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Optical Detector Systems at ESO (Projects completed or started since DfA2005)

Explore completed and ongoing projects since 2005, covering innovations in detector technology for various instruments at ESO, including MUSE, ZIMPOL, and more. Details on developments, upgrades, and future prospects.

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Optical Detector Systems at ESO (Projects completed or started since DfA2005)

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  1. Dietrich Baade: Optical Detector Systems at ESO Optical Detector Systems at ESO (Projects completed or started since DfA2005) Dietrich Baade & Andrea Balestra, Claudio Cumani, Sebastian Deiries, Mark Downing, Christoph Geimer, Olaf Iwert, Roland Reiss, Javier Reyes, and Mirko Todorovic For more details see also www.eso.org/sci

  2. Dietrich Baade: Optical Detector Systems at ESO Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing

  3. Dietrich Baade: Optical Detector Systems at ESO New General detector Controller (NGC) • Joint development of IR and Optical Detector Departments • First preview at DfA2005 • First systems delivered to MUSE (24xCCD), KMOS (3xH2RG), • SPHERE (1xH1, 2xH2RG), ZIMPOL (2xCCD); < 1 MHz • High-speed versions for IR VLTI and WFS applications under test • (e.g., 3 MHz: Raytheon Aquarius; 10 MHz: Selex eAPD) • Compact optical WFS variant underway (e2v EMCCD220; 14 MHz) NGC is the standard for all forthcoming ESO detector systems. See also: Talk by Meyer et al. (H/W) Talk by Stegmeier & Cumani (S/W) Poster # 12-B by Reyes et al. (AO) Demonstration at ESO HQ

  4. Dietrich Baade: Optical Detector Systems at ESO Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing

  5. Dietrich Baade: Optical Detector Systems at ESO OmegaCAM 16k x 16k mosaic of 32 e2v CCD44-82 2k x 4k CCDs for one-degree imaging with the 2.6-m VLT Survey Telescope (VST) on Paranal Instrument on Paranal; fully functional and waiting for commissioning call However, one CCD arrived dead with an inner short Concern: Similar, earlier incident with one of the OmegaCAM spare CCDs Replacement in 11/2009 Iwert et al., DfA2005

  6. Dietrich Baade: Optical Detector Systems at ESO X-shooter • First ESO UV-to-IR (0.3-2.5 μ) instrument; three spectrographs / detector systems • IR arm (1.02-2.48 μ; H2RG) uses IRACE • For the optical, FIERA controller software • defines 2 nearly fully independent virtual • cameras on one common front-end electronics: • UVB system (0.3-0.56 μ; MIT/LL CCID-20) • VIS system (0.55-1.02 μ; e2v CCD44-82) • Last FIERA and IRACE systems • Delivered in 2008 (optical systems: M. Downing)

  7. Dietrich Baade: Optical Detector Systems at ESO MUSE (Multi-Unit Spectroscopic Explorer) • Survey instrument for deep spectroscopic stock taking • FoV: 1 arcmin x 1 arcmin (sampling: 0.2 arcsec x 0.2 arcsec) • 24 spectrographs with one e2v 4k x 4k DD CCD231 each • 0.4 Gpixels (50% more than OmegaCAM) • Four 6-board NGC boxes – single system Graded AR coating • First unit delivered, serial production through 2011 • CCD PSF ~0.8 pixels • ~50,000 spectra/exposure Poster # 11-B (Reiss et al.)

  8. Dietrich Baade: Optical Detector Systems at ESO ZIMPOL (SPHERE) SPHERE: (Exo-)planet finder ZIMPOL: Zurich Imaging Polarimeter Image exo-planets using the polarization of the star light scattered off their surfaces (contrast: ~108 @1”) • Two e2v CCD44-82 2kx4k detectors in • frame-transfer mode (2x2 binning) • kHz up/down line shift (“zebra” mask) • synchronized with polarization modulator • Frame rate: 1 Hz • Delivery: 2009/2010 (Mark Downing)

