The E-ELTTelescope, instruments, technology

Mark Casali

Project Goal

To deliver and commission, in 2024 and within

budget, the fully functional and complete

European Extremely Large Telescope

➢39.3 m segmented optical telescope on Cerro

Armazones

➢Part of the La Silla Paranal Observatory, operated

from existing facilities at Paranal

➢ It has been organised to include the essential planning

and management staff with most of the effort being

provided by Directorate of Engineering through the

matrix structure

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Armazones and Paranal

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The E-ELT

40-m class telescope: largest optical-

infrared telescope in the world.

Segmented primary mirror.

Active optics to maintain collimation

and mirror figure.

Adaptive optics assisted telescope.

Diffraction limited performance.

Wide field of view: 10 arcmin.

Mid-latitude site (Armazones in Chile).

Fast instrument changes.

VLT level of efficiency in operations.

The Science

Contemporary science:

Exoplanets: radial velocity detections, direct imaging,

transit spectroscopy, proto-planetary disks

Fundamental physics: GR in the strong field limit,

variation of fundamental constants, expansion history

of the Universe

Resolved stellar populations: beyond the Local

Group

The physics of high-redshift galaxies

…and much more!

Synergies with other top facilities:ALMA

JWST

LSST and other survey telescopes

SKA

Discovery potential:Opening new parameter space in terms of

spatial resolution and sensitivity

SKA

JWST

ALMA

LSST

The E-ELT Project

Top priority of European ground-based astronomy (on Astronet and ESFRI lists).

Cerro Armazones in Chile selected as the E-ELT site in April 2010.

Detailed Design Phase completed in 2011. Construction Proposal published in Dec

2011.

Instrument Roadmap (Nov 2011): 2 first-light instruments + plan for 1st generation.

Project fully approved in Dec 2012.

Construction started in 2013.

Start of operations early next decade.

Construction cost: 1083 M€ (including first-light instrumentation).

The Telescope

Nasmyth telescope with a segmented

primary mirror.

Novel 5 mirror design to include

adaptive optics in the telescope.

Classical 3mirror anastigmat + 2 flat

fold mirrors (M4, M5).

M1 (seg): 39.3 mM1 (seg): 39.3 m

M2: 4.2 mM2: 4.2 m

M5 (TT): 2.6x2.1 mM5 (TT): 2.6x2.1 m

Nasmyth focusNasmyth focus

M3: 3.8 mM3: 3.8 m

M4 (AO): 2.4 mM4 (AO): 2.4 m

M1 (seg): 39.3 m

M2: 4.2 m

M5 (TT): 2.6x2.1 m

Nasmyth focus

M3: 3.8 m

M4 (AO): 2.4 m

• Two instrument platforms nearly the size

of tennis courts can host 3 instruments

each + Coudé lab.

• Multiple laser guide stars, launched from

the side.

• Nearly 3000 tonnes of moving structure.

The Mirrors

M1: 39.3 m, 798 hexagonal segments of 1.45 m tip-to-tip: 978 m2 collecting area

M4: 2.4 m, flat, adaptive 6000 to 8000 actuators

M5: 2.6 x 2.1 m, flat, provides tip-tilt correction

The Dome

Classical design.

Diameter = 86 m, height = 74 m.

~3000 tonnes of steel.

Fully air-conditioned and wind

shielded.

✓Site visit 29 January 2014

✓Release Call for Tender Phase 1 5 May 2014

✓Acknowledgement of receipt 3 June 2014

✓Bidders Conference 12 June 2014

✓Deadline questions phase 1 5 January 2015

✓Closing date phase 1 31 January 2015

➢ Release Call for tender Phase 2 15 April 2015

➢ Closing date phase 2 15 June 2015

➢ Release BAFO 1 Sept 2015

➢ Deadline BAFO 15 Sept 2015

DMS CfT updated Planning

The first … … and the last

Before and after blasting

25 – 04 - 2014

Before and after blasting

15 – 02 - 2015

Instrumentation at ESO

13 operational instruments on the VLT

KMOS – in operation

Instrument projects

ESO

Consortium of

Institutes

ESO Project

Project

Industry

ESO Contracts and

Procurement

Instrument System

design

Subsystem

designSubsystem

design

manufacture manufacture

Industry

ESO/institutes

Level of procurement

Instrument Procurement model

Majority of instruments obtained from consortia (teams) of member-state institutes

➢Some instruments led by ESO often with institute participation

ESO establishes agreement for construction after a competitive phase

➢ESO pays full hardware/industrial costs• 2-6 M€ for VLT, 10-30 M€ for ELT

➢ Institutes pay for staff to run projects• ESO pays this back with Guaranteed time (200+ VLT nights)

Imager (LM and

N-band channels)

LM band IFU

spectrograph

AO module

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Developed in

consultation with

scientific advisory

groups

Status: Working

with selected

consortia on

Technical

Specifications,

Statements of

Work, Agreements

Instrument RoadmapYear ELT-

IFUELT-CAM

ELT-MIR

ELT-MOS

ELT-HIRES

ELT-6 ELT-PCS

2014 Decide science requirements, AO

architecture.

