Exoplanetary Science with the E-ELT
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1 SF2A, MONTPELLIER, 4-7 JUNE 2013 Exoplanetary Science with the E-ELT Gaël Chauvin - IPAG/CNRS - Institute of Planetology & Astrophysics of Grenoble/France In Collaboration with ESO-PST, and E-ELT CAM, IFU, MIDIR, MOS, HIRES & PCS consortium
2 Outline Exoplanetary Science with the E-ELT I- The E-ELT project II- Planet-forming Zones III- Exoplanetology IV- Planetary Archeology
3 I- The E-ELT Project The Telescope 40-m class telescope: largest opticalinfrared telescope in the world. (GMT = 25m; TMT = 30m) Segmented primary mirror. Adaptive optics assisted telescope. Wide field of view: 7 arcmin. Exquisite spatial resolution > 12mas@K-band Unprecedented sensitivity
4 I- The E-ELT Project Timeline: current/future missions Ground: Harps N/S, SOPHIE, NaCo, VISIR, CRIRES, WASP Space: Spitzer, Herschel, Kepler, CoRoT - VLT & VLTI 2 nd & 3 rd generation PRIMA, K-MOS, SPHERE, MUSE, ESPRESSO, GRAVITY - ALMA (ACA) - GAIA - Cheops - TESS - SKA - JWST - EChO/PLATO/FINESS? - TMT - GMT - E-ELT
5 I- The E-ELT Project Instrument Roadmap Instruments - First Light E-CAM 2023 E-IFU 2023 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 2024/2028 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 /2030 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry
6 I- The E-ELT Project 1st Light Instruments Instrument Roadmap Instruments - First Light E-CAM 2023 E-IFU 2023 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 2024/2028 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 /2030 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
7 I- The E-ELT Project 2 nd Pool Instruments Instrument Roadmap Instruments - First Light E-CAM 2023 E-IFU 2023 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 2024/2028 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 /2030 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 I- The E-ELT Project XAO Instrument Instrument Roadmap Instruments - First Light E-CAM 2023 E-IFU 2023 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 2024/2028 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 /2030 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 I- The E-ELT Project Science Priority / Exoplanets Instrument Roadmap Instruments - First Light E-CAM 2023 E-IFU 2023 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 2024/2028 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 /2030 XAO EPOL IFS / 2.3 mas 0.8 / 1.5 mas Polarimetry Low Medium High
10 II- Planet-Forming Zones Artist s View ESO-PR-0942
11 II- Planet-Forming Zones Key Scientific Questions. Disk Structure & Dynamics (Gas & Dust). Chemistry: Water & Organics in Planet-Forming Zones. Planetary Formation o Initial conditions. Planets/Disk interactions Fomalhaut ALMA/HST Bowler et al. 12
12 II- Planet-Forming Zones 1 L pc E-ELT s View of Circumstellar Environment 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 100pc = 1 AU E-MIDIR E-IFU, E-HIRES VLT/CRIRES ALMA
13 II- Planet-Forming Zones 1 L pc E-ELT s View of Circumstellar Environment 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
14 E-MIDIR II- Planet-Forming Zones Proto-planetary disk of SR21 (Ophiucus, 160pc, 1 Myr) Gap at 18 AU (sub-mm continuum emission Brown e al. 07) Gas Dynamics 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
15 E-MIDIR II- Planet-Forming Zones Gas Dynamics Water & Organics Distribution and Dynamics Disk cooling & Planetesimals formation Organic/Prebiotic chemistry (CH4, C2H2, HCN ) Isotopic Fractionation Transfer to Terrestrial Planets. 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
16 E-MIDIR II- Planet-Forming Zones Asymmetries/Spirals in proto-planetary disks Observing Planetary Formation 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
17 E-MIDIR II- Planet-Forming Zones Observing Planetary Formation Asymmetries/Spirals in proto-planetary disks 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
18 E-MIDIR II- Planet-Forming Zones Observing Planetary Formation Asymmetries/Spirals in proto-planetary disks 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
19 E-MIDIR II- Planet-Forming Zones Observing Planetary Formation Asymmetries/Spirals in proto-planetary disks 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
20 III- Exoplanets Artist s View ESO-PR-1106
21 III- Exoplanets Key Scientific Questions. Architecture of Exoplanetary Systems?. Formation & Evolution Processes. How does it depend on the Host properties? (Mass, Age, Composition ). How frequent are the Telluric planets in the HZ?. Physics & Atmosphere of Exoplanets? (Telluric & Giant). Bio-Signatures Discovery & Conditions favorable for Life?
