The E-ELT Instrumentation Roadmap

The E-ELT Instrumentation Roadmap 

Presentation to the Project Science Team 

Suzanne Ramsay 

Mark Casali, Norbert Hubin, Hans Ulrich Käufl, 

Jean-Louis Lizon, Josef Strasser, 

Juan Carlos Gonzalez

The instrument studies 

• The goal of the study programme was to carry-out 

a suitable number of instrument studies 

‣ to work with the ESO community towards construction 

‣ to verify that instruments can be built at an affordable 

cost and that they properly address the highest priority 

scientific goals, 

‣ to work with telescope and operation groups to identify 

and define interfaces with the other subsystems and 

the observatory infrastructure. 

• 9 instrument and 2 post-focal AO studies carried 

out by >300 scientists and engineers in 40 

institutes throughout the ESO community 

E-ELT Instrumentation Roadmap | PST 11.07.2012

OVERVIEW OF THE E-ELT INSTRUMENT 

STUDIES

Selection process: 

criteria 

ESO/COU 1275, December 2009 

Nr. 

Evaluation Criteria for E-ELT instrument selection 

1 Scientific Merit : 

(a) the instrument addresses science goals identified as of highest priority for the E-ELT 

(b) the instrument can be conceived as an E-ELT workhorse to be used for a variety of 

programmes, leading to a broad spectrum of potential discoveries 

(c) the instrument will benefit and complement observations of other major facilities in 

astrophysics like ALMA and the JWST , which will be already in operation at the time of first 

light 

2 Proven Technical Feasibility and Simulated Performance: the instrument feasibility and its 

expected performance have been properly demonstrated in the study 

3 Affordability: (a) the instrument cost is well estimated and justified (b) the cost to ESO falls within 

or close to the preliminary budget envelope. 

4 Timely Match to the telescope + PFAO performance: the instrument schedule of implementation is 

well matched to the path of the telescope +AO to full performance. The instrument includes the 

possibility to do prime science even during the time when the telescope cannot operate with AO.


scientific priority 

• Science based prioritisation 

‣ All instruments candidates for selection at first light with 

the exception of the planet camera and spectrograph, 

EPICS (highest scientific priority but long technology 

development) 

• Science Working Group Criteria for selection of first 

light instruments 

‣ Scientific impact, including certainty of scientific return 

‣ Complementarity with other facilities 

‣ Scientific Flexibility 

‣ Coverage of expected observing conditions 



the first light pair 

• First light instruments 

‣ ELT-CAM: NIR diffraction-limited camera with moderate 

field size 

‣ ELT-IFU: NIR IFU spectrograph with optical-IR coverage 

and seeing limited to diffraction limited capabilities 

‣ Adaptive optics systems as required to meet the science 

cases of each instrument 


• Primary Imaging Field 

‣ 53” across, 3mas pix 

‣ 4x4 HAWAII 4RG det 

‣ ~20 filter slots 

‣ High throughput 

• Auxiliary Arm 

MICADO: 

Diffraction-limited NIR Camera 

‣ Imager: 1.5mas & 4mas pixels 

‣ Spectrograph: R=3000 

‣ 1 HAWAII 4RG detector 

• AO System – MCAO/MAORY 

PI: Reinhard Genzel (Ric Davies) 

MPE, MPIA, USM, INAF-OAPD, 

NOVA , LESIA 


MAORY : 

Multi-conjugate adaptive optics relay 

• Multi-conjugate AO 

‣ 6 laser and 3 natural guide stars 

‣ Deformable mirrors conjugated to atmospheric 

layers at 4km, 12.7km 

‣ Very high quality images (S.R. >50% in K) over a 

wide field - 2‟, 

‣ Central 1‟ clear 

‣ Two output ports 

PI: Emiliano Diolaiti 

INAF (Bologna, Padova, Arcetri, 

IASF-Bologna), Univ.Bologna, 

ONERA 

MICADO mounted under MAOR 


HARMONI 

Single field, wide band IFU, NIR spectrometer 

• Wavelength range 0.47-2.45µm 

• Spectral resolving power 

‣ R ≈ 4000, 10000, 20000 

• 4 spatial scales 

‣ 4mas, 10mas, 20mas, 40mas 

• 4 fields of view 

‣ 0.5'' x 1.0'' , 1.25'' x 2.5'' 

