Robo-AO: Robotic Laser Guide Star Adaptive Optics on the Palomar 60 in Christoph Baranec (PI) & Nick Law (PS)
|
|
|
- Quentin Crawford
- 6 years ago
- Views:
Transcription
1 Robo-AO: Robotic Laser Guide Star Adaptive Optics on the Palomar 60 in 2011 Christoph Baranec (PI) & Nick Law (PS)
2 Why Robo-AO? Robotic high efficiency observing Adaptive Optics spatial resolution set by D Laser Guide Star high sky coverage Small Telescopes lots of available time
3 Robo-AO at the P60
4 Robo-AO in the lab
5 Vision Designing the system to be affordable and portable to 1-3 m class telescopes Demonstrate Robo-AO at P60 Inter-University Centre for Astronomy and Astrophysics 2 m Girawali Observatory Clone and deploy Robo-AO around the world
6 Robo-AO General AO facility + unique capabilities
7 AO capabilities Diffraction-limited resolution 0.5+ Strehl in the NIR ~1 field of view General imaging range of filters, exposure times, observation setups
8 What s unique? Large surveys High efficiency Continual availability Great sky coverage Visible-light & high speed imaging
9 Large Surveys Overhead ~70 seconds per target So, with 2 mins integration time, ~150 targets per night 4200 targets in 4 weeks -- actually possible on a 2m-class telescope!
10 Survey Programs - Binarity all spectral types, companions down to brown dwarfs for most cover range of stellar parameter space with one instrument and one coherent survey
11 Very high contrast? 3 planets around HR 8799 Image taken with 1.5m portion of P200 w. PALMAO Vortex coronagraph for high-contrast imaging Serabyn et al. 2010
12 Survey Programs - Lensed Quasars Cover all quasars above a mag. limit Search for multiple images Model lenses for galaxy mass distribution (in a very large sample) Follow up for time delays
13 Sky coverage All targets brighter than V=17 30% sky coverage at diffraction-limited resolution 100% sky coverage in no-tip/tilt mode
14 Monitoring Trent Dupuy 2008, 2009
15 SNR Improvements B and S NR Compared to 1.5 m S NR Compared to 4 m FWHM (1 is typical) S trehl J 2.9X 0.4X % H 7.1X 0.98X % Astrometric precision gains in both SNR and FWHM Prediction: 100uas precision in around 15 mins (based on Cameron et al. Keck & Palomar performance)
16 High availability programs New SDSS Old Subtraction The Palomar Transient Factory finds 1 transient candidate every ~10 minutes Many found near galactic nuclei - how do we separate them?
17
18 High-speed, high-resolution imaging
19 High-speed, high-resolution imaging
20 Robo-AO as part of the community ROBO-AO
21 Robo-AO as part of the community ROBO-AO ROBO-AO ROBO-AO ROBO-AO ROBO-AO ROBO-AO
22 Robo-AO Science Workshop Please come to the Robo-AO science workshop on Thursday afternoon! Details online and at end of talk
23 Building Robo-AO Laser guide star Adaptive optics system Science instruments Robotic control software Robotic telescope
24 Laser guide star Rayleigh LGS (e.g. Starfire, Mt. Wilson, MMT, WHT, SOAR, LBT?) Range gated 650 m at 10 km m V ~9 Less FA on small telescopes x10 more economical per W than Sodium
25 Laser beam projector Compact modular projector Optional periscope assembly UV Class 1 w.r.t. aircraft; no human spotters
26 Robo-AO adaptive optics
27 AO Wavefront sensors Shack-Hartmann 11 x 11 subapertures E2V CCD39 2kHz at 4.5 e- Image motion (tip/tilt) From science instruments
28 AO Wavefront reconstructor Lightweight, fast Linux/C++ software Capable of >3kHz Running at 1.2 khz Fully reconfigurable via user editable files Custom reconstructor matrices Adjustable loop parameters (gains, offsets, flat positions, etc.)
