SDW 2017 – MICADO for the ELT Baltimore, September 26th 2017

Slides:

Advertisements

Similar presentations

Max-Planck-Institut fuer extr. Physik, Garching, Germany Physics Dept, Univ. of Oxford, UK.

Advertisements

TheEuropean Extremely Large Telescope. The E-ELT 40-m class telescope: largest optical- infrared telescope in the world. Segmented primary mirror. Active.

Sarah Kendrew Leiden Instrumentation Group.  One of eight potential instruments for the European ELT, the largest planned optical/IR telescope for the.

HIRES Technical concept and design E. Oliva, HIRES meeting, Brera (Milan, Italy)1.

Sodium monitoring experiment in Chile Céline d’Orgeville.

SOME COMMENTS ABOUT THE GIANT CHINESE SOLAR TELESCOPE CONCEPT JACQUES M. BECKERS Beijing August 6 – 8, 2011.

Extragalactic AO Science James Larkin AOWG Strategic Planning Meeting September 19, 2004.

Jeff B. Pelz Visual Perception Laboratory Carlson Center for Imaging Science Rochester Institute of Technology Using Eyetracking to Improve Image Composition.

Adaptive Optics and Optical Interferometry or How I Learned to Stop Worrying and Love the Atmosphere Brian Kern Observational Astronomy 10/25/00.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Instrumentation Concepts Ground-based Optical Telescopes Keith Taylor (IAG/USP) Aug-Nov, 2008 Aug-Sep, 2008 IAG-USP.

CAMERA A Compact, Automated MEMs-based Rayleigh Adaptive Optics System Matthew Britton, Nick Law, Viswa Velur, Christoph Baranec.

AURA New Initiatives Office S.C. Barden, M. Liang, K.H. Hinkle, C.F.W. Harmer, R.R. Joyce (NOAO/NIO) September 17, 2001 Instrumentation Concepts for the.

Widening the Scope of Adaptive Optics Matthew Britton.

ASTRO 2233 Fall 2010 Adaptive Optics, Interferometry and Planet Detection Lecture 16 Thursday October 21, 2010.

California Association for Research in Astronomy W. M. Keck Observatory KPAO Keck Precision Adaptive Optics Keck Precision AO (KPAO) SSC Presentation January.

A Short Presentation of Ongoing AO Work at Lund Observatory Mette Owner-Petersen Lund Observatory Workshop for “Forskarskolen i Rymdteknik” Gothenburg.

1 Atmospheric Limits to Precision William van Altena Yale University Basic Astrometric Methods Yale University July 18-22, 2005.

E UROPEAN E XTREMELY L ARGE T ELESCOPE Aprajita Verma University of Oxford With thanks to UK E-ELT Project Team & E-ELT Team at ESO.

Galaxies. Our Galaxy (CP Fig 19.1a) Our Galaxy (CP Fig 19.1b)

IRIS Telescope Camera Kimberly Bott Institute for Astronomy Mentor: Klaus Hodapp Home Institution: University of Hawaii at Hilo 2008 Center for Adaptive.

1 ELT Instrumentation Development Mark Casali ELT Instrumentation Development Mark Casali.

Adaptive Optics in the VLT and ELT era

T-REX OU4 HIRES The high resolution spectrograph for E-ELT E. Oliva, T-REX meeting, Sexten Pustertal (I)1.

Big Bear Solar Observatory NST Main Features  All reflecting, off-axis Gregory optical configuration  PM: 1.6 m clear aperture with f/2.4  Figuring.

A visible-light AO system for the 4.2 m SOAR telescope A. Tokovinin, B. Gregory, H. E. Schwarz, V. Terebizh, S. Thomas.

STATUS REPORT OF FPC SPICA Task Force Meeting March 29, 2010 MATSUMOTO, Toshio (SNU)

OWL Instrument Concept Studies Within the OWL Conceptual Design to be completed by ESO in 3Q 2005, ESO collaborates with external institutes in the study.

The Atacama Cosmology Telescope New Views of the Universe December 11, 2005 Joe Fowler Princeton University.

SOFIA Observatory Overview and Specifications Last Updated –

Circular aperture Rectangular aperture Fraunhofer Diffraction.

Adaptive Optics Nicholas Devaney GTC project, Instituto de Astrofisica de Canarias 1. Principles 2. Multi-conjugate 3. Performance & challenges.

“Twinkle, Twinkle Little Star”: An Introduction to Adaptive Optics Mt. Hamilton Visitor’s Night July 28, 2001.

AO for ELT – Paris, June 2009 MAORY Multi conjugate Adaptive Optics RelaY for the E-ELT Emiliano Diolaiti (INAF–Osservatorio Astronomico di Bologna)

European Extremely Large Telescope - Status April ESO.

