Download Exo-planets Direct Imaging

AO4ELT3 CONFERENCE. FLORENCE, ITALY, 26-31 MAY 2013
E-ELT’s View
of Stellar Environments
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
Outline
E-ELT’s View of Stellar Environments
I- The E-ELT project
• Telescope, Discovery Window, Other Projects
• Instrumentation Road Map
II- Stellar Environments
• Disks
• Exoplanets
• Evolved Stars
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.
• Diffraction limited performance:
12mas@K-band
Wide field of view: 7arcmin.
• Mid-latitude site (Amazones/Chile).
Fast instrument changes.
VLT level of operations efficiency.
The E-ELT Project
E-ELT & other competitive projects
Discoveries by opening a new parameter space
• Increased Sensitivity
• Spatial resolution (10 mas scale)
2 µm
50m2
50mas
400m2
18mas
600m2
14mas
1200m2
10mas
(JWST: 25m2)
(JWST: 68mas)
The E-ELT Project
Timeline: current/future missions
2012
2014
2016
2018
2020
2022
2024
Ground: Harps N/S, SOPHIE, NaCo, VISIR, CRIRES, WASP…
Space: Spitzer, Herschel, Kepler, CoRoT
- VLT & VLTI 2nd & 3rd generation
PRIMA, K-MOS, SPHERE, MUSE, ESPRESSO, GRAVITY…
- ALMA (ACA)
- GAIA
- Cheops
- TESS
- SKA
- JWST
- EChO/PLATO/FINESS?
- TMT
- GMT
- E-ELT
2026
2028
The E-ELT Project
Instrument Roadmap
Instruments
- First Light
AO
Mode
λ (µm)
Resolution
FoV / Sampling
Add. Mode
E-CAM
– 2023
SCAO,
MCAO
- IMG
- MRS
0.8 – 2.4
BB, NB
3000
53.0” / 3 mas
Astrometry 40mas
Coronography
E-IFU
– 2023
SCAO,
LTAO
- IFU
0.5 – 2.4
4000
10 000
20 000
0.5×1.0” / 4mas
5.0×10.0” / 40mas
Coronography
E-MIDIR
– 2024/2028
SCAO,
LTAO
- IMG
- MRS
- IFU
3 – 13
3 - 13
3-5
BB, NB
5000
100 000
18” / 12 mas
Coronography
Polarimetry
SCAO
- HRS
0.37 – 0.71
0.84 – 2.50
200 000
120 000
0.82”
0.027”×0.5”
Polarimetry
MOAO
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” / 0.1”
420’ / 0.3”
2” / 40mas
Multiplex ~ 400
Multiplex ~100
Multiplex ~10
Imaging?
EPOL
IFS
0.6 – 0.9
0.95 – 1.65
125 – 20 000
2.0” / 2.3 mas
0.8“ / 1.5 mas
Coronography
Polarimetry
E-HIRES
- 2024/2028
E-MOS
- 2024/2028
E-PCS
- 2027/2030
XAO
0.4”×1.5” / 4 mas
The E-ELT Project
Instrument Roadmap
• 1st Light Instruments
Instruments
- First Light
AO
Mode
λ (µm)
Resolution
FoV / Sampling
Add. Mode
E-CAM
– 2023
SCAO,
MCAO
- IMG
- MRS
0.8 – 2.4
BB, NB
3000
53.0” / 3 mas
Astrometry 40mas
Coronography
E-IFU
– 2023
SCAO,
LTAO
- IFU
0.5 – 2.4
4000
10 000
20 000
0.5×1.0” / 4mas
5.0×10.0” / 40mas
Coronography
E-MIDIR
– 2024/2028
SCAO,
LTAO
- IMG
- MRS
- IFU
3 – 13
3 - 13
3-5
BB, NB
5000
100 000
18” / 12 mas
Coronography
Polarimetry
SCAO
- HRS
0.37 – 0.71
0.84 – 2.50
200 000
120 000
0.82”
0.027”×0.5”
Polarimetry
MOAO
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” / 0.1”
420’ / 0.3”
2” / 40mas
Multiplex ~ 400
Multiplex ~100
Multiplex ~10
Imaging?
