Astronomical Instrumentation at the European Southern Observatory

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1 Astronomical Instrumentation at the European Southern Observatory Mark Casali General introduction to instrumentation New instruments and opportunities La Silla Paranal Observatory (VLT) E-ELT Instrumentation R & D ESO Industry Days

2 1. Introduction What do we mean by Instrumentation? 3 Instrumentation ESO Industry Days

3 Instrumentation construction ESO Project Institute Consortium Project Industry ESO Industry Days Level of industrial procurements ESO/institutes Industry Instrument System design Subsystem design Subsystem design manufacture manufacture 6 3

4 10 years of change Non-astronomical technology developments Adapted for astronomy Computing, optics Targeted R&D in institutes and industry Detector developments, deformable mirrors Large increase in funds for instruments, matching telescope investments Instruments under development KMOS IR 24-IFU IR spectrograph MUSE 1 arcmin square optical IFU SPHERE high-order AO imager/spectrometer AOF 4-laser, deformable M2, AO facility MATISSE LMN band 4-UT VLTI instrument GRAVITY K-band precision microarcsec VLTI ESPRESSO 10 cm/sec precision optical spectrometer 4

5 Key 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 KMOS (2012) PI R.Sharples, Durham x2.8 IFUs. 0.2 sampling. 3 spectrographs (H2RG) 24 cryogenic pick-off arms, operating on 7.2 field 1 to 2.5 micron operation 10 5

6 l c =2.5 mm HgCdTe eapd unlike silicon HgCdTe offers noiseless avalanche gain of up to 33 3 successful predevelopment studies with 4-channel 320x256 prototype new 32-channel multiplexer in development at SELEX tailored to needs of GRAVITY fringe tracker and AO wavefront sensing 320x256 eapd array cryogenic preamplifier 12 6

7 CCD Mosaic for OmegaCAM 8 x 4 science mosaic of 2K x 4K e2v CCD44-82 devices µ x 15µ pixels (0.21 arcsec x 0.21 arcsec) + two 2K x 4K CCDs for autoguiding + two 2K x 4K CCDs for image analysis (AO and focus) To be commissioned in 2011 on 2.6-m VST 13 Lasers 7

8 Development of industrial fiber Raman sodium laser for VLT AOF 15 Laser Frequency Comb Laser Frequency Combs as calibrators Provides a series of perfectly equidistant lines Covers a large wavelength domain Stabilized at the to level The absolute reference linked to an atomic clock ESO in collaboration with the MPQ have been developing a LFC calibration system for use in astronomical spectrographs since 2008 Tested on HARPS comb Thorium-argon 16 8

9 Development of Piezo DM technology 52 actuator piezo DM COME-ON-PLUS 60 actuator bimorph piezo DM: MACAO 189 act. Piezo DM for NAOS 50x50 actuator matrix of 1mm pitch 1377 act. Piezo DM for SPHERE with its drive electronics Large Deformable mirrors development for AOF Hexapod for centring & fine focusing Cold Plate; heat evacuation & act. attachment Ø 1.1m convex 1170 actuators 29 mm actuator pitch 1 ms response Stroke 50 / 1.5 mm 2mm Thin Shell Reference body 18 9

10 Special optics for AO 1.1 m light-weighted reference body for the VLT Deformable Secondary Mirror 1.1m Zerodur shell, in manufacturing Mass= 47 kg 400 mm toric mirror for SPHERE using stress polishing; <1nm rms WFE VLT E-ELT R&D 2. New Instruments and opportunities If you are interested in specific opportunities please contact: eso_ins@eso.org 10

11 Scale of instrumentation programme Spend in industry M Year VLT ELT total ESO Industry Days VLT 22 11

12 VLT ERIS : AO high-resolution imager/spectrometer Precision mechanical assemblies Stiff mechanical structures Cryogenic Infrared imager (complete assembly) Low vibration 40K cooling system ESO project ESO Industry Days VLT Multi-Object Spectrograph conceptual design studies Two studies for optical and IR instruments Optical and IR fibres Fibre robotic positioners Optics IR and Optical detectors ESO Industry Days

13 ELT Instruments AO module LM band IFU spectrograph Imager (LM and N-band channels) 25 Phase A studies identified the key technologies 26 13

14 Industrial opportunities: detectors Visible light science detectors approx k x 4k low noise CCD detectors 4-6 9k x 9k format sought by optical spectrograph Infrared light science detectors approx 40 4k x 4k low noise NIR (HgCdTe) detectors x 1024 MIR (5-14um) detectors Near infrared and visible wavefront sensor detectors: fast read-out, low noise 20 CCD detectors, format k-squared ~5 HgCdTe detectors, format 1000k-squared (These numbers are inclusive of all planned instruments so will change.) Industrial opportunities: optics The instrument programme will require significant procurement of large optics ( up to ~400mm, lenses and mirrors) Other areas of possible interest Deformable mirrors of ~80x80 sub-apertures Lenslet arrays for wavefront sensors Micro-optics (mm scale) for integral field units (glass and Al) Optical fibres high transmission, broadband Large dichroic mirrors Estimated spend on optics ~30MEuros over