2.5'' x 5'„, 5'' x 10'„ 

• LTAO/ATLAS 

PI: Niranjan Thatte, 

Oxford, CRAL, CSIC, IAC,UK 

ATC, ONERA 


ATLAS: 

Advanced Tomographic Laser AO 

• Adaptive optics using laser guide stars 

‣ Uses the telescope adaptive mirrors, simple design 

‣ No additional mirrors in the instrument optical path 

‣ Very high quality images (S.R. >50% in K) over ~30‟‟ field 

‣ Fixed asterism of six laser guide stars, 2 NGS 

‣ Excellent sky coverage 

PI: Thierry Fusco 

ONERA,GEPI, LESIA, UK 

ATC, LAM 



planetary camera/spectrograph 


‣ ELT-CAM: NIR diffraction-limited camera 





• A planetary camera/spectrograph with Extreme AO 

(>90% Strehl) has high scientific priority and must 

be built once the technology is developed 


ELT-PCS/EPICS 

exo-planet imaging camera spectrograph 

Integral Field Spectrograph 0.95-1.65μm 

FOV: 0.8'' x 0.8'„/2.33mas 

0.8'' x 0.014'„ long slit 

R = 125, 1400 and 20000 

EPOL 0.6-0.9μm 

Coronagraphic polarimeter 

FOV: 2'' x 2'‘/1.5mas 

Contrast ratios – 10 -8 – 10 -9 

XAO – very high (90%) Strehl 

PI: Markus Kasper, ESO 

LAOG,LESIA, Uni. Nice, 

LAM,ONERA, Uni.Oxford, INAF, 

ETH Zurich, NOVA 

E-ELT Instrumentation Roadmap | PST 11.07.2012 

12


a pool of capabilities 


‣ ELT-CAM: NIR diffraction-limited camera 





• A planetary camera/spectrograph with Extreme AO 

has high scientific priority 

• Instruments thereafter of equal scientific priority 

‣ A pool of scientific capabilities : MIR imaging and 

spectroscopy, VIS-NIR multi-object spectroscopy, VIS- 

NIR high resolving power spectroscopy 


E-ELT Instrumentation 

Roadmap 

• ELT-IFU and ELT-CAM for first light 

(SWG/STC/ESO) 

• ELT-MIR, MOS, HIRES scientifically equivalent 

priorities (SWG/STC/ESO) 

‣ Selection by other considerations (project readiness) 

• Practical requirements 

‣ Staggered project schedule for funding profile 

‣ Staggered commissioning schedule 

• Start enabling technology development, especially 

for high-priority instruments e.g. ELT-PCS 

‣ Begin project when feasibility (TRL) is demonstrated 


Roadmap Considerations 

• ELT-3 to help cover poor IQ conditions (SWG/STC) 

• MOS/HIRES scientific requirements to be developed 

to allow selection between options (SWG) 

• Keep flexibility (SWG/STC/ESO) 

‣ Changing science, new member states, precursor 

instruments 

• Possibility for submission of new/revised ideas (ESO) 

• Competitive calls for proposals where sensible (STC) 


Instrument Roadmap 

• 7 instruments currently 

identified for 

construction 

• 100M Euros in 

construction budget 

• Construction proposal 

covers first four 

instruments 

• Project Science Team 

involvement in science 

requirements definition 

• This plan will evolve! 

Requirement to 

maintain an “Instrument 

Plan” into the 

operations phase 


ELT-1 and ELT-2 

• First light instruments selected as ELT-CAM and 

ELT-IFU 

‣ Unchanged from version 1 of Instrumentation Plan. 

• These instrument projects include AO capabilities 

• Require 1-2 years to define 

‣ Telescope interfaces, Specifications, Integration of AO 

‣ Contract details 

• Science requirements to be discussed here 

• Negotiation underway with the Phase A consortia 


ELT-3 

• ELT-MIR selected as instrument 3 based on 

readiness and will be based on the METIS study 

• Specifications are well defined 

• Less dependent on best image quality 

• Technically well developed proposal 

• Minimal technology development 

‣ Aquarius detector on-sky tests with VISIR 

‣ Successful outcome required before starting ELT-MIR 

‣ TRL review 2013 


ELT-MIR/METIS: 

MIR ELT Imager and Spectrograph 

o Diffraction limited imager 

[18˝ 18˝] 

o L/M band and N band 

o Includes coronography 

o R 5000 long-slit 

spectrometer 

o includes polarimetry 

o High resolution IFU [ 

0.4˝ 1.5˝] spectrograph 

o for L/M 

o R ~ 100,000 

PI: Bernhard Brandl, 

common 

fore-optics 

cold 

calibration unit 

LM band IFU 

spectrograph 

Nova, MPIA, CEA Saclay, KU Leuven, UKATC 

AO module 

Imager (LM and N- 

band channels) 


