Science Case
Science Case
Science Case
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European Extremely Large Telescope<br />
<strong>Science</strong> <strong>Case</strong><br />
Markus Kissler-Patig<br />
E-ELT Project Scientist<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
GMT<br />
TMT<br />
E-ELT
E-ELT Overview
• A project lead by ESO on behalf of 14 member states<br />
• Segmented mirror, adaptive telescope of 42m<br />
diameter with a 5 mirror design<br />
• Schedule:<br />
• Detail design phase until mid-2010<br />
• Start of construction by end of 2010<br />
• End of construction 2017<br />
The E-ELT in a Nutshell<br />
• Cost (Telescope + Instruments): ~1 billion Euros
The E-ELT Dome
BRD v1<br />
The E-ELT Structure<br />
Azimuth track Altitude cradle<br />
Two industrial studies: cost & schedule check<br />
BRD v2<br />
Baseline for updating requirements
$<br />
N?G7J8$:$$$.A6OD>I$$6=;>%L?AGJAO6$;K$@7JH8L$J8IB$/A>?;$A6$A$?;K$;8L$ED$L?;G$<br />
$<br />
.183 MM<br />
The BRD v2 Optical Design<br />
G<br />
49390$ #=>?@AB$C7AB?>D$<br />
M4 (AO): 2.6m<br />
G<br />
G<br />
!%!&'$#(')*+&$,!")-.$/!(#/'$<br />
M1 (seg): 42m<br />
M2: 5.7m<br />
M3: 4m<br />
G<br />
$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$>P;2$<br />
$ 19<br />
>?@7A8$4$*
The E-ELT Emphasis<br />
• Active optics to phase up the large mirror surfaces<br />
• Adaptive optics is being designed into the telescope<br />
and first-generation instruments<br />
to give maximum gains in resolution and sensitivity<br />
priority for diffraction-limited instruments
Adaptive Optics<br />
• The Telescope delivers:<br />
• seeing limited mode<br />
• Ground Layer AO (w/ and w/o LGS) [GLAO]<br />
• Post-Focal AO facilities:<br />
• Single Conjugated AO (no LGS) [SCAO]<br />
• Laser Tomography AO [LTAO]<br />
• Multi-conjugated AO [MCAO]<br />
• AO included in instruments:<br />
• Extreme AO [XAO]<br />
• Single Conjugated AO [SCAO]
Laser Guide Stars<br />
Baseline:<br />
•Six Continuous Wave lasers of 50 W (TBC) each at 589 nm<br />
•Gravity invariant laser clean room(s)<br />
•Launch from behind secondary mirror<br />
•Mirror relay to launch telescope<br />
•Rotate laser with the field (not with the pupil)<br />
LLT<br />
Sodium<br />
layer<br />
~5” elongation
Instrument Suite
E-ELT Instrumentation: Background<br />
E-ELT Proposal to ESO Council (Dec 2006)<br />
• High Priority Instruments<br />
• Policy of studies and instrument procurement<br />
• “5-6 first generation instruments” at an estimated hardware<br />
construction cost to ESO of 86 M€<br />
Instrument and AO modules Study Plan (April 2007)<br />
• Plan presented and discussed with STC foresees:<br />
8 instruments and 2 post-focal AO module preparatory<br />
studies<br />
• 2.3 M€ Study Budget 2007-2009 (now 90% committed) +<br />
30 ESO FTE for Study Phase<br />
• For the most demanding instruments and AO modules<br />
additional funding provided by EC Framework programs
Foreseen first generation of instruments<br />
Name Instrument type<br />
Wavelength<br />
range<br />
MICADO Diffraction limited NIR Imager 0.8-2.4 μm<br />
HARMONI Single-field NIR spectrograph 0.8-2.4 μm<br />
EAGLE<br />
CODEX<br />
Wide-field multi-object NIR<br />
spectrograph<br />
High-resolution visual<br />
spectrograph<br />
0.8-2.4 μm<br />
0.35-0.72<br />
μm<br />
METIS Mid-IR imager and spectrograph 3.5-20 μm<br />
FoV and<br />
sampling<br />
30”<br />
4 mas/pix<br />
~1”-10”<br />
20-50 mas/pix<br />
patrol field ≥5'<br />
10-50 mas/pix<br />
Spectral<br />
resolution<br />
~4000<br />
(~20.000)<br />
~5000<br />
(R>15.000)<br />
AO support<br />
envisaged<br />
SCAO/MCAO<br />
SCAO/LTAO<br />
point source >120.000 Tip-Tilt?<br />
30”<br />
15-30 mas/pix<br />
5-200<br />
~100.000<br />
Notes<br />
MOAO multiplex >20<br />
SCAO/LTAO<br />
stability < 2 cm/s<br />
over 30 years<br />
EPICS Planet finder 0.6-1.8 μm ~2”-4” >50 XAO Polarimetry<br />
?? Optical MOS 0.3-1.8 μm 5’-10’ FoV 1000-10.000 GLAO multiplex >100<br />