15 EAGLE: near-infrared multi integral-field spectrometer PI: Jean-Gabriel Cuby, LAM ONERA, OPM GEPI & LESIA, UK ATC, Durham Uni. Laser guide star pick-offs Selection of science sources MICADO: NIR, large field, diffraction limited camera PI: Reinhard Genzel, Garching MPE, MPIA Heidelberg, USM, INAF, NOVA, OPM LESIA pupil plane filter wheel input focal plane primary arm collimator MICADO at the direct Nasmyth focus with its own SCAO sensor detector array 30 15

16 MAORY: Multi-Conjugate Adaptive Optics module PI: Emiliano Diolaiti, Bologna INAF (OABo, OaPd, PA Arcetri) ONERA Facility adaptive optics system supporting two instruments. METIS: Mid IR Imager - Spectrograph PI: Bernhard Brandl, Amsterdam NOVA (Leiden and Dwingeloo), MPIfA Heidelberg, CE Saclay DSM/IRFU/Sap, KU Leuven, ATC U common fore-optics cold calibration unit Window AO module LM band IFU spectrograph Imager (LM and N-band channels) 16

17 HARMONI : Single IFU, vis-nir Spectrograph PI: Niranjan Thatte, Oxford Univ. Oxford, CRAL, CSIC, IAC,UK ATC Left, the opto-,mechanical structure inside the 4-m diam. cryostat. Above, the integral field unit. The slicer stack is 64x64mm ATLAS: laser-tomography adaptive optics PI: Thierry Fusco, Paris ONERA, OPM GEPI & LESIA LGS design 17

18 CODEX: high stability optical spectrograph PI: Luca Pasquini, ESO Geneve Observatory, IAC, INAF, IoA Cambridge 2.7m SIMPLE: high resolution NIR echelle spectrograph PI: Livia Origlia INAF (Bologna, Arcetri, Roma), UAO, TLS, PUC 18

19 EPICS Exoplanets Imaging Camera Spectrograph PI: Markus Kasper, ESO LAOG,LESIA, Uni. Nice, LAM,ONERA, Uni.Oxford, INAF (Padova), ETH Zurich, NOVA ( Amsterdam, Utrecht) OPTIMOS EVE: Optical-NIR MOS Fiber-based PI: Francois Hammer, GEPI NOVA, INAF, RAL, AIP, ZfA Heidelberg, NBI Copenhagen NIR camera VPH grating exchange Slit exchange 19

20 OPTIMOS-DIORAMAS: Optical slit-mos + imaging PI: Olivier LeFevre, Marseille LAM, IAC, IASF-Milano Camera entrance pupil ~250mm OPTIMOS-DIORAMAS at the E-ELT Nasmyth focus Instrumentation ELT R&D Short time, low risk development & prototyping will be made within the instrument projects Under the responsibility of the project consortium Funded within the cost of the instrument Related milestones will be defined with Consortium Longer time, key enabling technologies with higher risk for the project will start before the instrument selection (upon ELT approval) ESO is preparing a long term development plan for instrumentation which will be updated on a two-year basis 40 20

21 Technology developments required for the first light instruments (I) R&D description Purpose Time scale/funding remarks Hawaii 4RG developments 1.5K 2 visible wavefront sensor detector; low noise high frame rate 1.5k 2 detector controller at high frame rate IR detectors required for ELT-CAM & ELT-IFU ELT-MCAO & LTAO LGS WFSing require large detector to cope with laser spot elongation ELT-MCAO & LTAO LGS WFSing On-going development funded by ESA. Detectors will be provided on loan to ESO for testing. Dev. Time expected Simulations & laboratory experiment using actual Sodium profile from the University of British Columbia will be used to finalize the actual detector size required to achieve the MCAO & LTAO performance. The 1.5k 2 development will start when the will be completed end Development time expected FP7 OPTICON will start the design of the controller. Additional funding from ESO will be required to complete the work for the 1.5k 2. Synergies with the telescope wavefront Control needs will be explored. Dev. Time expected: R&D requirements for the capabilities in the pool for future instruments (I) R&D description Purpose Time scale /funding remarks 1k 2 Mid IR detector: AQUARIUS fast low noise visible detector system for WFSing High efficiency, large format VPH & grating Conventional Cryogenic Robotic filter/grating exchange Mid IR detector required for ELT-MIR ELT-PCS: Planetary Camera & Spectrograph Better ELT-IFU, ELT- HRS: High stability optical spectrograph & ELT-MOS: Multiobject spectrograph ELT-MOS Funded by on-going VISIR upgrade project. Dev. Time expected The SPHERE dev. has funded the dev of a WFS detector able to run at 1.2kHz. Further work on the detector controller should bring the frame rate to the required level of 2.5kHz for the ELT High contrast instrument. This should be confirmed early enough such as to determine if a new detector dev. is required or not: Some of that effort might be funded by OPTICON-JRA2. On-going work in the frame of OPTICON may provide the R&D funding from the current plan. Marginal effort still required to secure the technology: Share efforts between ESO & the potential instrument builders will be needed to identified 42 21

