Enrico Pinna INAF - Osservatorio Astrofisico di Arcetri
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Enrico Pinna INAF – Osservatorio Astrofisico di Arcetri
LARGEST OPTICAL TELESCOPES
Credits: ESO
Doubling diameter time = 28yrs
Jump 8m 30m
The key technologies:
• primary segmentation
• adaptive optics
The key technology: active optics
Jump
1989 ESO NTT 3.6m
4m 8m
Subaru 8.2m primary mirror
Credits: ESO/C.Madsen
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
ADAPTIVE OPTICS CONCEPT AND TIMELINE
1953 Babcock: the concept
70s US Military: first real system
1989 first AO astronomical system, COME-ON
1997 NAOS@VLT (185acts)
2000 Keck NGS
2000 Gemini North
2003 MACAO@VLT
Credits: C. Max
2006 NAOS + Na Laser
2007 MAD@VLT (experiment)
2010-12 LBT FLAO 1&2 and LBTI
2012 GEMS @Gemini South
2014 GPI@ Gemini S. (already on the mountain)
2014 SPHERE@VLT (ongoing acceptance test Europe)
2015 AOF@VLT
2020-.... ELTs: adaptive telescopes
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
THE FIRST HIGH CONTRAST AO SYSTEM
Large Binocular Telescope, the new generation of AO
2 AO systems commissioned 2010-2012 H-band H-band
Seeing limited Vs. AO corrected The first high contrast image
Simard
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
THE FIRST HIGH CONTRAST AO SYSTEM
Large Binocular Telescope, the new generation of AO
HR8799 first H-band
detection of 4 planets.
Constrain on the planet
Exo atmoshperic model.
planets
Esposito et al. 2013
Skemer et al. 2012
IR data combined with
radio ones are
Star consistent with outflow
formation and disk structures
Cesaroni al. 2013
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
THE FIRST HIGH CONTRAST AO SYSTEM
Large Binocular Telescope, the new generation of AO
Theta Ori trapezium
Position accuracy 0.5mas
Astrometry Proper motion detectd
0.3mas/yr
Close et al. 2012
LBT no AO J - K FLAO+PISCES J - HST H - FLAO+P. K
Crowded fields (wide field) K
(narrow field)
(narrow field field)
Globular cluster age
can be estimated
considering the
20 arcsec
difference of the
two knees (red)
Bono et al.
in submission ?
HST/WFC3 F110W LBT AO Ks-band
integration = 21 min. Integration = 10 min.
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
HIGH CONTRAST,
23M INTERFEROMETER READY TO GO
HOSTS
Hunt for Observable Signatures of Terrestrial planetary Systems
The first survey to detect faint warm dust from collisions in asteroid
belts around other stars. Detection of the dust would indicate a
planetary system similar to ours, with small rocky bodies.
NASA-supported 60 night survey to be
carried out in the 2013-2016 time frame.
Top level goal is to reduce risk for future
NASA exoplanet imaging missions
LEECH
LBTI Exozodi, Exoplanet Common Hunt
Parallel observations of the same stars during the HOSTS survey at
4 microns wavelength. These observations will be sensitive to
Jupiter-like gas giant planets.
Roberge et al. 2012
0.25s @10.6 µm
Zodiacal dust around other stars can obscure flux from an exo-Earth.
At 10 times our own density (10 zodies) the dust will impact the
Simard performance of exo-Earth imaging missions.
LBTI is designed to probe for zodiacal dust at 10 µm down to 10
zodies. It is unique in being able to accomplish this task
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
MAIN AO SYSTEM TYPES
Natural Guide Star Na Laser Guide Star Multi Conjugated
Single Conjugated Single Conjugated
Requires a bright star I
THE FIRST LASER MCAO SYSTEM
2 deformable mirrors 5 Shack-Hartmann
Wavefront Sensors
Asterims of 5 Na Laser Guide
Stars arrenged on a square
GeMS performance is very uniform over a 85x85 arcsec square field,
both in terms of Strehl ratios and more general PSF characteristics;
Sky coverage of ~55% for all the portion of the sky reachable from
Gemini South
1.5 to 1.7 magnitude sensitivity gain over the 1-2.5 micron range on
point sources with respect to seeing limited imaging.
