1. DfA2009 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 1 / 18Dietrich Baade: Optical Detector Systems at ESO

2. DfA2009 Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing 2 / 18Dietrich Baade: Optical Detector Systems at ESO

3. 3 / 18DfA2009 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. Dietrich Baade: Optical Detector Systems at ESO 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. DfA2009 Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing 4 / 18Dietrich Baade: Optical Detector Systems at ESO

5. DfA2009 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 5 / 18Dietrich Baade: Optical Detector Systems at ESO

6. DfA2009 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) 6 / 18Dietrich Baade: Optical Detector Systems at ESO

7. 7 / 18DfA2009 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 First unit delivered, serial production through 2011 CCD PSF ~0.8 pixels ~50,000 spectra/exposure Graded AR coating Poster # 11-B (Reiss et al.) Dietrich Baade: Optical Detector Systems at ESO

8. DfA2009 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: ~10 8 @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) 8 / 18Dietrich Baade: Optical Detector Systems at ESO

9. FORS1GiraffeUVES redVIMOS Focal reducerMedium- resolution MOS Echelle spectrographWide-angle MOS 20072009 2010 Tek 2048EB4-1 2kx2k, 24 μ e2v CCD 44-82 2kx4k, 15 μ 20 μ std silicon MIT/LL 2kx4k, 15 μ 20 μ thick e2v CCD 44-82 4x 2kx4k, 15μ 20 μ std silicon e2v CCD 44-82 2x 2kx4k, 15 μ e2v CCD 44-82 2kx4k, 15 μ 40 μ DD silicon MIT/LL 2kx4k, 15 μ 40 μ high-res. silicon e2v CCD 44-82 4x 2kx4k, 15μ 40 μ DD silicon 1.3x increase in UVB response Red response doubled; much reduced fringing R/NIR response nearly doubled; much reduced fringing Doubled R/NIR response & reduced fringing (TBC) Roland ReissMark DowningOlaf Iwert / Nicolas Haddad Nicolas Haddad / Mark Downing Dietrich Baade: Optical Detector Systems at ESO9 / 18DfA2009 Detector Upgrades of Existing Instruments Reduced fringing (additional graded AR coating - as in MUSE - is still better!) Improved red QE Standard silicon Deep-depletion silicon See also talk by Downing et al. on bulk-silicon (70 μ) CCDs

10. DfA2009 Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing 10 / 18Dietrich Baade: Optical Detector Systems at ESO

11. DfA2009 Curved Detectors Poster # 18-A (Iwert et al.) 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 Concave detectors Rogers et al.Rogers et al. 2008 11 / 18

12. DfA2009 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. Poster # 17-A (Iwert et al.) Requirements on detector stability are formidable : ~100 pm or ~1 Si atom Adam Riess 12 / 18Dietrich Baade: Optical Detector Systems at ESO

13. DfA2009 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 H 2 O (or H + ) from the AR coating. Poster # 09-A (Deiries et al.) UV-bright surface features on some devices seem to resist degradation of the UV response: (still unknown) key to H 2 O-tight seal? 350 nm 13 / 18

14. DfA2009 Controller Scientific Detector Systems R&D Projects Signal (Wavefront) Sensing 14 / 18Dietrich Baade: Optical Detector Systems at ESO

15. DfA2009 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 Jupiter Moretti et al. (2009, A&A, 493, 539) MAD@VLT + HSTHST 15 / 18 Globular Cluster NGC 6388

16. DfA2009 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 Test controller OCam developed by 3 institutes in France, in close cooperation with ESO. RON: < 1 e- (w/ gain) See talk by Feautrier et al. and demonstration at ESO HQ Transfer of OCam analog electronics to NGC underway. See Poster # 12-B by Reyes et al. CCD 16 / 18Dietrich Baade: Optical Detector Systems at ESO NGC AO head

17. 17 / 18DfA2009 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. Dietrich Baade: Optical Detector Systems at ESO

18. DfA2009 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 Growing importance of signal sensing CMOS technology making its way into optical astronomy CMOS technology making its way into optical astronomy Photo: Stéphane Guisard (ESO) 18 / 18