2032 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry
7 The E-ELT Project Instrument Roadmap 1st Light Instruments Instruments - First Light E-CAM 2024 E-IFU 2024 AO Mode λ (µm) Resolution FoV / Sampling Add. Mode SCAO, MCAO SCAO, LTAO - IMG - MRS BB, NB IFU / 3 mas Astrometry 40µas / 4mas / 40mas E-MIDIR 2025 SCAO LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Polarimetry E-HIRES /2028 SCAO - HRS Polarimetry E-MOS /2028 MOAO Slits IFUs IFUs / / / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS /2032 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO MOAO: Multi-Object AO XAO: Extreme-AO
8 The E-ELT Project Instrument Roadmap 2 nd Pool Instruments Instruments - First Light E-CAM 2024 E-IFU 2024 AO Mode λ (µm) Resolution FoV / Sampling Add. Mode SCAO, MCAO SCAO, LTAO - IMG - MRS BB, NB IFU / 3 mas Astrometry 40µas / 4mas / 40mas E-MIDIR 2025 SCAO LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Polarimetry E-HIRES /2028 SCAO - HRS Polarimetry? E-MOS /2028 MOAO Slits IFUs IFUs / / / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS /2032 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO MOAO: Multi-Object AO XAO: Extreme-AO
9 The E-ELT Project Instrument Roadmap XAO Instrument Instruments - First Light E-CAM 2024 E-IFU 2024 AO Mode λ (µm) Resolution FoV / Sampling Add. Mode SCAO, MCAO SCAO, LTAO - IMG - MRS BB, NB IFU / 3 mas Astrometry 40µas / 4mas / 40mas E-MIDIR 2025 SCAO LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Polarimetry E-HIRES /2028 SCAO - HRS Polarimetry E-MOS /2028 MOAO Slits IFUs IFUs / / / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS /2032 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO MOAO: Multi-Object AO XAO: Extreme-AO
10 The E-ELT Project Instrument Roadmap Various AO Flavors Instruments - First Light E-CAM 2024 E-IFU 2024 AO Mode λ (µm) Resolution FoV / Sampling Add. Mode SCAO, MCAO SCAO, LTAO - IMG - MRS BB, NB IFU / 3 mas Astrometry 40µas / 4mas / 40mas E-MIDIR 2025 SCAO LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Polarimetry E-HIRES /2028 SCAO - HRS Polarimetry E-MOS /2028 MOAO Slits IFUs IFUs / / / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS /2032 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO MOAO: Multi-Object AO XAO: Extreme-AO
11 The E-ELT Project Instrument Roadmap Science Priority / Exoplanets Instruments - First Light E-CAM 2024 E-IFU 2024 AO Mode λ (µm) Resolution FoV / Sampling Add. Mode SCAO, MCAO SCAO, LTAO - IMG - MRS BB, NB IFU / 3 mas Astrometry 40µas / 4mas / 40mas E-MIDIR 2025 SCAO LTAO - IMG - MRS - IFU BB, NB / 12 mas / 4 mas Polarimetry E-HIRES /2028 SCAO - HRS Polarimetry E-MOS /2028 MOAO Slits IFUs IFUs / / / 40mas Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging? E-PCS /2032 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry Low Medium High
12 Outline Exoplanets at the E-ELT era I- The E-ELT project Telescope & context Instrumentation road map II- Exoplanetary science 2.1 Study of planet-forming regions 2.2 Exoplanetary system characterization (Architecture, Formation, Atmosphere)
13 2.1 Planet-forming regions. Star/disk Evolution o Accretion, Mass loss & Magnetic fields. Disk Structure & Dynamics o Gas & Dust components. Composition & Chemistry: o Water & Organics. Planetary Formation & Observation o Initial conditions. Planets/Disk interactions Key Scientific Questions Fomalhaut ALMA/HST Bowler et al. 12