Extremely Large Telescope and its AO systems

Viewing the Universe through distorted lenses: Adaptive optics in astronomy Steven Beckwith Space Telescope Science Institute & JHU.

Searching for Brown Dwarf Companions to Nearby Stars Michael W. McElwain, James E. Larkin & Adam J. Burgasser (UC Los Angeles) Background on Brown Dwarfs.

Observing Venus (and Mars) with Adaptive Optics

Conference “Feeding the Giants: ELTs in the era of Surveys” -- Ischia 31/08/2011 Large field of view and ELTs: an impossible marriage? Paolo Ciliegi (INAF.

Ground Layer AO at ESO’s VLT Claire Max Interim Director UC Observatories September 14, 2014.

KMOS Instrument Overview & Data Processing Richard Davies Max Planck Institute for Extraterrestrial Physics  What does KMOS do?  When will it do it?

LINC-NIRVANAW. Gaessler 03/10/2006 LINC-NIRVANA Wolfgang Gaessler J. Berwein, F. Briegel, F. Kittmann, A. Pavlov, C. Storz MPIA (Germany),

NEWFIRM: the NOAO Extremely Wide Field IR Imager Presented by Ron Probst, Project Scientist.

The Far-Infrared Universe: from the Universe’s oldest light to the birth of its youngest stars Jeremy P. Scott, on behalf of Locke D. Spencer Physics and.

Adaptive Optics for Astronomy Kathy Cooksey. AO Basics Photons –Travel in straight lines Wavefront –Line perpendicular to all photons’ paths Atmospheric.

Telescopes Refractors and Reflectors Various Designs Important Properties Modern Advances Beyond Visible Light Refractors and Reflectors Various Designs.

Keck Observatory Overview Peter Wizinowich W. M. Keck Observatory AOSC May 31, 2004.

Page 1 Adaptive Optics in the VLT and ELT era basics of AO Neptune François Wildi Observatoire de Genève Credit for most slides : Claire Max (UC Santa.

Why Mauna Kea?. Mauna Kea, Hawaii Mauna Kea 13,824 ft.

PHYS 221 Recitation Kevin Ralphs Week 11. Overview HW Questions Diffraction Interference.

Robo-AO Overview: System, capabilities, performance Christoph Baranec (PI)

Theme 2 AO for Extremely Large Telescopes Center for Adaptive Optics.

Page 1 Adaptive Optics in the VLT and ELT era François Wildi Observatoire de Genève Credit for most slides : Claire Max (UC Santa Cruz) Basics of AO.

Double the slit width a and double the wavelength

MSc-Student Activities at ESO

Jeffrey R. Regester Physics Department High Point University

Focal Plane Instrumentation at Big Bear Solar Observatory

Observing brown dwarfs in the E-ELT era

Pyramid sensors for AO and co-phasing

From: Binocular visual acuity for the correction of spherical aberration in polychromatic and monochromatic light Journal of Vision. 2014;14(2):8. doi: /

Photon counting CCDs as wavefront sensors for LBT A.O. systems

Adaptive optics Now: Soon: High angular resolution

System Overview CHRISS Combined High-Resolution Imaging and Spectroscopy System Intelligent Systems Group – University of Duisburg-Essen, Germany.

الإشعاع الكهرومغناطيسي ووسائل الاستشعار عن بعد

Theme 2 AO for Extremely Large Telescopes

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,

Example: 633 nm laser light is passed through a narrow slit and a diffraction pattern is observed on a screen 6.0 m away. The distance on the screen.

MFM setup. MFM setup. The excitation lasers are combined in a fiber through an acousto-optic tunable filter, collimated, reflected on a dichroic mirror.

Theme 2 AO for Extremely Large Telescopes

Theme 2 AO for Extremely Large Telescopes

Presentation transcript:

SDW 2017 – MICADO for the ELT Baltimore, September 26th 2017 Christopher Mandla Max Planck Institute for Extraterrestrial Physics, Germany On behalf of the MICADO Consortium

SDW 2017, Baltimore, September 26th 2017 MICADO Overview MICADO (Multi-AO Imaging Camera for Deep Observations) First Light imager/spectograph at ELT Near Infrared (0.8-2.4µm) Diffraction limited imaging Optimised for laser guide star multi-conjugate adaptive optics module (MCAO) Stand-alone function with single-conjugate adaptive optics (SCAO) by using a single natural guide star First Light date: 2024 Spectral Resolution: R~ 8000 across slit R~ 15000 for point sources ELT location Cerro Armazones Atacama Desert Chile SDW 2017, Baltimore, September 26th 2017