VISIR start

on-sky

Develop TLRs for MOS/HIRES

Calls for Proposals

Start ETD

2015 Start Phase A

2016 Consortium Selection for construction

Call for proposal

2017

2018 TRL check

2019 Selection Start if ready

2020

2021

2022

2023

2024

Pre-studies taking the form of phase A or delta-phase A work and/or ESO-fundedEnabling Technology Development (ETD)

Decision point

We intend to sign 4 contracts for instrument

construction in 2015

➢ MICADO MCAO camera

➢ MAORY MCAO system

➢ HARMONI IFU spectrometer + LTAO system(PDR)

➢ METIS thermal IR imager & spectrometer

Instrument progress

HARMONI (+LTAO)

IFS spectrometer. PI : Niranjan Thatte

Univ of Oxford UK

UK ATC UK

CRAL France

ONERA France

Obs Marseille France

IAC Spain

CSIC Spain

ESO

MICADO

AO-corrected camera. PI: Ric Davies

MPIE Germany

USM Germany

MPIA Germany

IoA Gőttingen Germany

Nova Netherlands

LESIA France

Univ of Vienna & Linz Austria

INAF (Padova) Italy

ESO

METIS

Mid-IR imager & spectrometer. PI: B Brandl

NOVA Netherlands

CEA Saclay France

ETH Switzerland

KU Leuven Belgium

MPIA Germany

UKATC UK

Univ of Vienna Austria

ESO

MAORY

MCAO system for MICADO: Emiliano Diolaitti

INAF/IASF(Bol) Italy

INAF –Padova/Capod./Brera

Italy

UKATC UK

Univ of Durham UK

IPAG France

ESO

Base-line 39m E-ELT design to be kept➢No need for further technical or programmatic reviews

➢Essentially no scope for overall reduction in cost• All such options exercised by going from 42m to 39m design

Divide construction into two phases➢Phase 1 affordable without Brazil as MS

• Provides working 39m E-ELT with limited instrumentation

• Scientifically world-leading and programmatically feasible

• Council to authorize major spending in Dec 2014

➢Phase 2 should be possible at any time• Components could be approved when funding would allow it

• Would be reinstated in toto as soon as Brazil joins

The two-phase approach

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KO

Foundations

Acceptance Dome Acceptance MS

Design

Manufacture

Assembly

Complete

M1 Blanks

M1 Polishing

M2 Blank

M2 Mirror and Cell

M3 Mirror and Cell

M3 Blank

M4

M5/PFS/Lasers

Road and Platform

ARM/PAR Facilities

Mirror Facilities 1st LightMirror Coating and Assembly

Integration and Alignment

Commissioning

E-ELT Construction Schedule & Critical Path

M1 Segment Supports

Cryogenics

Optics

Vacuum

Precision mechanics (also cryogenics)

Deformable mirrors

Stiff, light structures

Imaging detectors

Low-noise electronics

Real-time computing

Control systems and software

Technologies

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HO deformable mirror systems

crucial for ELT instrumentation

➢ Currently in a very difficult situation

➢ MCAO. 2000 actuators.

➢ PCS (Epics). >20,000 actuators

➢ Open-loop DMs

VLT AO instruments envisioned

➢ MCAO

➢ Extension to optical range

SPHERE DM

First Light at OT, 21.1.2015

dbonacci@eso.org

589nm Na Laser testing ongoing

Brightness of artificial star

Seasonal variations

Variations with earths field angle

Pumping of satellite lines

Preliminary Design Review for the M1 Local Control System (LCS) PDR passed successfully end of 2014

➢Supported by prototyping activities

ELT Engineering

✓Contracts signed by CESA (Spain) and VDL-TNO (NL) for final

design. One to be selected for construction.

✓Kick-off-Meetings held with VDL (26 Jan), and with CESA (10 Feb)

M1 Segment Support

CESA proposed concept VDL-TNO proposed concept

M4 Unit (ADS), DP integration results

Demonstration

Prototype

INTEGRATED

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M4 Unit, DP final optical tests

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end