14 2.1 Planet-forming regions Accessing the AU to the sub-au scale 1 L pc snow line Distance [AU] Temperature [K] Time 0.4 days 2 weeks 1 yr 30 yr 1000 yr E-ELT : 10 mas x 100pc = 1 AU E-MIDIR E-IFU, E-HIRES VLT/CRIRES ALMA
15 2.1 Planet-forming regions Accessing the AU to the sub-au scale 1 L pc Co-rotation radius Magnetospheric radius dust sublimation crystallization snow line Distance [AU] Temperature [K] Time 0.4 days 2 weeks 1 yr 30 yr 1000 yr E-ELT : 10 mas x 0.01 x 100pc = 0.01 AU Spectro-astrometry E-MIDIR E-IFU, E-HIRES VLT/CRIRES ALMA
16 2.1 Planet-forming regions E-IFU, E-HIRES & E-MIDIR Geometry of Accretion Channels Inner Disk Properties (Warp, asymmetries ) Role of Magnetic Fields (Config., Reconnection) Jet L aunching Zone, Stellar & Disk Winds (0.01 AU) Star/Disk interactions MHD star disk simulations R/Ro Spectro-astrometry E-ELT : 10 mas x 0.01 x 100pc = 0.01 AU = 2 Ro Zanni & Ferreira 09
17 2.1 Planet-forming regions Asymmetries/Spirals in proto-planetary disks Dusty Disk Structures E-CAM, MIDIR E-MIDIR simulations of high-contrast imaging at 10 µm. Jupiter footprint at 20 AU from G-star, Gap detection at a few mjy/as2 at (10 20 AU) ELT-MIR very competitive with JWST Grain differentiation with size Pressure Bump and dust trap Hot spot/proto-planets
18 2.1 Planet-forming regions Dusty Disk Structures Asymmetries/Spirals in proto-planetary disks E-CAM, MIDIR E-MIDIR simulations of high-contrast imaging at 10 µm. Jupiter footprint at 20 AU from G-star, Gap detection at a few mjy/as2 at (10 20 AU) ELT-MIR very competitive with JWST Grain differentiation with size Pressure Bump and dust trap Hot spot/proto-planets
19 2.1 Planet-forming regions Dusty Disk Structures Asymmetries/Spirals in proto-planetary disks E-CAM, MIDIR E-MIDIR simulations of high-contrast imaging at 10 µm. Jupiter footprint at 20 AU from G-star, Gap detection at a few mjy/as2 at (10 20 AU) ELT-MIR very competitive with JWST Grain differentiation with size Pressure Bump and dust trap Hot spot/proto-planets
20 2.1 Planet-forming regions Dusty Disk Structures Asymmetries/Spirals in proto-planetary disks E-CAM, MIDIR E-MIDIR simulations of high-contrast imaging at 10 µm. Jupiter footprint at 20 AU from G-star, Gap detection at a few mjy/as2 at (10 20 AU) ELT-MIR very competitive with JWST Grain differentiation with size Pressure Bump and dust trap Hot spot/proto-planets
21 E-MIDIR 2.1 Planet-forming regions Gas Distribution & Dynamics Proto-planetary disk of SR21 (Ophiucus, 160pc, 1 Myr) Gap at 18 AU (sub-mm continuum emission Brown e al. 07) E-ELT-MIDIR simulations of 12 CO line emission at 4.7µm of SR21. o Left: Continuum subtracted and velocity channel co-added o Right: Velocity map with a resolving power of (3 km/s) 32 AU
22 E-MIDIR 2.1 Planet-forming regions Proto-planet direct detection Proto-planetary disk in young SFRs (solar-type star, 150pc) 10 M Jup protoplanet at 30 AU surrounded by a circumplanetary disk E--MIDIR simulations of 12 CO line emission at 4.7µm, continuum subtracted