EPOL
IFS
0.6 – 0.9
0.95 – 1.65
125 – 20 000
2.0” / 2.3 mas
0.8“ / 1.5 mas
Coronography
Polarimetry
E-HIRES
- 2024/2028
E-MOS
- 2024/2028
E-PCS
- 2027/2030
XAO
SCAO: single-conjugated AO
MCAO: Multi-Conjugated-AO
MOAO: Multi-Object AO
XAO: Extreme-AO
0.4”×1.5” / 4 mas
LTAO: Laser-Tomographic AO
The E-ELT Project
•
2nd
Instrument Roadmap
Pool Instruments
Instruments
- First Light
AO
Mode
λ (µm)
Resolution
FoV / Sampling
Add. Mode
E-CAM
– 2023
SCAO,
MCAO
- IMG
- MRS
0.8 – 2.4
BB, NB
3000
53.0” / 3 mas
Astrometry 40mas
Coronography
E-IFU
– 2023
SCAO,
LTAO
- IFU
0.5 – 2.4
4000
10 000
20 000
0.5×1.0” / 4mas
5.0×10.0” / 40mas
Coronography
E-MIDIR
– 2024/2028
SCAO,
LTAO
- IMG
- MRS
- IFU
3 – 13
3 - 13
3-5
BB, NB
5000
100 000
18” / 12 mas
Coronography
Polarimetry
SCAO
- HRS
0.37 – 0.71
0.84 – 2.50
200 000
120 000
0.82”
0.027”×0.5”
Polarimetry
MOAO
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” / 0.1”
420’ / 0.3”
2” / 40mas
Multiplex ~ 400
Multiplex ~100
Multiplex ~10
Imaging?
EPOL
IFS
0.6 – 0.9
0.95 – 1.65
125 – 20 000
2.0” / 2.3 mas
0.8“ / 1.5 mas
Coronography
Polarimetry
E-HIRES
- 2024/2028
E-MOS
- 2024/2028
E-PCS
- 2027/2030
XAO
SCAO: single-conjugated AO
MCAO: Multi-Conjugated-AO
MOAO: Multi-Object AO
XAO: Extreme-AO
0.4”×1.5” / 4 mas
LTAO: Laser-Tomographic AO
The E-ELT Project
Instrument Roadmap
• XAO Instrument
Instruments
- First Light
AO
Mode
λ (µm)
Resolution
FoV / Sampling
Add. Mode
E-CAM
– 2023
SCAO,
MCAO
- IMG
- MRS
0.8 – 2.4
BB, NB
3000
53.0” / 3 mas
Astrometry 40mas
Coronography
E-IFU
– 2023
SCAO,
LTAO
- IFU
0.5 – 2.4
4000
10 000
20 000
0.5×1.0” / 4mas
5.0×10.0” / 40mas
Coronography
E-MIDIR
– 2024/2028
SCAO,
LTAO
- IMG
- MRS
- IFU
3 – 13
3 - 13
3-5
BB, NB
5000
100 000
18” / 12 mas
Coronography
Polarimetry
SCAO
- HRS
0.37 – 0.71
0.84 – 2.50
200 000
120 000
0.82”
0.027”×0.5”
Polarimetry
MOAO
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” / 0.1”
420’ / 0.3”
2” / 40mas
Multiplex ~ 400
Multiplex ~100
Multiplex ~10
Imaging?
EPOL
IFS
0.6 – 0.9
0.95 – 1.65
125 – 20 000
2.0” / 2.3 mas
0.8“ / 1.5 mas
Coronography
Polarimetry
E-HIRES
- 2024/2028
E-MOS
- 2024/2028
E-PCS
- 2027/2030
XAO
SCAO: single-conjugated AO
MCAO: Multi-Conjugated-AO
MOAO: Multi-Object AO
XAO: Extreme-AO
0.4”×1.5” / 4 mas
LTAO: Laser-Tomographic AO
The E-ELT Project
Instrument Roadmap
• Various AO Flavors
Instruments
- First Light
AO
Mode
λ (µm)
Resolution
FoV / Sampling
Add. Mode
E-CAM
– 2023
SCAO,
MCAO
- IMG
- MRS
0.8 – 2.4
BB, NB
3000
53.0” / 3 mas
Astrometry 40mas
Coronography
E-IFU
– 2023
SCAO,
LTAO
- IFU
0.5 – 2.4
4000
10 000
20 000
0.5×1.0” / 4mas
5.0×10.0” / 40mas
Coronography
E-MIDIR
– 2024/2028
SCAO,
LTAO
- IMG
- MRS
- IFU
3 – 13
3 - 13
3-5
BB, NB
5000
100 000
18” / 12 mas
Coronography
Polarimetry
SCAO
- HRS
0.37 – 0.71
0.84 – 2.50
200 000
120 000
0.82”
0.027”×0.5”
Polarimetry
MOAO
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” / 0.1”
420’ / 0.3”
2” / 40mas
Multiplex ~ 400
Multiplex ~100
Multiplex ~10
Imaging?
