pyramid 4 epics? · 2013-10-10 · instrument / mode capabilities λ range, μm resolution field of...

Enrico Pinna

INAF – Osservatorio Astrofisico di Arcetri

SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013

2

LARGEST OPTICAL TELESCOPES

Cre

dits: E

SO

Doubling diameter time = 28yrs

The key technology: active optics

1989 ESO NTT 3.6m

Cre

dits: E

SO

/C.M

adse

n Subaru 8.2m primary mirror

Jump

4m 8m

The key technologies:

• primary segmentation

• adaptive optics

Jump 8m 30m


3

ADAPTIVE OPTICS CONCEPT AND TIMELINE

Credits: C. Max

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

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


4

Simard

H-band

Seeing limited Vs. AO corrected

H-band

The first high contrast image

2 AO systems commissioned 2010-2012

THE FIRST HIGH CONTRAST AO SYSTEM Large Binocular Telescope, the new generation of AO


5

Exo

planets

HR8799 first H-band

detection of 4 planets.

Constrain on the planet

atmoshperic model.

Esposito et al. 2013

Skemer et al. 2012

IR data combined with

radio ones are

consistent with outflow

and disk structures

Cesaroni al. 2013

Star

formation



6

Position accuracy 0.5mas

Proper motion detectd

0.3mas/yr

Close et al. 2012

Globular cluster age

can be estimated

considering the

difference of the

two knees (red)

Bono et al.

in submission

Theta Ori trapezium

20

arc

sec

HST/WFC3 F110W

integration = 21 min. LBT AO Ks-band

Integration = 10 min.

LBT no AO J - K

(wide field) FLAO+PISCES J -

K

(narrow field)

HST H - FLAO+P. K

(narrow field field)

?

Astrometry

Crowded fields



7

HIGH CONTRAST,

23M INTERFEROMETER READY TO GO

Simard

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.

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.

Ro

be

rge

et a

l. 2

01

2

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

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

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

0.25s @10.6 µm


8

MAIN AO SYSTEM TYPES

Natural Guide Star

Single Conjugated

Requires a bright star I<15 @20’’

Scientific field d ~ 40’’ diameter in K

Na Laser Guide Star

Single Conjugated

Requires a faint star I<17 @1’

Scientific field d ~ 40’’ diameter in K

Multi Conjugated

Requires multiple faint star I<17 @1’

Scientific field d ~ 1.5’ diameter in K

... and many more


9

Simard

THE FIRST LASER MCAO SYSTEM

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.

Gains with respect to HST/NICMOS, in the same conditions, are 0.3 (J)

and 1.2 (K) magnitudes;

Asterims of 5 Na Laser Guide

Stars arrenged on a square

2 deformable mirrors 5 Shack-Hartmann

Wavefront Sensors


10

3.0 arcmin

3.9

arc

min

Seeing @550nm

0.6-1.1arcsec

H2 – Fe II – Ks

FWHM 90mas

Cre

dit: G

em

ini O

bse

rvato

ry / A

UR

A


Ideal resolution for knots and filament study

1pix = 7AU

[HST Helix program resolution28AU]

11


12

Seeing limited @Ks

FWHM = 0.9arcsec

Integration = 19.4min

Brandl et al. 2005

Antennae Galaxies

GeMS AO 2012

FWHM = 0.1arcsec

Integration = 8min


13


14

sensitivity gain with AO

for ELT is 10 times more than 8m

Cre

dits: G

MT

Scie

nce

bo

ok

AO GAIN ON 30M TELESCOPES

5s detection limits in 1h of integration @1mm gain of factor 30 (Seeing 0.5’’)


15

Giant Magellan Telescope www.gmto.org

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

(6 Na Lasers)

SCAO, MCAO

(6 Na LGS)

SCAO, GLAO, LTAO, MOAO,

MCAO, XAO (6 Na Lasers)

First Science 2020 4 segments only

(2022 full)