Simard Gains with respect to HST/NICMOS, in the same conditions, are 0.3 (J)
and 1.2 (K) magnitudes;
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
Credit: Gemini Observatory / AURA
Seeing @550nm
3.9 arcmin
0.6-1.1arcsec
H2 – Fe II – Ks
FWHM 90mas 3.0 arcmin
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013Ideal resolution for knots and filament study
1pix = 7AU
[HST Helix program resolution28AU]
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013Seeing limited @Ks
Antennae Galaxies FWHM = 0.9arcsec
Integration = 19.4min
Brandl et al. 2005
GeMS AO 2012
FWHM = 0.1arcsec
Integration = 8min
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 201313 SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
AO GAIN ON 30M TELESCOPES
sensitivity gain with AO
for ELT is 10 times more than 8m
5s detection limits in 1h of integration @1mm gain of factor 30 (Seeing 0.5’’)
Credits: GMT Science book
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013THE EXTREMELY LARGE TELESCOPES
Giant Magellan Telescope Thirty Meter Telescope European - ELT
www.gmto.org www.tmt.org www.eso.org/public/teles-instr/e-elt
Diameter 24m 30m 39m
Segments 7 X 8.4m 492 X 1.44m 798 x 1.45m
Collecting area 368m2 660m2 1077m2
Diffraction limit @1mm 9mas 7mas 5mas
AO Systems SCAO, LTAO, GLAO SCAO, MCAO SCAO, GLAO, LTAO, MOAO,
(6 Na Lasers) (6 Na LGS) MCAO, XAO (6 Na Lasers)
First Science 2020 4 segments only 2022 2023
(2022 full)
Cost 700 M$ 1000 M$ 1000 M€
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013ELT’S SCIENCE CASES
• Cosmology & fundamental physics
• Early Universe
• Galaxy formation and evolution
• Black holes
• Stellar population and chemical evolution
• Extra solar planetary systems
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013GIANT MAGELLAN TELESCOPE
Adaptive secondary mirror
feeding all the focal stations
7 deformable shells of 1.1m
4700 actuators
SCAO
LTAO
GLAO
High spatial
resolution instruments
Aplanatic Gregorian
No Nasmyth focus
Primary f/0.7
Gregorian focus f/8
Wide field
instruments
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013THE INSTRUMENT SUITE
Instrument / Mode Capabilities λ Range, μm Resolution Field of View
[2019-2021]
Optical High Resolution 7 x 0.7,1.2”
G-CLEF / NS, GLAO 0.35 – 0.95 20 – 100K
Spectrometer / PRV fibers
GMTIFS / LTAO, NGSAO NIR IFU / Imager 0.9 – 2.5 5,000 & 10,000 10 / 400 arcsec2
Wide-Field Optical Multi-Object 1,500 – 4,000
GMACS / NS, GLAO 0.36 – 1.0 40-60 arcmin2
Spectrometer (10K with MANIFEST)
JHKLM High Resolution
GMTNIRS / NGSAO, LTAO 1.2 – 5.0 50K, 100K 1.2” long-slit
Spectrometer
MANIFEST* / NS, GLAO Facility Robotic Fiber Feed 0.36 – 1.0 20’ diameter
Spectral resolution Angular resolution
Credits: G. Jacoby
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013INSTRUMENT SUITE
Classic Ritchey-Chrétien configuration
Postfocal AO system providing:
MCAO
SCAO
LTAO
(GLAO)
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013EUROPEAN ELT
5 mirror optical design
M4: a 2.5 adaptive mirror w/ 4800 actuators
SCAO
GLAO
LTAO
MCAO
MOAO
XAO
Instruments AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
- First Light
E-CAM SCAO, - IMG 0.8 – 2.4 BB, NB 53.0” / 3 mas Astrometry 40mas
– 2023 MCAO - MRS 3000 Coronography
E-IFU SCAO, - IFU 0.5 – 2.4 4000 0.5×1.0” / 4mas Coronography
– 2023 LTAO 10 000 5.0×10.0” / 40mas
20 000
E-MIDIR SCAO, - IMG 3 – 13 BB, NB 18” / 12 mas Coronography
– 2024/2028 LTAO - MRS 3 - 13 5000 Polarimetry
- IFU 3-5 100 000 0.4”×1.5” / 4 mas
1st light E-HIRES SCAO - HRS 0.37 – 0.71 200 000 0.82” Polarimetry
- 2024/2028 0.84 – 2.50 120 000 0.027”×0.5”
E-MOS Slits 0.37 – 1.4 300- 2500 6.8” / 0.1” Multiplex ~ 400
2nd light - 2024/2028 IFUs 0.37 – 1.4 5000 – 30 000 420’ / 0.3” Multiplex ~100
MOAO IFUs 0.8 – 2.45 4000 – 10 000 2” / 40mas Multiplex ~10
Imaging?