29 AO Wavefront correctors Micro-Electro-Mechanical Systems deformable mirror 12 x 12 actuators 3.5 μm stroke Piezo fast steering mirror USB electronics 8 khz (IUCAA developed drivers)
30 Robo-AO in action
31 Visible science instrument Andor ixon EM + DU-888 Electron Multiplying CCD 44 x 44 square FoV pixels (Nyquist at λ = 620 nm) Full frame rate: 9 Hz Sub frame rate: ~200 Hz
32 NIR science instrument InGaAs (Xenics: Xeva) + Affordable, readily available - Noisy, small format HgCdTe (Teledyne: H2RG) + 2 FoV, pixels (Nyquist at λ = 900 nm) + Excellent noise, flexible readout - Cost, development time Xeva JWST Fine Guidance Sensor H2RG
33 Robotic control software Fully robotic control system Subsystems work as daemons Supervisor controls scheduling, operations Watchdog processes Programming intelligence is a challenge Error control and exception handling Safety system for equipment Laser safety a priority
34 Palomar Observatory's P60 Upgraded to robotic operation in 2004 Part of Palomar Transient Factory providing primary rapid follow up observation with standard CCD camera Perfect platform for Robo-AO
35 Progress to date Lab AO system at 1.2 khz Laser system designed, fabrication in progress, under full computer control Optimized WFS camera Visible camera integrating tip/tilt control Currently reviewing optical design of Cassegrain instrument
36 Schedule On-sky laser test at P60 in August Full system test in January 2011 Likely science demo period in Spring 2011
37 Upcoming Science Workshop Many new discoveries await with Robo-AO Encourage participation bring your ideas! Guided lab tour Thursday 12:30pm-5pm
38 Acknowledgements
Robo-AO: The first autonomous laser guide star adaptive optics system for 1 to 3 meter telescopes
Robo-AO: The first autonomous laser guide star adaptive optics system for 1 to 3 meter telescopes Reed L. Riddle for the Robo-AO Team Telescopes from Afar March 1, 2011 The Robo-AO Team California Institute
Putting the Robo in Robo-AO
Putting the Robo in Robo-AO Reed L. Riddle for the Robo-AO Team Workshop on Astronomy with Adaptive Optics on Moderate Sized Telescopes IUCAA, Pune, India August 23, 2011 The Robo-AO Team California Institute
Adaptive Optics Lectures
Adaptive Optics Lectures Andrei Tokovinin 3. SOAR Adaptive Module (SAM) SAM web pages: SOAR--> SAM http://www.ctio.noao.edu/new/telescopes/soar/instruments/sam/ Paper (2016, PASP, 128, 125003): http://www.ctio.noao.edu/~atokovin/papers/sam-pasp.pdf
Adaptive Optics lectures
Adaptive Optics lectures 2. Adaptive optics Invented in 1953 by H.Babcock Andrei Tokovinin 1 Plan General idea (open/closed loop) Wave-front sensing, its limitations Correctors (DMs) Control (spatial and
Adaptive Optics for LIGO
Adaptive Optics for LIGO Justin Mansell Ginzton Laboratory LIGO-G990022-39-M Motivation Wavefront Sensor Outline Characterization Enhancements Modeling Projections Adaptive Optics Results Effects of Thermal
GPI INSTRUMENT PAGES
GPI INSTRUMENT PAGES This document presents a snapshot of the GPI Instrument web pages as of the date of the call for letters of intent. Please consult the GPI web pages themselves for up to the minute
MAORY E-ELT MCAO module project overview
MAORY E-ELT MCAO module project overview Emiliano Diolaiti Istituto Nazionale di Astrofisica Osservatorio Astronomico di Bologna On behalf of the MAORY Consortium AO4ELT3, Firenze, 27-31 May 2013 MAORY
Gemini 8m Telescopes Instrument Science Requirements. R. McGonegal Controls Group. January 27, 1996
GEMINI 8-M Telescopes Project Gemini 8m Telescopes Instrument Science Requirements R. McGonegal Controls Group January 27, 1996 GEMINI PROJECT OFFICE 950 N. Cherry Ave. Tucson, Arizona 85719 Phone: (520)
GMT Instruments and AO. GMT Science Meeting - March
GMT Instruments and AO GMT Science Meeting - March 2008 1 Instrument Status Scientific priorities have been defined Emphasis on: Wide-field survey science (cosmology) High resolution spectroscopy (abundances,