ELT-4 and 5 

• Selected to be a MOS instrument (ELT-MOS) and a highresolution 

spectrograph (ELT-HIRES) 

• Science requirements for MOS in 2013 

‣ Call for proposals 


ELT-MOS/OPTIMOS-DIORAMAS 

a wide field imaging MOS 

o Wavelength range 0.37 m-1.4(1.6) m 

o MOS and Imager 

o 6.8‟x6.8‟ FOV 

o Standard visible and NIR filters 

o Multiplex: 

o 480 slits in the visible; 120 for NIR 

o Spectral resolution 

o R~300, 1000, 2500 visible 

o R~400,800,3000 for NIR 

PI: Olivier Le Fèvre 

LAM, IASF-Milano, Obs. 

Haute Provence, Obs. 

Genève, IAC 


ELT-MOS/OPTIMOS-EVE: 

optical-Hband fibre MOS 

o Wavelength range 0.37 m-1.7 m 

o Patrol field - ~7‟ 

o Multiplex options 

o 240 fibres /R~5000 

o 70 fibres / R~15000 

o 40 fibres / R~30000 

o 30 IFUs 1.8” x 3” 

o 1 IFU 7.8”x13.5” 

o Both IFUs / R~5000 

PI: Francois Hammer 

GEPI,NOVA, INAF, RAL, Nils 

Bohr I. 


o Near-infrared: 0.8-2.45 m 

o Patrol field 38arcmin 2 

o 20-IFU fields 

o 

1.65”x1.65” 

o R~4000,10000 

o Multi-Object AO 

o 6LGS, 6NGS 

ELT-MOS/EAGLE: a wide-field 

multi-IFU AO assisted NIR spectrograph 

o >30%EE in 75mas pixels 

PI: Jean-Gabriel Cuby, Simon Morris 

LAM, Uni. Durham, UK ATC, GEPI, 

ONERA, LESIA 


39-mTelescope-Instrument 

Interface Change 

• Removal of the gravity invariant platform 

‣ Implications for the EAGLE instrument are being studied 

by the team as “delta-Phase A” study 







• Science requirements for HIRES spec option in 2013 



ELT-HIRES/CODEX 

high stability, high resolution visible spectrograph 

• Wavelength range 0.37-0.71 m 

• R~130,000 

• Field of view (0.82”) 

• ~2cms -1 Doppler precision over 30yrs 

• no adaptive optics 

• located in the coudé room 

PI: Luca Pasquini, ESO 

Geneve Observatory, IAC, 

INAF-Trieste and Brera, 

IoA 


ELT-HIRES/SIMPLE: 

High resolution NIR spectrograph 

• Wavelength 0.84-2.5 m 

• Complete spectrum 

• R~130,000 

• Slit: 27x450mas 

• Adaptive optics 

‣ SCAO on-board 

‣ MCAO/MAORY 

‣ LTAO/ATLAS 

PI: Livia Origlia 

INAF,UAO, TLS, PUC 







• Science requirements for HIRES spec option in 2013 


• Followed by 1-2 years of further Phase-A 

design/technology development 

• Select in 2015 whether MOS or HIRES to become ELT- 

4/5 

‣ ELT-4 starts in 2016 

‣ ELT-5 starts in 2018 


ELT-6 

• Unspecified instrument 

• A new call for Phase A studies will be issued in 2015 

‣ For rework of existing unselected Phase A studies 

‣ For new ideas 

• Successful proposals will be funded for Phase A or ∆- 

Phase A studies (2 years) 

‣ Competitive Phase A studies 

‣ Technical and scientific reviews of Phase A results 

‣ Proposal to STC/Council 

• 2019 selection/2020 start 


ELT-PCS 

• Instrument selected for construction 

• High priority key instrument 

• High technical risk 

‣ Enabling technology required 

• Strongly affected by ultimate performance of 

telescope 

• Baseline start as late as 2022. Can start earlier if 

required TRL has been reached. 


E-ELT Instrumentation Roadmap | PST 11.07.2012 

Instrument Roadmap

E-ELT Instrumentation Roadmap | PST 11.07.2012 32

The E-ELT Instrumentation Roadmap

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