23 2.1 Planet-forming regions Gas Composition & Chemistry Water & Organics Distribution and Dynamics Disk cooling & Planetesimals formation Organic/Prebiotic chemistry (CH4, C2H2, HCN ) Isotopic Fractionation Water Transfer to Terrestrial Planets E-MIDIR. Keck-NIRSPEC. high HRS (R = ) in L-band.. Detection of H20 and OH radicals MIR lines. Hot (800K) water from the inner AUs DR Tau, AS 205 N; Salyk et al. 08
24 2.2 Exoplanets Characterization Artist s View ESO-PR-1106
25 2.2 Exoplanets Characterization. Architecture of Planetary Systems o Frequent of GP/Telluric planets o Dynamical evolution/stability. Formation/Internal Evolution of Young Planets o Accretion history/cooling. Physics of Planetary Atmospheres o Composition/Chemistry o Bio-Signatures Discovery Key Scientific Questions
26 2.2 Exoplanets Characterization Architecture & Formation/Evolution E-CAM, IFU, MIDIR, PCS Exoplanets, current view (2014)
27 2.2 Exoplanets Characterization Architecture & Formation/Evolution E-CAM, IFU, MIDIR, PCS At E-ELT 1 st Lights (2024):. RV, Astro., Transit & DI surveys over?. Complete census of nearby planetary systems? GAIA TESS, CHEOPS ESPRESSO SPHERE
28 2.2 Exoplanets Characterization Architecture & Formation/Evolution E-CAM, IFU, MIDIR, PCS At E-ELT 1 st Lights (2024):. RV, Astro., Transit & DI surveys over?. Complete census of nearby planetary systems? E-ELT High-contrast Imaging (CAM, IFU, MIDIR, PCS) Overlap btw techniques Planetary freq. at all Periods Global view of planetary systems architecture Dominant formation mechanisms Dynamical evolution & stability GAIA TESS, CHEOPS ESPRESSO PCS SPHERE
29 2.2 Exoplanets Characterization Young Jupiters Properties/History E-CAM, IFU, MIDIR, PCS Physics of Giant Planets Observables: Luminosity Orbital properties: a, e, i, Complementarity RV, Astr > Access Dynamical Mass Bpic; Lagrange et al. 09, 10, Chauvin et al. 12 Bonnefoy et al. 14
30 2.2 Exoplanets Characterization E-CAM, IFU, MIDIR, PCS Physics of Giant Planets Observables: Luminosity Orbital properties: a, e, i, Complementarity RV, Astr > Access Dynamical Mass Formation/Cooling Evolution Lum. Mass parameter space Calibrate model predictions Gas Accretion History Presence of a core Young Jupiters Properties/History Accretion Shock Cold-start Mordasini et al. 12 No Accretion Shock Hot start
31 2.2 Exoplanets Characterization Physics of the Planetary Atmosphere Wide orbit self-lum. planets High-contrast LRS High-contrast + HDS Close-in Irradiated planets Transmission/Eclipse LRS HDS
32 E-IFU, MIDIR, PCS 2.2 Exoplanets Characterization Physics of the Atmosphere i/ High-Contrast Low-Resolution Spectroscopy - Contrast Goal: 10-6 (50mas) to 10-9 (20mas) - Targets: M-dwarfs, young stars - Emitted (E-IFU, MIDIR) and Reflected (E-PCS) light of giant icy planets (Super-Earths?) - Broad molecular absorptions: H2O, CO, CH4, NH3, CO2
33 2.2 Exoplanets Characterization Physics of the Atmosphere i/ High-Contrast Low-Resolution Spectroscopy - Contrast Goal: 10-6 (50mas) to 10-9 (20mas) - Targets: M-dwarfs, young stars - Emitted (E-IFU, MIDIR) and Reflected (E-PCS) light of giant icy planets (Super-Earths?) - Broad molecular absorptions: H2O, CO, CH4, NH3, CO2 E-IFU, MIDIR, PCS Beta Pic b GPI and SPHERE Observations in J-band (Res = 50) 8 13 M Jup planet, 9 AU; T eff = K, log(g) = 4.0±0.5 and R = R jup H2O, FeH absorptions (Bonnefoy et al. 14)