Proposed Adaptive Optics system for Vainu Bappu Telescope
Proposed Adaptive Optics system for Vainu Bappu Telescope Essential requirements of an adaptive optics system Adaptive Optics is a real time wave front error measurement and correction system The essential
MODULAR ADAPTIVE OPTICS TESTBED FOR THE NPOI
MODULAR ADAPTIVE OPTICS TESTBED FOR THE NPOI Jonathan R. Andrews, Ty Martinez, Christopher C. Wilcox, Sergio R. Restaino Naval Research Laboratory, Remote Sensing Division, Code 7216, 4555 Overlook Ave
Robo-AO Network. Reed L. Riddle. Workshop on Astronomy with Adaptive Optics on Moderate Sized Telescopes IUCAA, Pune, India August 24, 2011
Robo-AO Network Reed L. Riddle Workshop on Astronomy with Adaptive Optics on Moderate Sized Telescopes IUCAA, Pune, India August 24, 2011 Collaborative groups Can only do science Astronomy Networks - With
Modeling the multi-conjugate adaptive optics system of the E-ELT. Laura Schreiber Carmelo Arcidiacono Giovanni Bregoli
Modeling the multi-conjugate adaptive optics system of the E-ELT Laura Schreiber Carmelo Arcidiacono Giovanni Bregoli MAORY E-ELT Multi Conjugate Adaptive Optics Relay Wavefront sensing based on 6 (4)
DESIGNING AND IMPLEMENTING AN ADAPTIVE OPTICS SYSTEM FOR THE UH HOKU KE`A OBSERVATORY ABSTRACT
DESIGNING AND IMPLEMENTING AN ADAPTIVE OPTICS SYSTEM FOR THE UH HOKU KE`A OBSERVATORY University of Hawai`i at Hilo Alex Hedglen ABSTRACT The presented project is to implement a small adaptive optics system
Wavefront Sensing In Other Disciplines. 15 February 2003 Jerry Nelson, UCSC Wavefront Congress
Wavefront Sensing In Other Disciplines 15 February 2003 Jerry Nelson, UCSC Wavefront Congress QuickTime and a Photo - JPEG decompressor are needed to see this picture. 15feb03 Nelson wavefront sensing
Development of a Low-order Adaptive Optics System at Udaipur Solar Observatory
J. Astrophys. Astr. (2008) 29, 353 357 Development of a Low-order Adaptive Optics System at Udaipur Solar Observatory A. R. Bayanna, B. Kumar, R. E. Louis, P. Venkatakrishnan & S. K. Mathew Udaipur Solar
GROUND LAYER ADAPTIVE OPTICS AND ADVANCEMENTS IN LASER TOMOGRAPHY AT THE 6.5M MMT TELESCOPE
GROUND LAYER ADAPTIVE OPTICS AND ADVANCEMENTS IN LASER TOMOGRAPHY AT THE 6.5M MMT TELESCOPE E. Bendek 1,a, M. Hart 1, K. Powell 2, V. Vaitheeswaran 1, D. McCarthy 1, C. Kulesa 1. 1 University of Arizona,
PhD Defense. Low-order wavefront control and calibration for phase-mask coronagraphs. Garima Singh
PhD Defense 21st September 2015 Space Telescope Science Institute, Baltimore on Low-order wavefront control and calibration for phase-mask coronagraphs by Garima Singh PhD student and SCExAO member Observatoire
Subject headings: turbulence -- atmospheric effects --techniques: interferometric -- techniques: image processing
Direct 75 Milliarcsecond Images from the Multiple Mirror Telescope with Adaptive Optics M. Lloyd-Hart, R. Dekany, B. McLeod, D. Wittman, D. Colucci, D. McCarthy, and R. Angel Steward Observatory, University
Ultra-Flat Tip-Tilt-Piston MEMS Deformable Mirror
Ultra-Flat Tip-Tilt-Piston MEMS Deformable Mirror Mirror Technology Days June 16 th, 2009 Jason Stewart Steven Cornelissen Paul Bierden Boston Micromachines Corp. Thomas Bifano Boston University Mirror
MAORY ADAPTIVE OPTICS
MAORY ADAPTIVE OPTICS Laura Schreiber, Carmelo Arcidiacono, Giovanni Bregoli, Fausto Cortecchia, Giuseppe Cosentino (DiFA), Emiliano Diolaiti, Italo Foppiani, Matteo Lombini, Mauro Patti (DiFA-OABO) MAORY
Wavefront sensor design for NGAO: Assumptions, Design Parameters and Technical Challenges Version 0.1
Wavefront sensor design for NGAO: Assumptions, Design Parameters and Technical Challenges Version 0.1 V. Velur Caltech Optical Observatories M/S 105-24, 1200 E California Blvd., Pasadena, CA 91125 Sept.