?? NIR high-resolution spectrograph 0.8-2.4 μm slit >100.000 GLAO<br />
MAORY Multi-conjugated AO module 0.6-2.4 μm 2’ FoV<br />
2 DMs + M4,<br />
6 LGS<br />
?? Laser tomography AO module 0.6-2.4 μm 1’ FoV M4, 6 LGS
Markus Kissler-Patig E-ELT Status GSMT Workshop, Chicago, 16 June 2008 15
Markus Kissler-Patig E-ELT Status GSMT Workshop, Chicago, 16 June 2008 15
Markus Kissler-Patig E-ELT Status GSMT Workshop, Chicago, 16 June 2008 16
TEST INSTRUMENT DISTRIBUTION (NASMYTH PLATFORMS)<br />
MCAO & LTAO modules, MICADO, HARMONI, EPICS, METIS , one WF INSTRUMENT<br />
Test<br />
Camera<br />
WIDE FIELD<br />
INSTRUMENT<br />
MICADO<br />
MCAO module<br />
P<br />
M6<br />
units,<br />
Adaptors<br />
P<br />
HARMONI<br />
LTAO<br />
modules<br />
METIS<br />
EPICS+<br />
XAO
EAGLE<br />
+MOAO<br />
TEST INSTRUMENT DISTRIBUTION (GI and COUDE foci)<br />
CODEX
PRELIMINARY<br />
NIRSpec<br />
E-ELT Instrumentation Project Office<br />
WAVELENGTH vs. SPECTRAL RESOLUTION<br />
Wavelength (nm)<br />
MET<br />
IS
PRELIMINARY<br />
JWST MIRI<br />
Strehl<br />
0 0.5 1<br />
E-ELT Instrumentation Project Office<br />
PIXEL SAMPLING vs.STREHL for diffraction limited E-ELT INSTRUMENTS<br />
Pixel size<br />
0.90(N)<br />
0.72 (K)<br />
JWST NIRCam<br />
0.5 (K)<br />
30” field<br />
20
PRELIMINARY<br />
WF, visual-red camera or<br />
spectrograph with GLAO<br />
E-ELT Instrumentation Project Office<br />
PIXEL SAMPLING, EE within 2x2 spaxels of Wide Field E-ELT INSTRUMENTS<br />
EE<br />
0 100<br />
Pixel size (mas)<br />
EE 30% at I<br />
5’<br />
EAGLE, NIR<br />
MIFU with<br />
MOAO
<strong>Science</strong> <strong>Case</strong>
The <strong>Science</strong> <strong>Case</strong> for Giant Telescope builds on three pillars:<br />
Discovery / the unknown<br />
Synergy with large facilities (VLT/I, JWST, ALMA, LSST, SKA, ...)<br />
Contemporary <strong>Science</strong><br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
The Unknown<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Enabling discovery by opening parameter space<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Synergy with Large Facilities<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
The main synergy is expected with:<br />
The 8-10m class Telescopes (VLT/I, ...)<br />
The JWST<br />
ALMA<br />
LSST<br />
SKA / SKA Pathfinders<br />
...<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
JWST key science<br />
The End of the Dark Ages: First Light and Reionization<br />
Assembly of Galaxies<br />
➱ suite of optical/NIR sensitive multi-object spectrographs<br />
The Birth of Stars and Protoplanetary Systems<br />
Planetary Systems and the Origins of Life<br />
➱ METIS: mid-IR instrument (high spatial/spectral resolution at<br />
3-15 μm)<br />
➱ EPICS: planet-finder (incl. low-resolution spectroscopy and<br />
polarimetry)<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
ALMA key science<br />
Detect spectral line emission from CO or CII in a normal<br />
galaxy like the Milky Way at a redshift of z = 3, in less than 24<br />
hours of observation.<br />
➱ NIR sensitive integral spectrograph and imager<br />
Image the gas kinematics in protostars and in protoplanetary<br />
disks around young Sun-like stars at a distance of the nearest<br />
star-forming clouds.<br />
➱ NIR and mid-IR high-spectral resolution instruments<br />
Provide precise images at an angular resolution of 0.1 arcsec.<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Contemporary <strong>Science</strong><br />
The Design Reference Mission<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Planets & Stars<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Planets & Stars<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Planets & Stars<br />
Stars & Galaxies<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Planets & Stars<br />
Stars & Galaxies<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Planets & Stars<br />
Stars & Galaxies<br />
