Technological Developments at ESO. Adrian Russell Director of Programmes

Transcription

1 Technological Developments at ESO Adrian Russell Director of Programmes

2 Philosophy Delivery of maximum science Need to be at cutting edge of technology in key areas (detectors, AO, optics, lasers) Risk mitigation Areas of risk in projects must be controlled and limited New technology must be demonstrated and prototyped before instrument final design

3 Scope and organisation Technology development is handled variously Most commonly, developments are included within the scope of a project Appropriate technology readiness criteria and milestones defined as part of project lifecycle Some developments are pursued outside an approved instrument project In anticipation of future requirements Especially if development time is very long Some Recent highlights...

4 mid-ir array AQUARIUS 1Kx1K Si:As blocked impurity band array covering =5-28 m first light image TIMMI2 test camera AQUARIUS 1Kx1K array in socket simple SFD in unit cell low gain : 1E6 electrons high gain : 1E7 electrons 64 outputs: 32 at top 32 at bottom stripe in center: start of readout 120 frames/s temperature T=8K needed for VISIR upgrade and MATISSE pathfinder for ELT (METIS)

5 c =2.5 m 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 sensor 320x256 eapd array cryogenic preamplifier thermal target

6 Noise of eapd prototype VLTI needs readout noise of 3 erms at frame rate of 1KHz APD gain ~ 33 frame time 3.37 ms 6 Mpixel/s on 4 outputs readout noise: 2.8 e rms DCS 0.95 e rms Fowler-8 for comparison readout noise of conventional CMOS H2RG: ~100erms cosmetic quality of APD may improve by replacing LPE with MOVPE (next study)

7 SIDECAR ASIC for Hawaii-2RG complete controller integrated on a single chip including MHz ADCs with 12 bit resolution only digital fiber interface to NGC environment Hawaii-2RG can be read with 7 frames /s facilitates deployment of large ELT mosaics HyViSI detector SIDECAR ASIC Flexcable ESO interface card

8 Camera for AO Wavefront Sensing Key requirements: 1200 frames/s < 1 e - read noise Detector not available off the shelf Custom development of CCD220 device with e2v (UK), based on e2v L3Vision electron-multiplication technology Developed special branch of ESO s New General detector Controller (NGC)

9 CCD Mosaic for OmegaCAM 8 x 4 science mosaic of 2K x 4K e2v CCD44-82 devices 268x 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

10 Laser Frequency Comb Actual calibration sources for high resolution - high precision spectrographs have achieved its limits To meet new scientific challenges such the detection of Earth-like planets or the measure of the expansion of the Universe, novel systems are required Laser Frequency Combs are the right choice 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

11 Laser Frequency Comb Development carried out in phases: Assessment of mode separation: achieved beyond initial specs (> 50 GHz) LFC source: Yb fs-fibre 1030 nm, repetition rate 250 MHz plus frequency doubling Spectral broadening: Photonic Crystal Fiber (achieved bandwidth so far > 150nm) Test at telescope (HARPS) confirmed successful achievements Astro-comb Th-Ar Astro-comb: ~450 lines per order, 5cm/sec PHOTON NOISE LIMITED stability in short term Th-Ar: ~150 lines per order AND STILL ROOM FOR IMPROVEMENT!!! Application: HARPS, CRIRES, ESPRESSO and any requiring high precision and accurate calibrations!

12 Continuous Flow Cryostats Need for small, light and orientation in-sensitive system to cool CCD detector to 140 K A compact (8 Kg) cryostat have been designed based on a continuous circulation of LN2 Actually 15 of these cryostats are in operation One of the future instrument MUSE will be fitted with 24 of them

13 Cryomechanisms Developed by the KMOS consortium

14 Large Cryogenic Bearings Need for large ball bearings for movable components in cryogenic instrument Some hybrid bearings have been build They have been tested in our cryogenic test facility The slit wheel of ISAAC is working since 1998 with a 2000 mm bearing with gold races and ruby balls Corresponding ball bearings Filter wheel for 4m telescope instrument Filter wheel for 8m telescope instrument

15 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 m 2mm Thin Shell Reference body

16 1.1 m light-weighted reference body for the VLT Deformable Secondary Mirror Special optics for AO 1.1m Zerodur shell, in manufacturing Mass= 47 kg 400 mm toric mirror for SPHERE using stress polishing; <1nm rms WFE

17 SPARTA ESO today Real Time Computer & control GB Ethernet Switch RTC box Complexity vs time EPICS Future E-ELT needs MAORY Complexity (logscale in MAC/s) NAOS Co-processing cluster AOF SPHERE NGSGLAO RTC for MACAO In 2002 SCAO ATLAS LGSGLAO NAOS MACAO EAGLE SPHERE AOF SCAO NGSGLAO LGSGLAO ATLAS MAORY EAGLE MACAO EPICS

18 Development of Piezo DM technology 52 actuator piezo DM COME-ON-PLUS 60 actuator bimorph piezo DM: MACAO 189 act. Piezo DM for NAOS 2500 actuator matrix of 1mm pitch 1377 act. Piezo DM for SPHERE with its drive electronics

19 The Current LGSF at UT4

20 Development of industrial fiber Raman sodium laser for VLT AOF

21 High contrast demonstration experiments XAO with 90% H-band Strehl APLC coronagraphy for EPOL Speckle Nulling /10 Spectral deconvolution with 250x speckle rejection

22 AO Future WFS detectors (large format, low noise) e-apd in IR, CMOS Fast RTCs High order deformable mirrors Pulsed Lasers Science Detectors 4kx4k in the IR Cryogenics Vibration control and specification Continuous flow infrastructure for ELT