E-PCS XAO EPOL 0.6 – 0.9 2.0” / 2.3 mas Coronography
- 2027/2030 IFS 0.95 – 1.65 125 – 20 000 0.8“ / 1.5 mas Polarimetry
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013ELT’S INSTRUMENT SUMMARY
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013DYNAMICS OF HIGH REDSHIFT GALAXIES
ULIRG at z~2
• shocks, winds, interaction with IGM
• dynamical masses
Mergers at z~4 • rotation (kinematics),
• chemical composition (fraction of
• Major or minor mergers? heavy metals)
• Are rotating disks present?
• Accretion of hot or cold gas? Simulated ELT-IFU observation of Ha
Simulated major merger z = 4 (1.4bn yrs)
ELT-IFU + MOAO
Images: HARMONI consortium
(simulations by Tim Goodsall)
75mas/pix 150x150mas 2
Puech et al 2008
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013SUPERMASSIVE BLACK HOLES
E-ELT provides resolution to probe sphere of influence
• 106M BH at Virgo distance • Statistical samples
• 109M BHs to z~0.2 • Understand scatter in MBH-s relation
Test case: simulation of NGC4486 at 16Mpc (Virgo)
Resolution 5mas (E-ELT + LTAO)
Resolution 50mas (SINFONI@VLT) 0.8 ”
3”
Velocity
Image credit: NASA/Dana
Velocity
Berry, SkyWorks Digital
Velocity dispersion
Velocity dispersion
1.25e7 M⊙ BH no BH
1.25e7 M⊙ BH no BH
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013CROWDED FIELDS
Simulated
K-band imaging of a dense star cluster
Natural seeing 0.6’’
HST - NICMOS
JWST NIRCAM
GMT Strehl Ratio 80%
Credit: P. McCarthy
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013CROWDED FIELDS
Central 30arcsec of M32 in the NIR
Gemini AO (2000) JWST TMT AO
Credit: TMT Science Book
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013PROTO PLANETARY DISK
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
Asymmetry Credits: G. Chauvin
Asymmetry and spyral
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013EXO-PLANETS DIRECT IMAGING
Credits: TMT Science Book
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013GIANT EXOPLANET 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 No Thermal Inversion
. Circulation
Thermal inversion
. Evaporation
Spitzer
Knutson et al. 09
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013EXO-EARTH IN THE HZ DETECTION (RV)
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 CODEX on the E-ELT(precision 1 cms−1; right)
CODEX, required to detect Earth-like planets in Habitable Zone of solar-type stars
HARPS (ESO 3.6m) ESPRESSO (VLT) CODEX (E-ELT)
Credits: G. Chauvin
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013SYNERGIES
The «questions»:
• Are there habitable planets around near stars?
• How and when did the first stars begin to shine?
• Can we model the complex physics that is involved in the formation of
stars, galaxies, and supermassive black-holes?
• … and much more
The answer will come from the synergy between:
• Big radio telescope arrays (ALMA, ...)
• Next generation of space telescopes (JWST,...)
• ELTs
• Next generation of ground based survey telescopes (LSST, ...)
• New generation of solar telescopes (EST)
Spectral line sensitivity Angular resolution
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013CONCLUSIONS
• The key technology for the ELTs is Adaptive Optics
• The current forefront AO systems for 8m telescopes are:
• the FLAO system of LBT (INAF) for the high contrast
• GeMS at Gemini South as the first multi conjugated laser
system
• 3 ELTs upcoming in the next decade
• All will implement several AO systems to exploit their huge
apertures in angular resolution and sensitivity
• The ELT’s instruments will span l from 0.35 to 20mm with R
up to 200k to explore from the solar system to the first light
objects
• ELTs will create a strong synergy with new generation of
satellites and radio arrays
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