Galaxies & Cosmology<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Planets & Stars<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
From giant to terrestrial exo-planets:<br />
detection, characterisation and evolution<br />
Circumstellar disks<br />
Young clusters and the Initial Mass Function<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
From giant to terrestrial exo-planets:<br />
detection, characterisation and evolution<br />
Circumstellar disks<br />
Young clusters and the Initial Mass Function<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Today, we can detect Jupiter-mass planets indirectly.<br />
What the ELT would allow us to do:<br />
1- detect Earth-mass planets indirectly<br />
2- perform direct imaging of planets<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
To date: 270 extra-solar planets<br />
have been detected
Derived key requirements:<br />
• measure radial velocities with
From giant to terrestrial exo-planets:<br />
detection, characterisation and evolution<br />
Circumstellar disks<br />
Young clusters and the Initial Mass Function<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Evolution of planetary systems in Orion<br />
Transition from disks to planetary systems<br />
McCaughrean, Stapelfeldt, & Close PPIV, 2000<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
McCaughrean
Circumstellar disks are the birthplaces of planets<br />
How is material assembled?<br />
And on which time scales?<br />
The ELT will allow us to study the morphology, dynamics<br />
and chemistry of the young disks.<br />
The ELT has ~10 the spatial resolution of the JWST in<br />
the mid-infrared<br />
Artist’s representation of a protoplanetary disk<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
Hartmann
Derived key requirements:<br />
• diffraction limited imaging at 2-10 μm wavelength<br />
‣ efficient telescope and AO in the mid-infrared<br />
• diffraction limited spectroscopy at 2-20 μm wavelength<br />
‣ telescope transmitting all the way to 20 μm<br />
‣ spectrograph with high resolution (100.000) at 5 μm<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
From giant to terrestrial exo-planets:<br />
detection, characterisation and evolution<br />
Circumstellar disks<br />
Young clusters and the Initial Mass Function<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
How do molecular clouds fragment?<br />
What is the mass spectrum of stars?<br />
(Extension of ALMA science) !<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
-<br />
0<br />
8
Derived key requirements:<br />
• “wide field” diffraction limited imaging at 2 μm wavelength<br />
‣ Multi-Conjugate AO over >30” FoV in the near<br />
infrared<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Stars & Galaxies<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Imaging and spectroscopy of resolved stellar<br />
populations in galaxies<br />
Black holes and AGN<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Imaging and spectroscopy of resolved stellar<br />
populations in galaxies<br />
Black holes and AGN<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Understanding the formation and evolution of galaxies<br />
The goals with the ELT are:<br />
Leo A<br />
Deepest ever CMD (in<br />
absolute mag) for an<br />
isolated dwarf irregular.<br />
M814 ! +3.4<br />
M475 ! +4.2<br />
1- to obtain ultra-deep photometry of stars in nearby galaxies<br />
2- to understand the very first stars formed in our galaxy<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
Cole et al. 2007<br />
Leo A: Deepest colourmagnitude<br />
diagram ever<br />
obtained for a galaxy
Derived key requirements:<br />
• “wide field” diffraction limited imaging down to visible<br />
wavelength<br />
‣ Multi-Conjugate AO over >60” FoV down to 0.6 μm<br />
• high-resolution spectrograph in the UV<br />
‣ telescope efficient down to the atmospheric cut-off<br />
(340 nm)<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Imaging and spectroscopy of resolved stellar<br />