22 III- Exoplanets Exploration of Telluric Planets Expected planet population detected by Doppler spectroscopy with: o HARPS on the ESO 3.6-metre (precision 1 ms 1), Observed (Mayor et al. 11) Predicted (Mordasini et al. 09) corrected observed
23 E-HIRES III- Exoplanets Exploration of Telluric Planets Expected planet population detected by Doppler spectroscopy with: o HARPS on the ESO 3.6-metre (precision 1 ms 1; left), o ESPRESSO on the VLT(precision 10 cms 1; middle) o and HIRES on the E-ELT(precision 1 cms 1; right). > HIRES, required to detect Earth-like planets in HZ of solar-type stars
24 E-HIRES III- Exoplanets Twin Earth Discovery Simulations: 1.8 M Earth Exo-Earth in HZ (P=145 days) around a bright and low-activity K1V star. RV precision: 1 cm/s. Limitations: instr. noise, stellar oscillations, granulation and activity. Dedicated observing strategy: 3 meas./night, every 3 nights over 8 months Periodogram: 3σ detection (red)
25 E-HIRES, E-MIDIR, E-PCS III- Exoplanets 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? Secondary-Eclipse/Strongly irradiated GPs; Knutson et al. 09 No Thermal Inversion Thermal inversion Spitzer
26 E-IFU, E-MIDIR, E-PCS III- Exoplanets Physics of Giant Planets (down to Super-Earths) Observables: Luminosity, Teff & Gravity Atmospheric properties Orbital properties: a, e, i, Complementarity RV, Astr > Access Dynamical Mass Imaging Planetary Systems Hd95086; Rameau et al. 13 January 11 th, 2012 Bpic; Lagrange et al. 10 HR8799; Marois et al. 10 NaCo (Lp) 0.5 ESO-PR-1324 (June 3 rd, 2013)
27 E-IFU, E-MIDIR, E-PCS III- Exoplanets Physics of Giant Planets (down to Super-Earths) Observables: Luminosity, Teff & Gravity Atmospheric properties Orbital properties: a, e, i, Complementarity RV, Astr > Access Dynamical Mass Imaging Planetary Systems GAIA SPHERE E-IFU/MIDIR Mesa et al. 11 Kasper et al. 10 Lattanzi & Sozzetti 10 E-PCS
28 E-IFU, E-MIDIR, E-PCS III- Exoplanets Physics of Giant Planets (down to Super-Earths) Observables: Luminosity, Teff & Gravity Atmospheric properties Orbital properties: a, e, i, Complementarity RV, Astr > Access Dynamical Mass Imaging Planetary Systems Mordasini et al. 12 No Accretion Shock Formation/Evolution Theories L Mass Relation Gas Accretion Phase Accretion Shock
29 E-IFU, E-MIDIR, E-PCS III- Exoplanets Physics of Giant Planets (down to Super-Earths) Observables: Luminosity, Teff & Gravity Atmospheric properties Orbital properties: a, e, i, Complementarity RV, Astr > Access Dynamical Mass Imaging Planetary Systems Formation/Evolution Theories L Mass Relation Gas Accretion Phase Planetary System Architecture Dynamical stability Planet-disk interactions Bpic b; ESO PR 0842
30 IV- Planetary Archeology Artist s View NASA/JPL CALTECH
31 IV- Planetary Archeology White dwarfs polluted by planetary debris Photospheric abundances: Fe, Si, Ca, C, O, Mg abundances Physical/Chemical properties of WD circumstellar disks Frequency of terrestrial planet building Bulk chemistry of solid planetary bodies Mass constraints for exoplanetary building blocks Frequency of water-rich exo-asteroids Constraints on habitable environments Farihi et al. 2010
32 Want to know more The E-ELT Science Case: The E-ELT Design Reference Mission: drm_report.pdf The science users web pages: Shaping the E-ELT Conference (Fév 2013) The PNPS E-ELT Workshop (Fréjus, Fev 2013) E-ELT Exoplanetary Science Colloquium (2.2014)
33 Thank You!
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35 E-IFU, E-HIRES & E-MIDIR 1/ Disks Star disk interactions Star/Disk evolution under the microscope Geometry of Accretion Channels Inner Disk Properties (Warp, asymmetries ) Role of Magnetic Fields (Config., Reconnection) Jet L aunching Zone, Stellar & Disk Winds E-ELT : 10 mas x 0.01 x 100pc = 0.01 AU = 2 Ro. VLT/CRIRES, CO emission lines at 4.7µm (< 2 AU) AS 205 N, Pontopiddan et al. 11
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