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Optical Detector Systems at the European Southern Observatory

Optical Detector Systems at the European Southern Observatory. Dietrich Baade & Optical Detector Team (ODT). Work at ESO on infrared detectors covered in:. Dorn et al. Finger et al. Mehrgan et al. Beletic et al. The ODT Themes. VLT 2 nd generation instruments:.

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Optical Detector Systems at the European Southern Observatory

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  1. Optical Detector Systems at the European Southern Observatory Dietrich Baade & Optical Detector Team (ODT) Work at ESO on infrared detectors covered in: Dorn et al. Finger et al. Mehrgan et al. Beletic et al. Dietrich Baade & ODT: Optical Detector Systems at ESO

  2. The ODT Themes VLT 2nd generation instruments: • X-shooter – the 0.3-to-2.4 μm rapid-response spectro-cannon • MUSE – the cosmic inventory taker • Shift in emphasis from scientific imaging to signal sensing: Without AO, ELTs will not bring any improvement. • The MAD adaptive optics system tests enabling technology with bright natural guide stars. • The OPTICON project with e2v L3 Vision technology aims to push this towards the ultra-low noise domain. • The New General detector Controller (NGC) is a key stepping stone. • More to come VLT projects in their own right but with an additional view of getting ready for OWL: OmegaCAM for the VLT Survey Telescope (VST) Dietrich Baade & ODT: Optical Detector Systems at ESO

  3. Multi-conjugated Adaptive Optics Demonstrator • MAD tests two wavefront-sensing (WFS) concepts: • star oriented, using multiple Shack-Hartmann (SH) systems • layer oriented (LO), using multiple pyramids • 3 SHWFS + 2 LOWFS detector systems with • e2v CCD39 devices (80 x 80 pixels) • Only one method used at a time • One FIERA controller • Up to 400 frames/s (500 frames/s with 2x2 binning) • Considerably exceeds original FIERA spec of 1 Mpixel/s • Read noise: ~7 e- Reiss et al. Dietrich Baade & ODT: Optical Detector Systems at ESO

  4. Next-generation Wavefront Sensing: OPTICON and e2v L3 Vision Technology AO systems for 2nd-gen. VLT instruments and OWL require: • >1,000 actuators (→ >1,000 x 6x6 pixels) • ~1 kHz frame rate • negligible read noise even when photon noise ~100% • high movability (→ no real cryogenics → dark current) • OPTICON project received funding from EU Commission • CCD220 being developed by e2v • 1 system foreseen for HAWK-I, 4 for MUSE Downing et al. Dietrich Baade & ODT: Optical Detector Systems at ESO

  5. OmegaCAM (1° x 1° imager) • Three FIERAsand 32 (+4) e2v CCD44-82 devices • Very robust since first switch-on • The coordination of autoguiding, closed-loop wavefront sensing, and shutter control is one of the show pieces. • Built as designed • Commissioning in 2006 • Strict attention to safety • Extensive detector characterization on ESO’s test bench • Innovative cooling system very effective Iwert et al. Christen et al. (2x) Lizon et al. Dietrich Baade & ODT: Optical Detector Systems at ESO

  6. X-shooter • Basically a single-mode VLT Cassegrain instrument for singular events (`point and shoot´) • Simultaneous wavelength coverage 0.3 – 2.4 μm • First ESO instrument to bridge the 1-micron barrier • 2 optical arms (e2v CCD44-82 and MIT/LL CCID-20) • 1 IR arm (Rockwell Hawaii-2 RG) • 1 IRACE and 1 FIERA controller each • FIERA software defines 2 fully independent virtual cameras on one common DFE • Approaching Final Design Review • Commissioning in 2008 Dietrich Baade & ODT: Optical Detector Systems at ESO

  7. Multi-unit Spectroscopic Explorer (MUSE) • Twenty-four separate detector systems • 4K x 4K CCDs (or 2 x 1 mosaics) • 465 – 930 nm: high red response is mission critical • Need to save mass and volume • Must ease AIT • Reliability will be vital • First optical instrument to use NGC • 2nd-generation cryostat head • Prototype detector system at the end of 2006 Reiss et al. Dietrich Baade & ODT: Optical Detector Systems at ESO

  8. Cryostat Cleanliness and Control Plasma cleaning: • fast, effective, low risk, low operating cost • excellent results with big OmegaCAM cryostat Deiries et al. • H20 exorcism • baking of CCDs in gas stream • accidental (re-)discovery • PULPO2 housekeeping unit with enhanced • shutter ( ) and temperature control • temperature and pressure monitoring Reif et al. Geimer et al. Dietrich Baade & ODT: Optical Detector Systems at ESO

  9. New General detector Controller (NGC) • In the decade since 1998, a total of 30 FIERA and IRACE systems will be deployed. • Extremely successful (nearly negligible telescope downtime) but some other limitations: • mass, volume, power dissipation • obsolete components • voltage range and swing • speed, number of channels • 2 successes (= 2 costs) • Proto-typeof joint successor NGC has seen `first light´ • First deployments: KMOS (2009) and MUSE (2011) Meyer et al. Cumani et al. Reyes et al. a Dietrich Baade & ODT: Optical Detector Systems at ESO

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