populations in galaxies<br />
Black holes and AGN (Active Galactic Nuclei)<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Probing closer to black holes:<br />
Is the black hole intimately connected with the<br />
evolution of the galaxy?<br />
With a combination of high spatial and spectral resolution, the<br />
ELT will be able to probe black hole over a large range of masses<br />
in all types of galaxies<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
M87 hosts a 10 9 Mo black hole
Derived key requirements:<br />
• high spatial and spectral resolution spectroscopy<br />
‣ spectroscopy with resolution 5.000 to 10.000 at the<br />
diffraction limit in the near-infrared<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Galaxies & Cosmology<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
The physics of high-redshift galaxies<br />
First light - the highest redshift galaxies<br />
Is the low-density intergalactic medium<br />
metal enriched?<br />
A dynamical measurement of the expansion<br />
history of the universe<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
The physics of high-redshift galaxies<br />
First light - the highest redshift galaxies<br />
Is the low-density intergalactic medium<br />
metal enriched?<br />
A dynamical measurement of the expansion<br />
history of the universe<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
What did galaxies look like 10 billion years ago?<br />
The ELT will allow to measure the kinematics (masses/structure)<br />
of galaxies in the very early universe (redshifts between 2 and 6)<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
V σ<br />
z ~ 4 50 mas pixels<br />
z=0 rotating disk simulations (M. Puech)<br />
42-m, 10-hr integration, MOAO (MCAO)
Derived key requirements:<br />
• spectroscopy at high spatial resolution for multiple sources<br />
in a large field<br />
‣ field of view of 5’ to 10’<br />
‣ FoV corrected locally with Mutli-Object AO<br />
‣ gravity invariant focus<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
The physics of high-redshift galaxies<br />
First light - the highest redshift galaxies<br />
Is the low-density intergalactic medium<br />
metal enriched?<br />
A dynamical measurement of the expansion<br />
history of the universe<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Scanning the Inter-Galactic Medium back in time with Quasars:<br />
Where are the metals formed by the galaxies?<br />
To Earth<br />
The ELT with its large collecting area allows to probe the faintest<br />
lines in the IGM at high redshift<br />
QSO absorption lines<br />
Lyman limit Ly"<br />
Ly!<br />
Ly" em<br />
Ly! forest<br />
Quasar<br />
Ly! em<br />
SiII<br />
CII<br />
NV em<br />
SiIV<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong><br />
SiIV em<br />
SiII CIV<br />
CIV em
Derived key requirements:<br />
• high spectral resolution spectrograph in the blue/UV<br />
‣ spectroscopy with resolution 50.000+ down to 380 nm<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
The physics of high-redshift galaxies<br />
First light - the highest redshift galaxies<br />
Is the low-density intergalactic medium<br />
metal enriched?<br />
A dynamical measurement of the expansion<br />
history of the universe<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
For the very first time, a direct measurement of the dynamical<br />
evolution of the universe is possible.<br />
The experiment requires 4000h of observations over 20 years.<br />
The systematic errors must be kept below 1cm/s spectral<br />
resolution.<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Derived key requirements:<br />
• lifetime of the telescope > 20 years<br />
‣ reproducibility of the wavelength calibration over that<br />
time<br />
• Ultra-high resolution (i.e. stable) spectrograph<br />
‣ Coudé focus for the spectrograph<br />
Markus Kissler-Patig - ELT <strong>Science</strong> <strong>Case</strong>
Thank You