1. INTRODUCTION ABSTRACT
Acquisition and Dithering with the TMT IRIS On-Instrument Wavefront Sensor System David R. Andersen* a, Jennifer Dunn a, James Larkin b, Shelley Wright c, Eric Chisholm d, Jenny Atwood a, Edward Chapin
CHARA AO Calibration Process
CHARA AO Calibration Process Judit Sturmann CHARA AO Project Overview Phase I. Under way WFS on telescopes used as tip-tilt detector Phase II. Not yet funded WFS and large DM in place of M4 on telescopes
Bruce Macintosh for the GPI team Presented at the Spirit of Lyot conference June 7, 2007
This work was performed under the auspices of the U.S. Department of Energy by University of California, Lawrence Livermore National Laboratory under Contract W-7405-Eng-48. Bruce Macintosh for the GPI
Segmented deformable mirrors for Ground layer Adaptive Optics
Segmented deformable mirrors for Ground layer Adaptive Optics Edward Kibblewhite, University of Chicago Adaptive Photonics LLC Ground Layer AO Shack Hartmann Images of 5 guide stars in Steward Observatory
Infrared detectors for wavefront sensing
Infrared detectors for wavefront sensing Jean-Luc Gach et al. The project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 673944 First
Puntino. Shack-Hartmann wavefront sensor for optimizing telescopes. The software people for optics
Puntino Shack-Hartmann wavefront sensor for optimizing telescopes 1 1. Optimize telescope performance with a powerful set of tools A finely tuned telescope is the key to obtaining deep, high-quality astronomical
Designing Adaptive Optics Systems
Designing Adaptive Optics Systems Donald Gavel UCO/Lick Observatory Laboratory for Adaptive Optics Designing Adaptive Optics Systems Outline The design process AO systems taxonomy Commonalities and differences
The Extreme Adaptive Optics test bench at CRAL
The Extreme Adaptive Optics test bench at CRAL Maud Langlois, Magali Loupias, Christian Delacroix, E. Thiébaut, M. Tallon, Louisa Adjali, A. Jarno 1 XAO challenges Strehl: 0.7
Simultaneous Infrared-Visible Imager/Spectrograph a Multi-Purpose Instrument for the Magdalena Ridge Observatory 2.4-m Telescope
Simultaneous Infrared-Visible Imager/Spectrograph a Multi-Purpose Instrument for the Magdalena Ridge Observatory 2.4-m Telescope M.B. Vincent *, E.V. Ryan Magdalena Ridge Observatory, New Mexico Institute
Effect of segmented telescope phasing errors on adaptive optics performance
Effect of segmented telescope phasing errors on adaptive optics performance Marcos van Dam Flat Wavefronts Sam Ragland & Peter Wizinowich W.M. Keck Observatory Motivation Keck II AO / NIRC2 K-band Strehl
OWL Phase A Review - Garching - 2 nd to 4 th Nov Adaptive Optics. (Presented by N. Hubin) European Southern Observatory
OWL Phase A Review - Garching - 2 nd to 4 th Nov 2005 Adaptive Optics (Presented by N. Hubin) 1 Overview Adaptive Optics concepts and performances Single Conjugate Adaptive Optics (SCAO) Ground Layer Adaptive
Performance of Keck Adaptive Optics with Sodium Laser Guide Stars
4 Performance of Keck Adaptive Optics with Sodium Laser Guide Stars L D. T. Gavel S. Olivier J. Brase This paper was prepared for submittal to the 996 Adaptive Optics Topical Meeting Maui, Hawaii July
Calibration of AO Systems
Calibration of AO Systems Application to NAOS-CONICA and future «Planet Finder» systems T. Fusco, A. Blanc, G. Rousset Workshop Pueo Nu, may 2003 Département d Optique Théorique et Appliquée ONERA, Châtillon
Capabilities of SST* and CHROMIS
Capabilities of SST* and CHROMIS Göran Scharmer Institute for Solar Physics Stockholm University *Swedish 1-m Solar Telescope Hinode 9, Belfast, 16 September 2015 Strengths of SST Outstanding image quality
Electron Multiplying Charge Coupled Devices. Craig Mackay, Institute of Astronomy, University of Cambridge.
