SDW 2005, TaorminaReiss et al., We Must be MAD1 We Must be MAD Pushing FIERA to its Limits Roland Reiss, Andrea Balestra, Claudio Cumani, Christoph Geimer,

Slides:



Advertisements
Similar presentations
Dealing with turbulence in MCAO Roberto Ragazzoni INAF – Padova (Italy) Alghero, Sept. 17 th 2008 Astronomy meets Metereology Dealing with turbulence in.
Advertisements

Institute for Gravitational Research
Institute for Gravitational Research
Using a DSLR to Study Variable Stars. Canon 450D - linear over a magnitude using RAW images with a specific setting.
19-24 June 2005 Philippe Feautrier - SDW Zero noise wavefront sensor development within the Opticon European network Philippe Feautrier a, Thierry.
Parameters to choose the CCD The CCD test bench *Temperature range : -55 to +40°C. *Stabilization : < 0.05°C/hour. *5 temperature probes : CCD and electronics.
Wide-Band Spice Model of the High-Speed and High-Voltage Transformers for the CCD220 Jorge Romero University of Málaga ( Javier Reyes.
IR Cloud Camera D. Burke DES Calibration Telecon May 13, 2009.
Adaptive Optics for Wavefront Correction of High Average Power Lasers Justin Mansell, Supriyo Sinha, Todd Rutherford, Eric Gustafson, Martin Fejer and.
MMT Megacam Brian McLeod Smithsonian Astrophysical Observatory.
NIR LOWFS for Keck and TMT Roger Smith & David Hale.
The Research School of Astronomy and Astrophysics of the Australian National University at Mt Stromlo Observatory is developing a wide-field Cassegrain.
PALM-3000 PALM-3000 Instrument Architecture Antonin Bouchez PALM-3000 Requirements Review November 12, 2007.
SDW20051 Vincent Lapeyrère LESIA – Observatoire de Paris Calibration of flight model CCDs for CoRoT mission.
NGAO NGS WFS design review Caltech Optical Observatories 31 st March 2010.
Keep Control: PULPO 2 ESO‘s new housekeeping unit Christoph Geimer, Claudio Cumani, Nicolas Haddad, Javier Reyes, Javier Valenzuela, Bernhard Lopez PULPO.
P3K WFS development meeting #2 V Velur Caltech Optical Observatories Pasadena, CA
LGS wavefront sensor : Type and number of sub-apertures NGAO Team Meeting #4 V. Velur Caltech Optical Observatories 01/22/2007.
High level requirements:  VLT does not see difference to FIERA/IRACE Intermediate level requirements: Huge on-the-fly data processing (infrared) Shutter/telemetry.
Detector Array Controller Based on First Light First Light PICNIC Array Mux PICNIC Array Mux Image of ESO Messenger Front Page M.Meyer June 05 NGC High.
LGS diagnostics Results (so far) Anna Moore, Hal Petrie LGS facility meeting 30 th Jan 2007.
Telescope Errors for NGAO Christopher Neyman & Ralf Flicker W. M. Keck Observatory Keck NGAO Team Meeting #4 January 22, 2007 Hualalai Conference Room,
June 2005 SDW Dedicated L3CCD for AO 1 Mark Downing, Norbert Hubin, Markus Kasper, Javier Reyes, Manfred Meyer, Dietrich Baade European Southern.
SDW2005, juin, Taormina The Corot Space instrument.
1 Activity and Motion Detection in Videos Longin Jan Latecki and Roland Miezianko, Temple University Dragoljub Pokrajac, Delaware State University Dover,
Copyright : Marconi Applied Technologies Limited. All Rights Reserved. CCDs for Adaptive Optics CfAO Workshop: Nov 1999 By P.
Eddington Kick-Off. Vienna, September 17th, 2001 T.Muñoz/C.Laviada (INTA) 1 EddiCam: The Eddington Photometric Camera Preliminary Design Layout.
SciMeasure Wavefront Sensor Cameras and their Application in the 5m Palomar Adaptive Optics System SciMeasure Analytical Systems, Inc. Ray DuVarney, Charlie.
 Johann Kolb, Norbert Hubin  Mark Downing, Olaf Iwert, Dietrich Baade Simulation results:  Richard Clare Detectors for LGS WF sensing on the E-ELT 1AO.
[1] Reference: QCam API reference manual document version Charge Coupled Device (CCD)
Bulk Silicon CCDs, Point Spread Functions, and Photon Transfer Curves: CCD Testing Activities at ESO Mark Downing, Dietrich Baade, Sebastian Deiries, (ESO/Instrumentation.
A visible-light AO system for the 4.2 m SOAR telescope A. Tokovinin, B. Gregory, H. E. Schwarz, V. Terebizh, S. Thomas.
Institute: ISE, group: PERG CCD USB 2.0 Camera for the Pi of The Sky Project Grzegorz Kasprowicz semester: T1EL-PE Cooperation with Soltan Institute for.
Position sensing in Adaptive Optics Christopher Saunter Durham University Centre for Advanced Instrumentation Durham Smart Imaging.
Our Mission Visible detectors fully matching the requirements of Adaptive Optics wavefront sensors for 10m class telescopes do not yet exist: current detectors.
Adaptive Optics Nicholas Devaney GTC project, Instituto de Astrofisica de Canarias 1. Principles 2. Multi-conjugate 3. Performance & challenges.
1 Palomar Tomograph V. Velur 1, B. Platt 2, M. Britton 1, R. Dekany 1 1 Caltech Optical Observatories, California Institute of Technology 2 Interferometry.
Performances of the COROT CCDs for high accuracy photometry Pernelle Bernardi and the CCD team From Meudon : Tristan Buey, Vincent Lapeyrere, Régis Schmidt,
NORDFORSK Summer School, La Palma, June-July 2006 NOT: Telescope and Instrumentation Michal I. Andersen & Heidi Korhonen Astrophysikalisches Institut Potsdam.
DfA2009 Optical Detector Systems at ESO (Projects completed or started since DfA2005) Dietrich Baade & Andrea Balestra, Claudio Cumani, Sebastian Deiries,
Transit Timing, Radius, Albedo, and Satellites of Extrasolar Planets with MagIC’s Upgrade Mercedes López-Morales Carnegie-DTM.
W2D1. HSV colour model Source: Primary colours Red Green Blue Secondary Cyan Magenta.
Development of CCDs for the SXI We have developed 2 different types of CCDs for the SXI in parallel.. *Advantage =>They are successfully employed for current.
FLAO_01: FLAO system baseline & goal performance F. Quirós-Pacheco, L. Busoni FLAO system external review, Florence, 30/31 March 2009.
Slicing the Universe CCDs for MUSE Roland Reiss a, Sebastian Deiries a, Jean Louis Lizon a, Manfred Meyer a, Javier Reyes a, Roland Bacon b, François Hénault.
Page 1 Adaptive Optics in the VLT and ELT era Wavefront sensors, correctors François Wildi Observatoire de Genève.
Active Optics and Wavefront Sensing at the Upgraded 6.5-meter MMT Xiaoyin Zhu Dec 12, 2012 OPTI 521 Paper Synopsis By T.E. Pickering, etc.
Dietrich Baade 1 Scientific Detectors Workshop SDW2005AD - Taormina (Sicily) June A summary: A) ESO Presentations B) Sicily C) Optical Detectors.
Optical Detector Systems at the European Southern Observatory
SDW 2013 Cabling design for a CCD231 based camera Cabling Design for a CCD231 based camera Dr. Simon Tulloch University of Sheffield.
Beam Halo Monitoring using Optical Diagnostics Hao Zhang University of Maryland/University of Liverpool/Cockcroft Institute.
SDW 2013 Theoretical Comparison of CCD Video Processors Focal-Plane electronics Roundtable.
Robo-AO Overview: System, capabilities, performance Christoph Baranec (PI)
1 Performance of a CCD tracker at room temperature T. Tsukamoto (Saga Univ.) T. Kuniya, H. Watanabe (Saga Univ.); A. Miyamoto, Y. Sugimoto (KEK); S. Takahashi,
THE CCD RIDDLE REVISTED: SIGNAL VERSUS TIME – LINEAR SIGNAL VERSUS VARIANCE – NON-LINEAR Mark Downing, Peter Sinclaire. European Southern Observatory ESO.
Date of download: 6/2/2016 Copyright © 2016 SPIE. All rights reserved. View of the XMM-Newton spacecraft subsystems, with external shrouds and structure.
SERIAL ACCEPTANCE TESTING OF 24 DETECTORS FOR „Scientific Detector Workshop“, Florence, 7 th - 11 th Oct Andreas Kelz a J.-L. Lizon b, R. Bacon c.
MagIC Upgrade for High-Speed Photometry Jim Elliot, MIT Magellan SAC
Example data of Visible lights from scintillator form a relatively small symmetric islands. 20 keV 70 keV 500 μm 500 μm.
SciMeasure Analytical Systems, Inc.
Optimisation of an EMCCD
OptiSystem-MATLAB data formats (Version 1.0)
CCD wavefront sensing system for the ESO Multi-conjugate Adaptive Optics Demonstrator (MAD) C.Cavadore, C.Cumani, The ESO-ODT team, F.Franza, E.Marchetti,
Pushing FIERA to its Limits Reiss et al., We Must be MAD
Brian McLeod Smithsonian Astrophysical Observatory
High-denisty DOT system.
The whole is… 10-FRAME PART-WHOLE EARLY NUMBER SENSE.
Christian Wolf Jean-Michel Jolion Françoise Chassaing
Optical Detector Systems at the European Southern Observatory
Table 2. Modal parameters estimated by Pulse Reflex®
Presentation transcript:

