The E-ELT Telescope, instruments, technology. Mark Casali

Transcription

1 The E-ELT Telescope, instruments, technology Mark Casali

2 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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4 Armazones and Paranal 4

5 The E-ELT 40-m class telescope: largest opticalinfrared 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.

6 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 Group The physics of high-redshift galaxies and much more! Local ALMA Synergies with other top facilities: ALMA JWST LSST and other survey telescopes SKA Discovery potential: Opening new parameter space in terms spatial resolution and sensitivity JWST of LSST SKA

7 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 Detailed Design Phase completed in Construction Proposal published in Dec Instrument Roadmap (Nov 2011): 2 first-light instruments + plan for 1st generation. Project fully approved in Dec Construction started in Start of operations early next decade. Construction cost: 1083 M (including first-light instrumentation).

8 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). M2: 4.2 m M4 (AO): 2.4 m M5 (TT): 2.6x2.1 m M3: 3.8 m Nasmyth focus M1 (seg): 39.3 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.

9 The Mirrors M1: 39.3 m, 798 hexagonal segments of 1.45 m tip-to-tip: 978 m 2 collecting area M4: 2.4 m, flat, adaptive 6000 to 8000 actuators M5: 2.6 x 2.1 m, flat, provides tip-tilt correction

10 The Dome Classical design. Diameter = 86 m, height = 74 m. ~3000 tonnes of steel. Fully air-conditioned and wind shielded.

11 DMS CfT updated Planning 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

12 The first and the last

13 Before and after blasting

14 Before and after blasting

15 Instrumentation at ESO 13 operational instruments on the VLT

16 KMOS in operation

17 Instrument projects ESO ESO Project Consortium of Institutes ESO Contracts and Procurement Project Industry

18 Level of procurement ESO/institutes Industry Instrument System design Subsystem design Subsystem design manufacture manufacture

19 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, M for ELT Institutes pay for staff to run projects ESO pays this back with Guaranteed time (200+ VLT nights)

20 AO module LM band IFU spectrograph Imager (LM and N-band channels) 20

21 Year ELT- IFU ELT- CAM 2014 Decide science requirements, AO architecture. ELT- MIR VISIR start on-sky ELT- MOS ELT- HIRES Develop TLRs for MOS/HIRES Calls for Proposals 2015 Start Phase A 2016 Consortium Selection for construction 2017 Instrument Roadmap ELT-6 Call for proposal ELT- PCS Start ETD 2018 TRL check 2019 Selection Start if ready Pre-studies taking the form of phase A or delta-phase A work and/or ESO-funded Enabling Technology Development (ETD) Decision point Developed in consultation with scientific advisory groups Status: Working with selected consortia on Technical Specifications, Statements of Work, Agreements

22 We intend to sign 4 contracts for instrument construction in 2015 MICADO MCAO camera MAORY MCAO system Instrument progress HARMONI IFU spectrometer + LTAO system(pdr) METIS thermal IR imager & spectrometer

23 HARMONI (+LTAO) IFS spectrometer. PI : Niranjan Thatte Univ of Oxford UK ATC CRAL ONERA Obs Marseille IAC CSIC ESO UK UK France France France Spain Spain

24 MICADO AO-corrected camera. PI: Ric Davies MPIE USM MPIA IoA Gőttingen Nova LESIA Univ of Vienna & Linz INAF (Padova) ESO Germany Germany Germany Germany Netherlands France Austria Italy

25 METIS Mid-IR imager & spectrometer. PI: B Brandl NOVA CEA Saclay ETH KU Leuven MPIA UKATC Univ of Vienna ESO Netherlands France Switzerland Belgium Germany UK Austria

26 MAORY MCAO system for MICADO: Emiliano Diolaitti INAF/IASF(Bol) INAF Padova/Capod./Brera UKATC Univ of Durham IPAG ESO Italy Italy UK UK France

27 27 The two-phase approach 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

28 E-ELT Construction Schedule & Critical Path Road and Platform KO Design Manufacture Foundations Assembly Acceptance Dome Acceptance MS M1 Segment Supports M1 Blanks M1 Polishing M2 Blank M2 Mirror and Cell M4 M3 Mirror and Cell M3 Blank M5/PFS/Lasers ARM/PAR Facilities Mirror Facilities Mirror Coating and Assembly 1 st Light Integration and Alignment Commissioning Complete

29 29 Technologies Cryogenics Optics Vacuum Precision mechanics (also cryogenics) Deformable mirrors Stiff, light structures Imaging detectors Low-noise electronics Real-time computing Control systems and software

30 HO deformable mirror systems crucial for ELT instrumentation Currently in a very difficult situation MCAO actuators. PCS (Epics). >20,000 actuators Open-loop DMs VLT AO instruments envisioned MCAO Extension to optical range SPHERE DM

31 First Light at OT, nm Na Laser testing ongoing Brightness of artificial star Seasonal variations Variations with earths field angle Pumping of satellite lines

32 ELT Engineering Preliminary Design Review for the M1 Local Control System (LCS) PDR passed successfully end of 2014 Supported by prototyping activities

33 M1 Segment Support 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) CESA proposed concept VDL-TNO proposed concept

34 34 M4 Unit (ADS), DP integration results Demonstration Prototype INTEGRATED

35 M4 Unit, DP final optical tests 35

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