Electron Multiplying Charge Coupled Devices Craig Mackay, Institute of Astronomy, University of Cambridge. Outline Introduction to EMCCDs: General Characteristics Applications of EMCCDs: Current and Potential
A Ground-based Sensor to Detect GEOs Without the Use of a Laser Guide-star
A Ground-based Sensor to Detect GEOs Without the Use of a Laser Guide-star Mala Mateen Air Force Research Laboratory, Kirtland AFB, NM, 87117 Olivier Guyon Subaru Telescope, Hilo, HI, 96720 Michael Hart,
AVOIDING TO TRADE SENSITIVITY FOR LINEARITY IN A REAL WORLD WFS
Florence, Italy. Adaptive May 2013 Optics for Extremely Large Telescopes III ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13259 AVOIDING TO TRADE SENSITIVITY FOR LINEARITY IN A REAL WORLD WFS D. Greggio
OPTINO. SpotOptics VERSATILE WAVEFRONT SENSOR O P T I N O
Spotptics he software people for optics VERSALE WAVEFR SESR Accurate metrology in single and double pass Lenses, mirrors and laser beams Any focal length and diameter Large dynamic range Adaptable for
SHARK-NIR overview and optomechanical design: an update
SHARK-NIR overview and optomechanical design: an update Davide Greggio The SHARK-NIR Team: J.Farinato 1, F.Pedichini 2, E.Pinna 3, C.Baffa 3, A.Baruffolo 1, M.Bergomi 1, A.Bianco 8, L.Carbonaro 3, E.Carolo
The Wavefront Control System for the Keck Telescope
UCRL-JC-130919 PREPRINT The Wavefront Control System for the Keck Telescope J.M. Brase J. An K. Avicola B.V. Beeman D.T. Gavel R. Hurd B. Johnston H. Jones T. Kuklo C.E. Max S.S. Olivier K.E. Waltjen J.
a simple optical imager
Imagers and Imaging a simple optical imager Here s one on our 61-Inch Telescope Here s one on our 61-Inch Telescope filter wheel in here dewar preamplifier However, to get a large field we cannot afford
Open-loop performance of a high dynamic range reflective wavefront sensor
Open-loop performance of a high dynamic range reflective wavefront sensor Jonathan R. Andrews 1, Scott W. Teare 2, Sergio R. Restaino 1, David Wick 3, Christopher C. Wilcox 1, Ty Martinez 1 Abstract: Sandia
What is the source of straylight in SST/CRISP data?
What is the source of straylight in SST/CRISP data? G.B. Scharmer* with Mats Löfdahl, Dan Kiselman, Marco Stangalini Based on: Scharmer et al., A&A 521, A68 (2010) Löfdahl & Scharmer, A&A 537, A80 (2012)
ABSTRACT 1. INTRODUCTION
Tracking the sodium layer altitude with GeMS in the era of NGS2 Eduardo Marin* a, Gaetano Sivo a, Vincent Garrel b, Pedro Gigoux a, Cristian Moreno a, Marcos van Dam c, Brian Chinn a, Paul Hisrt d, Vanessa
Integrated Micro Machines Inc.