SDW 2005, TaorminaReiss et al., We Must be MAD1 We Must be MAD Pushing FIERA to its Limits Roland Reiss, Andrea Balestra, Claudio Cumani, Christoph Geimer, Javier Reyes, Enrico Marchetti, Joana Santos European Southern Observatory ( Karl-Schwarzschild-Str. 2 D Garching by Munich, Germanyhttp://

SDW 2005, TaorminaReiss et al., We Must be MAD2 We Must be MAD Pushing FIERA to its Limits MAD (Multi conjugate Adaptive optics Demonstrator) employs 5 CCDs in total 3 CCDs for Shack-Hartmann Wavefront Sensing (SHWFS) 2 CCDs for Layer-Oriented Wavefront Sensing (LOWFS)

SDW 2005, TaorminaReiss et al., We Must be MAD3 SHWFS vs. LOWFS Mode SHWFS: –3 CCDs –same frame rate –same binning factor –12 video channels (625 kpix/sec each) –window 64x64 per CCD LOWFS: –2 CCDs, –frame rate ratios of 2:1 and 4:1 –binning factors (2x2 and 4x4) –8 video channels (625 kpix/sec each) –Window 80x80 per CCD

SDW 2005, TaorminaReiss et al., We Must be MAD4 Mechanical Constraints Limited head size (96 x 68 x 30 mm 3 ) High flexibility of electrical connections required Peltier cooled CCD39- 01bi from e2v

SDW 2005, TaorminaReiss et al., We Must be MAD5 Performance (SHWFS) Frame rate 400 Hz (64 x192 pixels). Average pixel rate 4.9 Mpixel/sec. Burst pixel rate 7.5 Mpixel/sec. 400Hz approx. 6 e-RMS.