EPOL
IFS
0.6 – 0.9
0.95 – 1.65
125 – 20 000
2.0” / 2.3 mas
0.8“ / 1.5 mas
Coronography
Polarimetry
E-HIRES
- 2024/2028
E-MOS
- 2024/2028
E-PCS
- 2027/2030
XAO
SCAO: single-conjugated AO
MCAO: Multi-Conjugated-AO
MOAO: Multi-Object AO
XAO: Extreme-AO
0.4”×1.5” / 4 mas
LTAO: Laser-Tomographic AO
The E-ELT Project
• Science Priority / Stellar Environments
Instrument Roadmap
Instruments
- First Light
AO
Mode
λ (µm)
Resolution
FoV / Sampling
Add. Mode
E-CAM
– 2023
SCAO,
MCAO
- IMG
- MRS
0.8 – 2.4
BB, NB
3000
53.0” / 3 mas
Astrometry 40mas
Coronography
E-IFU
– 2023
SCAO,
LTAO
- IFU
0.5 – 2.4
4000
10 000
20 000
0.5×1.0” / 4mas
5.0×10.0” / 40mas
Coronography
E-MIDIR
– 2024/2028
SCAO,
LTAO
- IMG
- MRS
- IFU
3 – 13
3 - 13
3-5
BB, NB
5000
100 000
18” / 12 mas
Coronography
Polarimetry
SCAO
- HRS
0.37 – 0.71
0.84 – 2.50
200 000
120 000
0.82”
0.027”×0.5”
Polarimetry
MOAO
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” / 0.1”
420’ / 0.3”
2” / 40mas
Multiplex ~ 400
Multiplex ~100
Multiplex ~10
Imaging?
EPOL
IFS
0.6 – 0.9
0.95 – 1.65
125 – 20 000
2.0” / 2.3 mas
0.8“ / 1.5 mas
Coronography
Polarimetry
E-HIRES
- 2024/2028
E-MOS
- 2024/2028
E-PCS
- 2027/2030
Low
XAO
Medium
0.4”×1.5” / 4 mas
High
Outline
E-ELT’s View of Stellar Environments
I- The E-ELT project
• Telescope, Discovery Window, Other Projects
• Instrumentation Road Map
II- Stellar Environments
• Disks
• Exoplanets
• Evolved Stars
Stellar Environments
1/ Circumstellar Disks
Artist’s View ESO-PR-0942
1/ Disks
Key Scientific Questions
. Star/disk Evolution
o Accretion, photo-evaporation,
o Jets & Winds
o Magnetic Fields
. 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
1/ Disks
Probing Planet-forming Regions
snow line
1 Lsun
@100 pc
Distance
Temperature
Time
E-ELT :
10 mas x 100pc
0.01
3000
0.4 days
0.1
1000
2 weeks
1.0
300
1 yr
10.0
100
30 yr
E-MIDIR
100.0
30
1000 yr
[AU]
[K]
VLT/CRIRES
1/ Disks
Star – disk interactions
Co-rotation radius
Magnetospheric radius
dust sublimation
1 Lsun
@100 pc
Distance
Temperature
Time
snow line
crystallization
0.01
3000
0.4 days
E-ELT :
10 mas x 0.01 x 100pc
0.1
1000
2 weeks
1.0
300
1 yr
Spectro-astrometry
10.0
100
30 yr
E-MIDIR
100.0
30
1000 yr
[AU]
[K]
VLT/CRIRES
E-IFU, E-HIRES & E-MIDIR
1/ Disks
Star – disk interactions
Star/Disk evolution under the microscope…
•
•
•
•
Geometry of Accretion Channels
E-ELT : 10 mas x 0.01 x 100pc
Inner Disk Properties (Warp, asymmetries…)
= 0.01 AU
Role of Magnetic Fields (Config., Reconnection)
= 2 Ro
Jet Launching Zone,
MHD star – disk simulations
Stellar & Disk Winds
R/Ro
Zanni & Ferreira 09
1/ Disks
Gas Dynamics in planet-forming zones
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 12CO 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 100 000 (3 km/s)
E-MIDIR
32 AU
1/ Disks
Gas Dynamics in planet-forming zones
Water & Organics
E-MIDIR
• Distribution and Dynamics
• Disk cooling & Planetesimals formation
• Organic/Prebiotic chemistry
(CH4, C2H2, HCN…)
• Isotopic Fractionation
• Transfer to Terrestrial Planets
. Keck-NIRSPEC
. high HRS (R = 25 000) 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
1/ Disks
Observing the Dusty Disk Structures
Asymmetries/Spirals in proto-planetary disks
E-MIDIR
• E-MIDIR 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
1/ Disks
Observing the Dusty Disk Structures
Asymmetries/Spirals in proto-planetary disks
E-MIDIR
• E-MIDIR 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
1/ Disks
Observing the Dusty Disk Structures
Asymmetries/Spirals in proto-planetary disks
E-MIDIR
• E-MIDIR 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
1/ Disks
Observing the Dusty Disk Structures
Asymmetries/Spirals in proto-planetary disks
E-MIDIR
• E-MIDIR 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
Stellar Environments
2/ Exoplanets
Artist’s View ESO-PR-1106
2/ 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?
