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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20111102T000000
DTEND;TZID=Atlantic/Canary:20111102T010000
UID:iactalks-316
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/316
CREATED:2011-11-02T00:00:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:A decadal survey of AO wavefront sensing detector developments in E
 urope, the OCAM revolution 
DESCRIPTION:A decadal survey of AO wavefront sensing detector developments 
 in Europe, the OCAM revolution \nDr. Philippe Feautrier\n\nThe success of 
 the next generation of instruments for 8 to 40-m class telescopes will dep
 end on the ability of Adaptive Optics (AO) systems to provide excellent im
 age quality and stability. This will be achieved by increasing the samplin
 g, wavelength range and correction quality of the wave front error in both
  spatial and time domains.  The modern generation of AO wavefront sensor d
 etectors started in the late nineties with the development of the CCD50 de
 tector by e2v under ESO contract for the ESO NAOS AO system. With a 128x12
 8 pixels format, this 8 outputs CCD runs at a 500 Hz frame rate with a rea
 dout noise of 7e-. A major breakthrough has been achieved with the recent 
 development of the CCD220, also by e2v technologies. This 240x240 pixels 8
  outputs EMCCD (CCD with internal multiplication) has been jointly funded 
 by ESO and Europe under the FP6 programme. The CCD220 detector and the OCA
 M2 camera are now the most sensitive system in the world for advanced adap
 tive optics systems, offering an astonishing <0.2 e readout noise at a 
 frame rate of 1500 Hz with negligible dark current. Extremely easy to oper
 ate, OCAM2 only needs a 24 V power supply and a modest water cooling circu
 it. This system will be extensively described in this talk. An upgrade of 
 OCAM2 is foreseen to boost its frame rate to 2500 Hz, opening the window o
 f XAO wavefront sensing for the ELT.   Since this major success, new devel
 opments started in Europe. One is fully dedicated to Laser Guide Star AO f
 or the ELT with an ESO involvment. The spot elongation from a LGS SH wavef
 ront sensor induces an increase of the pixel format. Two detectors are cur
 rently developed by e2v. The NGSD will be a 672x672 pixels CMOS detector w
 ith a readout noise of 4e (goal 1e) at 700 Hz frame rate. The LGSD is a sc
 aling of the NGSD with 1680x1680 pixels and 3 e readout noise (goal 1e) at
  700 Hz frame rate. New technologies will be developed for that purpose: n
 ew CMOS pixel architecture, CMOS back thinned and back illuminated device,
  full digital outputs. In addition, the CMOS technology is extremely robus
 t in a telescope environment. Both detectors will be used on the ELT, depe
 nding on the AO system considered.  Additional developments also started f
 or wavefront sensing in the infrared based on new breakthrough using ultra
  low noise Avalanche Photodiode (APD) arrays within the RAPID project. The
  latter should offer a 320x240 8 outputs 30 microns IR array, sensitive fr
 om 0.4 to 3.2 microns, with 2 e readout noise at 1500 Hz frame rate. First
  results of this project will be showed.
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