22 Technology developments required for the first light instruments (II) R&D description Purpose Time scale/funding remarks Fast, low noise, NIR detector for tip-tilt/low order WFSing ELT-MCAO & LTAO low order WFSing & truth sensor Current R&D funding from ESO-VLT program is addressing that need for the E-ELT (Gravity WFSing and fringe tracking). Dev. Time expected: AO Real Time control & smart algorithms ELT-MCAO & LTAO On-going studies within the framework of the Austrian inkind contribution to ESO & other collaborations should provide a reasonable basis for the innovative algorithms required for the ELT AO systems ( ). The mapping of these algorithms to actual RTC architecture will need a specific effort included in the R&D plan. The dev. of the RTC able to cope with the computing power requirements both in Real-Time and Off-line needs a specific and significant effort included in the R&D plan. Conceptual design begins 2012, 1st MCAO RTC prototype in Additional inputs may come from OPTICON 43 Technology developments required for the first light instruments (III) R&D description Purpose Time scale/funding remarks Medium size (400mm) deformable mirror & drive electronics ELT-MCAO Deformable mirrors with about 8mm pitch & ~50x50 actuators as well as their drive electronics are not off the shelf product today. Development of a scaled down demonstrator and drive electronics will be required. ESO-TMT common interests have been identified here. This R&D will be launched when the design of the MCAO system is consolidated beg Design & prototyping of drive electronics should be done earlier 2012 AO simulations development ELT-MCAO & LTAO The existing ESO simulation tools/cluster will be upgraded such as to complement the simulations made by the Consortia actuator Open loop DM & drive ELT-LTAO for low order WFS and high sky coverage, potentially SCAO postfocal DM mitigation, longer term ELT-MOS with MOAO (TBC) An alternative technology to Piezo DM is essential to mitigate the risk of having only one DM supplier and to address the new open loop AO needs (LTAO & ELT-MOS-MOAO). Initial funding from OPTICON might be available to push further the appropriate technology but ESO will need to complement this dev.:

23 Technology developments required for the first light instruments (IV) R&D description Purpose Time scale /funding remarks AO critical studies: On-sky calibrations Optimum control Cn2 identification: MCAO-LTAO Control matrix rotation management PSF reconstruction Cryogenic: Explore the temperature limit of LN2 cooling Close Cycle coolers Advanced cryo-mechanics Very accurate and low continuous motion at cryogenic temperature Bearings development Motors (Brushless motors / stepper motors) Cryogenic encoders ELT-MCAO & LTAO Cryogenic instruments Cryogenic instruments Studies will be prioritized in 2012 according to the final AO-instrument plan. Some of these items are being addressed in the frame of VLT AOF, GALACSI and also by the CANARY pathfinder at WHT. All critical issued should be addressed by PDR of ELT MCAO & LTAO: ESO R&D plan will need to fund these areas. ESO R&D plan will need to fund these areas. 45 R&D requirements for the capabilities in the pool for future instruments (II) R&D description Purpose Time scale /funding remarks High Efficiency coatings: High reflectivity for Coude Required for the Coude path (800mm diameter, nm) Marginal effort still required to confirm the efficiency: IR Laser Comb development Fiber technology Cryogenic scrambling High contrast demonstrators ELT- High stability infrared spectrograph ELT-MOS ELT-HRS ELT-PCS: Planetary Camera and Spectrograph Visible laser comb dev are being funded for ESPRESSO. New dev. will be required for the IR Marginal R&D to consolidate the feasibility of these key components Marginal ESO funding will be required to accompany the essential on-going high contrast techniques in the community (Speckle nulling, Fresnel & Chromatic effects, polarimetric performance, slicer, algorithm, post-processing techniques..). ESO will accompany these efforts when appropriate

24 R&D requirements for the capabilities in the pool for future instruments (III) R&D description Purpose Time scale /funding remarks High computing power AO Real Time control and algorithms High density act. DM & drive electronics Novel roof-pyramid WFS ELT-PCS: Planetary Camera and Spectrograph ELT-PCS: Planetary Camera and Spectrograph ELT-PCS: Planetary Camera and Spectrograph The extreme computing power requirements for the ELT- PCS will need specific & well focused R&D in term of algorithms (on-going Austrian in-kind effort & other collaborations in FP7), algorithm mapping and Real Time Computer architecture beyond what will be done for ELT- MCAO. Current assumption: ELT-PCS requirements are taken into account in the ELT-MCAO RTC dev. therefore the delta effort for ELT PCS is minimum. This will need to be confirmed in st RTC prototype for ELT-PCS: The current R&D plan includes only the demonstration of the critical technological bricks required to dev the DM and drive electronics for ELT PCS, not the 1st DM included in the cost of the ELT-PCS. Some of these bricks might be funded in the frame of OPTICON: On-going effort within the community on that topic. 47 END 24