2/ 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)
corrected
observed
Predicted (Mordasini et al. 09)
2/ Exoplanets
E-HIRES
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
E-HIRES
2/ Exoplanets
Twin Earth Discovery
• Simulations: 1.8 MEarth Exo-Earth in HZ (P=145 days)
around a bright and low-activity K1V star.
• RV precision: 2cm/s. Limitations: instr. noise, stellar oscillations,
granulation and activity.
• Detailed observing strategy:
3 meas./night, every 3 nights over 8 months
• Periodogram: 3σ detection (red)
E-HIRES, E-MIDIR, E-PCS
2/ 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
Knutson et al. 09
- Chemical Composition
(H20, CH4, CO, CO2, NH3…)
- Atmosphere’s Dynamics
. Inversion,
. Vertical Mixing,
. Circulation,
. Evaporation,
• Imprints of Formation
Mechanisms?
No Thermal Inversion
Thermal inversion
Spitzer
2/ Exoplanets
E-IFU, E-MIDIR, E-PCS
Imaging Planetary Systems
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
Bpic; Lagrange et al. 10
HR8799; Marois et al. 10
2/ Exoplanets
E-IFU, E-MIDIR, E-PCS
Imaging Planetary Systems
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
SPHERE
E-IFU/MIDIR
GAIA
Mesa et al. 11
Kasper et al. 10
Lattanzi & Sozzetti 10
E-PCS
2/ Exoplanets
E-IFU, E-MIDIR, E-PCS
Imaging Planetary Systems
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
Mordasini et al. 12
No Accretion Shock
Formation/Evolution Theories
• L – Mass Relation
• Gas Accretion Phase
Accretion Shock
2/ Exoplanets
E-IFU, E-MIDIR, E-PCS
Imaging Planetary Systems
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
Formation/Evolution Theories
• L – Mass Relation
• Gas Accretion Phase
Planetary System Architecture
• Dynamical stability
• Planet-disk interactions
Bpic b; ESO PR 0842
Stellar Environments
3/ Evolved Stars
Eta Car (HST/WFPC2)
N. Smith/NASA
VLT/NaCo (L’, Bra, Pfg)
Chesneau et al. 08
1’’
3/ Evolved stars
Environments
• Disks, Outflows and Shocks Structure & Physical conditions
(Excitation, kinematics, density , temperature).
• Interacting binary systems: cataclysmic variables and symbiotic systems
Archeology of Planetary systems
> Photospheric abundances of polluted white dwarfs
> Fe, Si, Ca, C , O, Mg abundances
• 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
Conclusions
• Stellar environments under the Microscope
> 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…
• Incredible Machine for Disks, Exoplanets & Evolved stars
> Star/Disk Evolution Processes
> Disk Structure, Composition & Chemistry (Water & Organics)
> Gas/Dust components in planet-forming Regions
> Telluric and Giant Planets Characterization
(frequency, physics, atmosphere & formation)
> Twin Earth in RV & Imaging Super-Earths
> Conditions favorable for Life
E-IFU, E-HIRES & E-MIDIR
1/ Disks
Star – disk interactions
Star/Disk evolution under the microscope…
•
•
•
•
Geometry of Accretion Channels
E-ELT : 10 mas x 0.01 x 100pc
Inner Disk Properties (Warp, asymmetries…)
= 0.01 AU
Role of Magnetic Fields (Config., Reconnection)
= 2 Ro
Jet Launching Zone,
Stellar & Disk Winds
. VLT/CRIRES, CO emission
lines at 4.7µm (< 2 AU)
AS 205 N, Pontopiddan et al. 11