  9. Dietrich Baade: Optical Detector Systems at ESO Detector Upgrades of Existing Instruments Reduced fringing (additional graded AR coating - as in MUSE - is still better!) Improved red QE Deep-depletion silicon See also talk by Downing et al. on bulk-silicon (70 μ) CCDs Standard silicon

  10. Dietrich Baade: Optical Detector Systems at ESO Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing

  11. Dietrich Baade: Optical Detector Systems at ESO Curved Detectors Curved detectors enable optical designs not realistically feasible with flat detector plus field flattening lens. Radius of curvature: 500 mm (goal: 250 mm) CfT for feasibility study in preparation Poster # 18-A (Iwert et al.) Concave detectors Rogers et al. Rogers et al. 2008

  12. Dietrich Baade: Optical Detector Systems at ESO Ultrastable Cryostat The E-ELT echelle spectrograph CODEX and its VLT predecessor ESPRESSO aim at stepwise advancing the accuracy of velocity measurements from the present ~100 cm/s to ~1 cm/s (= 0.02 mph). Top scientific aim: Model-independent measurement of the expansion history of the Universe. Requirements on detector stability are formidable : ~100 pm or ~1 Si atom Poster # 17-A (Iwert et al.) Adam Riess

  13. Dietrich Baade: Optical Detector Systems at ESO UV QE Enhancements The QE of a wide range of CCDs responds positively to baking in dry air and simultaneous UV flooding. Long storage under high vacuum can have similar effect. More data have been collected since DfA2005. One possible explanation invokes the removal of H2O (or H+) from the AR coating. UV-bright surface features on some devices seem to resist degradation of the UV response: (still unknown) key to H2O-tight seal? Poster # 09-A (Deiries et al.) 350 nm

  14. Dietrich Baade: Optical Detector Systems at ESO Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing

  15. Wavefront Sensors for Adaptive Optics AO: Multi-conjugate Adaptive Optics Demonstrator (MAD) • 3 + 2 detector heads (e2v CCD39; 80x80 pixels) • Up to 400 fps (500 fps with 2x2 binning); RON: ~ 6-7 e- • With DSP optimization, original FIERA spec of 1 Mpix/s much exceeded • Delivered in 2007 (Roland Reiss) • ► AO enables quantitative improvements Globular Cluster NGC 6388 with 2 populations MAD@VLT + HST HST Moretti et al. (2009, A&A, 493, 539) Jupiter Globular Cluster NGC 6388

  16. Dietrich Baade: Optical Detector Systems at ESO Wavefront Sensors for Adaptive Optics@VLT: OCam and e2v CCD220/219 • e2v L3 Vision CCD220 • 240x240 pixels, up to 1500 fps • 15 systems for VLT AO Facility 2010-2012 CCD Test controller OCam developed by 3 institutes in France, in close cooperation with ESO. RON: < 1 e- (w/ gain) NGC AO head See talk by Feautrier et al. and demonstration at ESO HQ Transfer of OCam analog electronics to NGC underway. CCD See Poster # 12-B by Reyes et al.

  17. Dietrich Baade: Optical Detector Systems at ESO Wavefront Sensors for Adaptive Optics: The E-ELT Case • For 8-m class telescopes, AO is an efficiency booster. • For ELTs, AO is an enabling technology. • E-ELT: o 84x84 Shack-Hartmann lenslets, each feeding 20x20 pixels • o LARGE pixels: 20-24 μ • o Frame rate 100 – 700 Hz • o RON < 3 e- rms • Feasibility studies and pixel-design demonstrators with industry. • CMOS is the likely technology. • Released Call for Tenders for baseline device • for use with natural guide stars. For more about AO@ELTs see talk by Downing et al.

  18. Dietrich Baade: Optical Detector Systems at ESO Summary of (Optical) Detector Trends @ ESO • Complexity of design and operation increasing • Growing volume of parameter space (speed, noise, stability, etc.) • Multiple units – serial production • Much improved red QE with thicker devices • Future ESO detector systems based on NGC • Growing importance of signal sensing • CMOS technology making its way into optical astronomy Photo: Stéphane Guisard (ESO)

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