2022 2023

Cost 700 M$ 1000 M$

1000 M€

Thirty Meter Telescope www.tmt.org

European - ELT www.eso.org/public/teles-instr/e-elt

THE EXTREMELY LARGE TELESCOPES


16

ELT’S SCIENCE CASES

• Cosmology & fundamental physics

• Early Universe

• Galaxy formation and evolution

• Black holes

• Stellar population and chemical evolution

• Extra solar planetary systems


17

GIANT 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

Wide field

instruments

Aplanatic Gregorian

No Nasmyth focus

Primary f/0.7

Gregorian focus f/8


Instrument / Mode Capabilities λ Range, μm Resolution Field of View

G-CLEF / NS, GLAO Optical High Resolution

Spectrometer / PRV 0.35 – 0.95 20 – 100K

7 x 0.7,1.2”

fibers

GMTIFS / LTAO, NGSAO NIR IFU / Imager 0.9 – 2.5 5,000 & 10,000 10 / 400 arcsec2

GMACS / NS, GLAO Wide-Field Optical Multi-Object

Spectrometer 0.36 – 1.0

1,500 – 4,000

(10K with MANIFEST) 40-60 arcmin2

GMTNIRS / NGSAO, LTAO JHKLM High Resolution

Spectrometer 1.2 – 5.0 50K, 100K 1.2” long-slit

MANIFEST* / NS, GLAO Facility Robotic Fiber Feed 0.36 – 1.0 20’ diameter

18

THE INSTRUMENT SUITE

Cre

dits: G

. Ja

co

by

[20

19-2

02

1]

Spectral resolution Angular resolution


19

INSTRUMENT SUITE

Classic Ritchey-Chrétien configuration

Postfocal AO system providing:

MCAO

SCAO

LTAO

(GLAO)


20

EUROPEAN ELT

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 0.4”×1.5” / 4 mas

Coronography Polarimetry

E-HIRES - 2024/2028

SCAO

- HRS

0.37 – 0.71 0.84 – 2.50

200 000 120 000

0.82” 0.027”×0.5”

Polarimetry

E-MOS - 2024/2028

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?

E-PCS - 2027/2030

XAO 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

1st light

2nd light

SCAO

GLAO

LTAO

MCAO

MOAO

XAO

5 mirror optical design

M4: a 2.5 adaptive mirror w/ 4800 actuators


21

ELT’S INSTRUMENT SUMMARY


22

DYNAMICS OF HIGH REDSHIFT GALAXIES

Simulated ELT-IFU observation of Ha

Ima

ge

s: H

AR

MO

NI co

nso

rtiu

m

(sim

ula

tio

ns b

y T

im G

oo

dsa

ll)

• shocks, winds, interaction with IGM

• dynamical masses

• rotation (kinematics),

• chemical composition (fraction of

heavy metals) • Major or minor mergers?

• Are rotating disks present?

• Accretion of hot or cold gas?

ULIRG at z~2

Mergers at z~4

Puech et al 2008

Simulated major merger z = 4 (1.4bn yrs)

ELT-IFU + MOAO

75mas/pix 150x150mas2


E-ELT provides resolution to probe sphere of influence

• 106M BH at Virgo distance

• 109M BHs to z~0.2

Image credit: NASA/Dana

Berry, SkyWorks Digital

SUPERMASSIVE BLACK HOLES

Ve

locity d

ispe

rsio

n

Ve

locity

1.25e7 M⊙ BH no BH

3 ”

Resolution 50mas (SINFONI@VLT) 0.8 ”

1.25e7 M⊙ BH no BH

Ve

locity d

isp

ers

ion

V

elo

city

• Statistical samples

• Understand scatter in MBH-s relation

Resolution 5mas (E-ELT + LTAO)

Test case: simulation of NGC4486 at 16Mpc (Virgo)

23


24

Natural seeing 0.6’’

Simulated

K-band imaging of a dense star cluster

HST - NICMOS

JWST NIRCAM

GMT Strehl Ratio 80%

CROWDED FIELDS

Credit: P. McCarthy


25

CROWDED FIELDS

Central 30arcsec of M32 in the NIR

Gemini AO (2000) JWST TMT AO

Credit: TMT Science Book


26

PROTO 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

Credits: G. Chauvin

Asymmetry Asymmetry

and spyral


27

EXO-PLANETS DIRECT IMAGING

Credits: TMT Science Book


28

GIANT 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

. Circulation

. Evaporation

Knutson et al. 09

Spitzer

No Thermal Inversion Thermal inversion


29

EXO-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

Credits: G. Chauvin

HARPS (ESO 3.6m) ESPRESSO (VLT) CODEX (E-ELT)


30

SYNERGIES 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


31

• 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

CONCLUSIONS

pyramid 4 epics? · 2013-10-10 · instrument / mode capabilities λ range, μm resolution field of...

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