Integrated Micro Machines Inc. Segmented Galvanometer-Driven Deformable Mirrors Keith O Hara The segmented mirror array developed for an optical cross connect Requirements for the cross-connect Requirements
The First Light of the Subaru Laser Guide Star Adaptive Optics System
The First Light of the Subaru Laser Guide Star Adaptive Optics System Hideki Takami Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, Hawaii, USA 96720 Stephen
Science Detectors for E-ELT Instruments. Mark Casali
Science Detectors for E-ELT Instruments Mark Casali 1 The Telescope Nasmyth telescope with a segmented primary mirror. Novel 5 mirror design to include adaptive optics in the telescope. Classical 3mirror
MAORY for E-ELT. Emiliano Diolaiti (INAF Osservatorio Astronomico di Bologna) On behalf of the MAORY Consortium
MAORY for E-ELT Emiliano Diolaiti (INAF Osservatorio Astronomico di Bologna) On behalf of the MAORY Consortium Strumentazione per telescopi da 8m e E-ELT INAF, Roma, 5 Febbraio 2008 Multi Conjugate Adaptive
Pablo Artal. Adaptive Optics visual simulator ( and depth of focus) LABORATORIO DE OPTICA UNIVERSIDAD DE MURCIA, SPAIN
Adaptive Optics visual simulator ( and depth of focus) Pablo Artal LABORATORIO DE OPTICA UNIVERSIDAD DE MURCIA, SPAIN 8th International Wavefront Congress, Santa Fe, USA, February New LO UM building! Diego
SONG Stellar Observations Network Group. The prototype
SONG Stellar Observations Network Group The prototype F. Grundahl1, J. Christensen Dalsgaard1, U. G. Jørgensen2, H. Kjeldsen1,S. Frandsen1 and P. Kjærgaard2 1) Danish AsteroSeismology Centre, University
Non-adaptive Wavefront Control
OWL Phase A Review - Garching - 2 nd to 4 th Nov 2005 Non-adaptive Wavefront Control (Presented by L. Noethe) 1 Specific problems in ELTs and OWL Concentrate on problems which are specific for ELTs and,
A NEW SODIUM GUIDESTAR ADAPTIVE OPTICS SYSTEM FOR THE STARFIRE OPTICAL RANGE 3.5 m TELESCOPE: POST PRINT
AFRL-RD-PS TP-2009-1018 AFRL-RD-PS TP-2009-1018 A NEW SODIUM GUIDESTAR ADAPTIVE OPTICS SYSTEM FOR THE STARFIRE OPTICAL RANGE 3.5 m TELESCOPE: POST PRINT Robert Johnson, et al. The Boeing Company PO Box
Wavefront control for highcontrast
Wavefront control for highcontrast imaging Lisa A. Poyneer In the Spirit of Bernard Lyot: The direct detection of planets and circumstellar disks in the 21st century. Berkeley, CA, June 6, 2007 p Gemini
Raven a scientific and technical Multi-Object Adaptive Optics (MOAO) demonstrator
Raven a scientific and technical Multi-Object Adaptive Optics (MOAO) demonstrator Olivier Lardière, Célia Blain, Colin Bradley, Reston Nash, Darryl Gamroth, Kate Jackson, Dave Andersen, Shin Oya, Yoshito
Status of the DKIST Solar Adaptive Optics System
Status of the DKIST Solar Adaptive Optics System Luke Johnson Keith Cummings Mark Drobilek Erik Johannson Jose Marino Kit Richards Thomas Rimmele Predrag Sekulic Friedrich Wöger AO4ELT Conference June
TIRCAM2 (TIFR Near Infrared Imaging Camera - 3.6m Devasthal Optical Telescope (DOT)
TIRCAM2 (TIFR Near Infrared Imaging Camera - II) @ 3.6m Devasthal Optical Telescope (DOT) (ver 4.0 June 2017) TIRCAM2 (TIFR Near Infrared Imaging Camera - II) is a closed cycle cooled imager that has been
High contrast imaging lab
High contrast imaging lab Ay122a, November 2016, D. Mawet Introduction This lab is an introduction to high contrast imaging, and in particular coronagraphy and its interaction with adaptive optics sytems.