34 E-MOS 2.2 Exoplanets Characterization Physics of the Atmosphere ii/ MOS Transit Medium-Resolution Spectroscopy - Photometric accuracy Goal: Targets: M dwarfs - Search for bio-signatures to telluric planets - Complementarity to JWST in visible: Presence of Haze
35 2.2 Exoplanets Characterization Physics of the Atmosphere ii/ MOS Transit Medium-Resolution Spectroscopy - Photometric accuracy Goal: Targets: M dwarfs - Search for bio-signatures to telluric planets - Complementarity to JWST in visible: Presence of Haze GJ3470 b Keck/MOSFIRE; FoV = 6 x 6 ; Reference stars; Spectral range= µm; Resolution = 3500 (OH lines); 10-4 photometric precision; Hot Neptune Transmission spectrum looks flat! Suggests hazes and/or disequilibrium chemistry E-MOS (Crossfield et al. 13)
36 2.2 Exoplanets Characterization Physics of the Atmosphere iii/ High-Dispersed Spectroscopy - Contrast: Targets: bright stars with close-in planets (>40) - Search for molecular absorptions of CO, H2O, CH4, NH3 - Mass, inclination, thermal inversion, C/O ratio, atmosphere circulation rotation E-HIRES, MIDIR HD b, Non-transiting planets VLT/CRIRES observations, Resolution = ; Spectral coverage = µm Dayside seen in CO, H2O Kp = ± 3.4 km/s Mass = 0.98 ± 0.04 MJup Incl = 67.7 ± 4.3 deg (Brogi et al. 14)
37 2.2 Exoplanets Characterization Physics of the Atmosphere E-MIDIR & new PCS? iv/ XAO High-Contrast + High-Dispersed Spectroscopy Powerful technique, capable to characterize rocky planets in HZ? Reflected light (from 10-4 to 10-9 contrast); Search for O2 and bio-signatures Snellen et al. 13 and Talk
38 2.2 Exoplanets Characterization Physics of the Atmosphere E-MIDIR & new PCS? iv/ XAO High-Contrast + High-Dispersed Spectroscopy Powerful technique, capable to characterize rocky planets in HZ? Reflected light (from 10-4 to 10-9 contrast); Search for O2 and bio-signatures Doppler imaging mapping of Exoplanets: Cloud/Molecular Coverage Luhman 16 B, 2 pc, Rotation 4.9hrs spectroscopic variability (Crossfield et al. 14)
39 Conclusions The E-ELT project > Unique Spatial resolution & sensitivity > Offering a versatile instrumentation (wavelengths coverage, modes, spatial/spectral resolution ) > Will count on new discoveries (ALMA, SPHERE, GPI, GAIA, TESS...) > Mostly aimed at Characterizing, but not only Exoplanetary science > Observing planet-forming regions ( AU scale) > Initial conditions for planetary formation (Disk Structure, Composition & Chemistry) > Overlap btw observing techniques Architecture of planetary systems (Global view) Physics of Young Jupiters (Formation, Accretion) > Atmospheres Giant/Icy to Sper-Earths, T/P structure, composition, C/O ratio, cloud coverage & variab. Path toward characterization of exo-earths atmospheres
40 Thank you Cerro Amazones, Sep 12th, 2014
41
42 2.2 Exoplanets Characterization E-HIRES, E-MIDIR, E-PCS Planetary Atmospheres Reflected, Transmitted or Emitted light of Exoplanets Strongly or non-strongly irradiated planets Physics of Planetary Atmospheres (Giant, Exo-Neptunes to Super-Earths) - Geometric Albedos - Chemical Composition (H20, CH4, CO, CO2, NH3 ) - Atmosphere s Dynamics. Inversion,. Vertical Mixing,. Circulation,. Evaporation, Imprints of Formation Mechanisms? No Thermal Inversion Thermal inversion Knutson et al. 09 Spitzer
43 2.2 Exoplanets Characterization Physics of the Atmosphere iii/ High-Dispersed Spectroscopy
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