A New Era with E-ELT Drivers for circumstellar environment studies

PNPS-EELT Workshop February, 4-5th 2013, Fréjus A New Era with E-ELT Drivers for circumstellar environment studies Gaël Chauvin - IPAG/CNRS - Institute of Planetology & Astrophysics of Grenoble/France

Outline A New Era with E-ELT I- Roadmap for the E-ELT II- Science drivers for circumstellar environment 2.1 Star Disk interaction: Accretion/Outflows 2.2 Proto-planetary disks, debris disks & exo-zodiacal dust 2.3 Characterizing Exoplanets 2.4 Multiplicity in SFRs & IMF (> E. Moraux s Talk) 2.5 Environment of Evolved stars III/ Conclusions

I/ E-ELT Roadmap Synergy: current/future missions 2014 2016 2018 2020 2022 2024 2026 2028 Ground: Harps N/S, SOPHIE, NaCo, VISIR, CRIRES, WASP Space: Spitzer, Herschel, WISE, Corot, Kepler, VLT & VLTI 2 nd generation XShooter, PRIMA, K-MOS, SPHERE, MUSE, GRAVITY ALMA (ACA) GAIA 2013 SKA 2016 Cheops 2017 JWST 2018 Echo 2022 (?) Plato 2022 (?) NEAT 2025 (?) TMT 2022 GMT 2022 E-ELT 2022

Discoveries by opening a new parameter space Increased Sensitivity Spatial resolution (10 mas scale) I/ E-ELT Roadmap E-ELT & other competitive projects 50m2 400m2 600m2 1200m2 (JWST: 25m2) 1 µm 25mas 9mas 7mas 5mas (JWST: 34mas)

I/ E-ELT Roadmap Call for E-ELT Instruments

I/ E-ELT Roadmap Selection & Agenda Instruments AO Mode λ (µm) Resolution FoV & Sampling Add. mode ELT-1: CAM (MICADO) SCAO, MCAO - IMG - MRS 0.8 2.4 3000 53.0 / 3 mas Corono ELT-2 IFU (HARMONI) SCAO, LTAO - IFU (0.5) 2.4 4000 10 000 20 000 0.5*1.0-5.0*10.0 / 4 40 mas Corono ELT-3: MIR (METIS) SCAO, LTAO - IMG - MRS - IFU 3 13 3-5 5000 100 000 18 / 12 mas 0.4*1.5 / 4 mas Corono Polar. ELT-4/5: HIRES (CODEX/SIMPLE) No AO SCAO, MCAO, LTAO - HRS 0.37 0.71 0.84 2.50 130 000 130 000 0.82 0.027 *0.5 ELT-4/5: MOS (EAGLE/EVE/ DIORAMA) No AO, GLAO MCAO Slits IFUs IFUs 0.37 1.4 0.37 1.4 0.8 2.45 300-2500 5000 30 000 4000 10 000 6.8 420 420 ELT-X: PCS (EPICS) XAO EPOL IFS 0.6 0.9 0.95 1.65 125 20 000 2.0 / 2.3 mas 0.8 / 1.5 mas Corono Polar.

I/ E-ELT Roadmap Selection & Agenda

2.1 Star disk interactions, Jets and Outflows Science drivers for E-ELT: Inner disk structure (warp and asymmetries) Link to stellar magnetosphere Accretion flows (non steady accretion processes). Outflows nature: o steady (disk wind) o outburst (magneto-spheric ejections) Geometry of Jets & Outflows (collimation?) Romanova et al. 12

Star disk interactions at sub-au scale The AA Tau case Bouvier et al. 07 Light curve: periodical (~ 8.2 days) eclipses. Linear polarization increases as system fades. Periodical occultation by an optically thick, magnetically-warped inner disk region Periodic accretion shock synchronized with the disk warp Spectral lines: HeI, Balmer, Paschen, CaII

Jet and outflows geometry and kinematics Meliani et al. 07, Zani et al. 13 The young BD 2M1207 Jet launching region, kinematics and Collimation at < Aus Physical conditions (Excitation, temperature & density) Mass loss to mass accretion rate (mass dependence) Spectral lines: [SII], [OII], [OI], [NII], [FeII] Whelan et al. 07, 13 Artist s View

2.1 Star disk interactions, Jets and Outflows Diagnostics, Techniques & Requirements: Spectral lines (Balmer, Paschen and Brackett lines, S[II], HeI, FeII...) Spectral line imaging and/or spectro-astrometry HAR:10mas (1.5 AU at 150pc); Spectro-astrometry (0.015 AU) Visible, and NIR wavelengths (0.5 2.5 um) Spectral resolution (up to 20 000 to access velocity of a few km/s) Temporal resolution (from a few seconds to hrs) Most adapted instrument at E-ELT? EELT-IFU, IFU facility from visible to NIR. Interest in going to MIR (ELT-MIR/IFU?) 2D field velocity & adapted spectral coverage for the lines of interest

Gas dynamics in the proto-planetary disk of SR21 (Ophiucus, 160pc, 1 Myr) Dust Gap at 18 AU (sub-mm continuum emission Brown e al. 07) VLT/CRIRES (R = 100 000) Spectro-astrometry CO v=1.0 ro-vibration line at 4.7um > Tracer for warm gas in the inner disk CO emission within a ring cut at 7 AU Dust gap formation by grain growth? Companion at less than 4AU? Pontoppidan et al. 08, 10

Gas dynamics in the proto-planetary disk of SR21 (Ophiucus, 160pc, 1 Myr) Dust Gap at 18 AU (sub-mm continuum emission Brown e al. 07) E-ELT-MIR simulations of 12 CO line emission at 4.7um of SR21. o Left: Continuum subtracted and velocity channel co-added o Right: Velocity map with a resolving power of 100 000 (3 km/s) Brandl et al. 12 16 AU

