e- elt’s view of stellar environments
DESCRIPTION
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, - PowerPoint PPT PresentationTRANSCRIPT
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
AO4ELT3 CONFERENCE. FLORENCE, ITALY, 26-31 MAY 2013
OutlineE-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
• 40-m class telescope: largest optical-infrared 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 ProjectThe Telescope
50m2 400m2 600m2 1200m2 (JWST: 25m2)2 µm 50mas 18mas 14mas 10mas (JWST: 68mas)
E-ELT & other competitive projects
Discoveries by opening a new parameter space
• Increased Sensitivity
• Spatial resolution (10 mas scale)
The E-ELT Project
- VLT & VLTI 2nd & 3rd generation PRIMA, K-MOS, SPHERE, MUSE, ESPRESSO, GRAVITY…
2012 2014 2016 2018 2020 2022 2024 2026 2028
- GAIA
- GMT
- Cheops
- JWST- EChO/PLATO/FINESS?
Ground: Harps N/S, SOPHIE, NaCo, VISIR, CRIRES, WASP…
Timeline: current/future missions
- ALMA (ACA)
- E-ELT
- TMT
Space: Spitzer, Herschel, Kepler, CoRoT
- SKA
The E-ELT Project
- TESS
Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• 1st Light Instruments
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• 2nd Pool Instruments
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• XAO Instrument
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• Various AO Flavors
SCAO: single-conjugated AO MCAO: Multi-Conjugated-AO LTAO: Laser-Tomographic AO
MOAO: Multi-Object AO XAO: Extreme-AO
Instruments- First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO,MCAO
- IMG- MRS
0.8 – 2.4 BB, NB3000
53.0” / 3 mas Astrometry 40masCoronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 400010 00020 000
0.5×1.0” / 4mas5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG- MRS- IFU
3 – 133 - 133 - 5
BB, NB5000100 000
18” / 12 mas
0.4”×1.5” / 4 mas
CoronographyPolarimetry
E-HIRES- 2024/2028
SCAO - HRS 0.37 – 0.710.84 – 2.50
200 000120 000
0.82”0.027”×0.5”
Polarimetry
E-MOS- 2024/2028
MOAO
SlitsIFUsIFUs
0.37 – 1.40.37 – 1.40.8 – 2.45
300- 25005000 – 30 0004000 – 10 000
6.8” / 0.1”420’ / 0.3”2” / 40mas
Multiplex ~ 400Multiplex ~100Multiplex ~10Imaging?
E-PCS- 2027/2030
XAO EPOLIFS
0.6 – 0.90.95 – 1.65 125 – 20 000
2.0” / 2.3 mas0.8“ / 1.5 mas
CoronographyPolarimetry
Instrument RoadmapThe E-ELT Project
• Science Priority / Stellar Environments
Low Medium High
OutlineE-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 Environments1/ Circumstellar Disks
Artist’s View ESO-PR-0942
1/ DisksKey Scientific Questions
. Star/disk Evolutiono Accretion, photo-evaporation, o Jets & Windso Magnetic Fields
. Disk Structure & Dynamics (Gas & Dust)
. Chemistry: Water & Organics
in Planet-Forming Zones
. Planetary Formationo Initial conditions
. Planets/Disk interactions Fomalhaut ALMA/HSTBowler et al. 12
Probing Planet-forming Regions
snow line
E-MIDIR VLT/CRIRESE-IFU, E-HIRES
1/ Disks
ALMA
1 Lsun
@100 pc
Distance 0.01 0.1 1.0 10.0 100.0 [AU] Temperature 3000 1000 300 100 30 [K] Time 0.4 days 2 weeks 1 yr 30 yr 1000 yr
E-ELT : 10 mas x 100pc = 1 AU
Co-rotation radiusMagnetospheric radius
dust sublimation
crystallization
snow line
E-MIDIR VLT/CRIRESE-IFU, E-HIRES
1/ Disks
ALMA
1 Lsun
@100 pc
Distance 0.01 0.1 1.0 10.0 100.0 [AU] Temperature 3000 1000 300 100 30 [K] Time 0.4 days 2 weeks 1 yr 30 yr 1000 yr
Spectro-astrometry
Star – disk interactions
E-ELT : 10 mas x 0.01 x 100pc = 0.01 AU
Zanni & Ferreira 09
E-IF
U, E
-HIR
ES &
E-M
IDIR
Star – disk interactions
MHD star – disk simulations
R/Ro
1/ Disks
E-ELT : 10 mas x 0.01 x 100pc = 0.01 AU = 2 Ro
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
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-addedo Right: Velocity map with a resolving power of 100 000 (3 km/s)
32 AU
Gas Dynamics in planet-forming zones
E-M
IDIR
1/ Disks
Water & Organics• Distribution and Dynamics • Disk cooling & Planetesimals formation• Organic/Prebiotic chemistry (CH4, C2H2, HCN…)• Isotopic Fractionation• Transfer to Terrestrial Planets
E-M
IDIR . 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/ DisksGas Dynamics in planet-forming zones
Asymmetries/Spirals in proto-planetary disks
• 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
Observing the Dusty Disk Structures1/ Disks
E-M
IDIR
1/ DisksE-
MID
IR
Asymmetries/Spirals in proto-planetary disks
• 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
Observing the Dusty Disk Structures
1/ DisksE-
MID
IR
Asymmetries/Spirals in proto-planetary disks
• 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
Observing the Dusty Disk Structures
E-M
IDIR
1/ DisksAsymmetries/Spirals in proto-planetary disks
• 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
Observing the Dusty Disk Structures
Stellar Environments2/ Exoplanets
Artist’s View ESO-PR-1106
2/ ExoplanetsKey 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?
Expected planet population detected by Doppler spectroscopy with:o HARPS on the ESO 3.6-metre (precision 1 ms−1),
2/ ExoplanetsExploration of Telluric Planets
observed
corrected
Predicted (Mordasini et al. 09)Observed (Mayor et al. 11)
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
2/ ExoplanetsE-
HIRE
S
Exploration of Telluric Planets
• 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)
2/ ExoplanetsTwin Earth Discovery
E-HI
RES
2/ ExoplanetsE-
HIRE
S, E
-MID
IR, 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?
Knutson et al. 09
Spitzer
No Thermal InversionThermal inversion
E-IF
U, E
-M
IDIR
, E-
PCS
2/ ExoplanetsImaging Planetary Systems
HR8799; Marois et al. 10Bpic; Lagrange et al. 10
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-PCS
GAIA
Mesa et al. 11Kasper et al. 10Lattanzi & Sozzetti 10
E-IFU/MIDIR
E-IF
U, E
-M
IDIR
, E-
PCS
2/ ExoplanetsImaging 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
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
E-IF
U, E
-M
IDIR
, E-
PCS
2/ ExoplanetsImaging Planetary Systems
Accretion Shock
No Accretion Shock
Mordasini et al. 12
E-IF
U, E
-M
IDIR
, E-
PCS
2/ ExoplanetsImaging 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 Environments3/ Evolved Stars
Eta Car (HST/WFPC2)
VLT/NaCo (L’, Bra, Pfg)
N. Smith/NASA
Chesneau et al. 08
1’’
3/ Evolved starsEnvironments• 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-IF
U, E
-HIR
ES &
E-M
IDIR
. VLT/CRIRES, CO emission lines at 4.7µm (< 2 AU)
AS 205 N, Pontopiddan et al. 11
1/ DisksStar – disk interactions
E-ELT : 10 mas x 0.01 x 100pc = 0.01 AU = 2 Ro
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