Water in the planet-forming zones of DR Tau and AS 205N Keck-NIRSPEC high resolution (R = 25 000) spectroscopy in L-band Detection of strong MIR lines of H20 and related OH radicals Hot (800K) water detected probably from the inner AUs Salyk et al. 08

Imaging gaps and asymmetries in proto-planetary disks ELT-MIR simulations of high-contrast imaging at 10 µm. Jupiter footprint at 20 AU (@100pc) from G-star? Gap detection at a few mjy/as2 at 0.1-0.2 (10 20 AU) ELT-MIR very competitive with JWST (spatial resolution and sensitivity) Eric s Talk

2.2 Physics of proto-planetary and debris disks Diagnostics, Techniques & Requirements: Molecular lines (CO, H2, H20, OH, CH4, C2H2, HCN...) and Si/PAH signatures Visible, NIR and MIR (0.5 13 µm) Spectral resolution (up to 100 000 to access velocity of a few km/s) Imaging at AU scale & Spectral line imaging, spectro-astrometry HAR and High-contrast: o SCAO o Coronagraphy o differential imaging techniques Most adapted instrument at E-ELT? Imaging: EELT-CAM and MIR, then ELT-PCS Spectral line IMG: EELT-IFU and MIR, IFU facility from visible to NIR and LM

2.3 Exoplanets Characterization Science drivers for E-ELT: Detection of Exo-Earths, particularly an Earth-Twin Super-Earth to Giant Planet Imaging. Planet disk interactions Characterization of Super-Earths to Super Jupiters at all orbits o Frequency & multiple systems o Orbital & physical properties o Atmosphere (composition, evaporation...) o Dependence on stellar properties (mass, age, metallicity & binarity) Planetary formation & evolution mechanisms o Connection to the stellar properties o to the planet properties (composition, orbital & physical properties) Temporal variation of planet's properties o Atmospheric circulation (day/night variation) o Weather forecast (clouds formation) o Star planet magnetic interactions

An Earth-mass planet orbiting Alpha Centauri B ESO3.6m/HARPS observations Dealing with: instrumental noise, stellar oscillation, granulatio, rotation, longterm activity, contamination and binary signal. Alpha Cen Bb: T = 3.23 days M = 1.13±0.09 M Earth K = 0.51 m/s ecc = 0.0 (fixed) Dumusque et al. 12

Twin-Earth with E-ELT-HIRES Simulations of 1.8 M Earth Exo-Earth in HZ (P=145 days) around a bright and lowactivity K1V star. Limitations: instrumental noise, stellar oscillations, granulation and activity. Detailed observing strategy: 3 meas./night every 3 nights over 8 months Periodogram: 3σ detection (red)

Population of closed-in telluric and giant 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

Imaging Giant Planets to Super Earths VLT/NaCo ADI High-contrast imaging in NIR & LM β Pic b planet (Lagrange et al. 08), o Sep = 400 mas o ΔJ = 10.6+-0.3 mag, o 12 Myr @ 19.3 pc, o > Mass = 7 8 Mjup ( Hot-Start ) Atmospheric properties Bonnefoy et al. 13

Characterizing Giant Planets to Super Earths http://exoplanet.eu/ GAIA SPHERE ELT-PCS ELT-HIRES Mesa et al. 11 Kasper et al. 10 Lattanzi & Sozzetti 10 >> Synergy btw the different observing techniques

2.3 Exoplanets Characterization Diagnostics, Techniques & Requirements: High-Contrast Imaging from VIS to MIR at diffraction limit (XAO, coronagraphic, differential imaging ) LRS to MRS spectroscopy from NIR to MIR (Atmosphere) HRS (R > 100 000) spectroscopy for RV High astrometric accuracy(50 µas) High photometric accuracy(transit) Most adapted instrument at E-ELT? Imaging: EELT-IFU and MIR, then ELT-PCS LRS & MRS spectro: EELT-IFU and MIR HRS spectro: EELT-HIRES Transit: EELT-MIR, CAM, IFU?

2.5 Evolved stars Science drivers for E-ELT: Outflows geometry Interacting binaries and wind-wind collision Jet in cataclysmic variables and symbiotic system Disks around evolved stars Plasma disks around massive interacting systems Diagnostics, Techniques & Requirements: Similar to Accretion/Outflows Similar to Disks Most adapted instrument at E-ELT? Imaging: EELT-CAM and MIR, then ELT-PCS Spectral line IMG: EELT-IFU and MIR, IFU facility from visible to NIR and LM VLT/NaCo (Chesneau et al. 07)

III- Conclusions E-ELT, ideal for the future exploration of the circumstellar environment o Star disk interaction at sub-au scale (IFU) o Gas and dust component of proto-planetary disks (MIR) o Exoplanet Characterization (PCS) Still a lot to learn & develop, o o o MIR Sensitivity (MIR): Aquarius detectors on VISIR XAO design (PCS): SPHERE & GPI HRS (HIRES): HARPS & ESPRESSO and observing strategy for exo-earths BUT, o first-light instruments (-CAM and IFU, 2022) driven by the X-Gal community o Less interest for high-contrast imaging or HRS capabilities / MOS? o HIRES, PCS should not arrive before 2026-2028 o Must support Top Level Requirements that would serve the Stellar Community >> Exple: coronagraphic mode on CAM and IFU (disk & exoplanets) >> Astrometric precision on CAM for astrometric planet search >> Polarimetric capabilities of the E-ELT