MALA MATEEN. 1. Abstract
IMPROVING THE SENSITIVITY OF ASTRONOMICAL CURVATURE WAVEFRONT SENSOR USING DUAL-STROKE CURVATURE: A SYNOPSIS MALA MATEEN 1. Abstract Below I present a synopsis of the paper: Improving the Sensitivity of
Ultralight Weight Optical Systems using Nano-Layered Synthesized Materials
Ultralight Weight Optical Systems using Nano-Layered Synthesized Materials Natalie Clark, PhD NASA Langley Research Center and James Breckinridge University of Arizona, College of Optical Sciences Overview
Focal Plane and non-linear Curvature Wavefront Sensing for High Contrast Coronagraphic Adaptive Optics Imaging
Focal Plane and non-linear Curvature Wavefront Sensing for High Contrast Coronagraphic Adaptive Optics Imaging Olivier Guyon Subaru Telescope 640 N. A'ohoku Pl. Hilo, HI 96720 USA Abstract Wavefronts can
A new Infra-Red Camera for COAST. Richard Neill - PhD student Supervisor: Dr John Young
A new Infra-Red Camera for COAST Richard Neill - PhD student Supervisor: Dr John Young The Cambridge Optical Aperture-Synthesis Telescope: COAST is a
The Imaging Chain in Optical Astronomy
The Imaging Chain in Optical Astronomy 1 Review and Overview Imaging Chain includes these elements: 1. energy source 2. object 3. collector 4. detector (or sensor) 5. processor 6. display 7. analysis 8.
The Imaging Chain in Optical Astronomy
The Imaging Chain in Optical Astronomy Review and Overview Imaging Chain includes these elements: 1. energy source 2. object 3. collector 4. detector (or sensor) 5. processor 6. display 7. analysis 8.
A Quadrant-CCD star tracker
A Quadrant-CCD star tracker M. Clampin, S. T. Durrance, R. Barkhouser, D. A. Golimowski, A. Wald and W. G. Fastie Centre for Astrophysical Sciences, The Johns Hopkins University, Baltimore, MD21218. D.L
Wavefront Correction Technologies
Wavefront Correction Technologies Scot S. Olivier Adaptive Optics Group Leader Physics and Advanced Technologies Lawrence Livermore National Laboratory Associate Director NSF Center for Adaptive Optics
Adaptive Optics Phoropters
Adaptive Optics Phoropters Scot S. Olivier Adaptive Optics Group Leader Physics and Advanced Technologies Lawrence Livermore National Laboratory Associate Director NSF Center for Adaptive Optics Adaptive
NOAO Annual Management Report Adaptive Optics Development Program (AODP)
NOAO Annual Management Report Adaptive Optics Development Program (AODP) Prepared for: National Science Foundation Scientific Program Order No. 6 (AST-0336888) is awarded Pursuant to Cooperative Agreement
Design parameters Summary
634 Entrance pupil diameter 100-m Entrance pupil location Primary mirror Exit pupil location On M6 Focal ratio 6.03 Plate scale 2.924 mm / arc second (on-axis) Total field of view 10 arc minutes (unvignetted)
Potential benefits of freeform optics for the ELT instruments. J. Kosmalski
Potential benefits of freeform optics for the ELT instruments J. Kosmalski Freeform Days, 12-13 th October 2017 Summary Introduction to E-ELT intruments Freeform design for MAORY LGS Free form design for
A Segmented, Deployable, Primary Mirror for Earth Observation from a Cubesat Platform
A Segmented, Deployable, Primary Mirror for Earth Observation from a Cubesat Platform Noah Schwarz, David Pearson, Stephen Todd, Andy Vick, David Lunney, Donald MacLeod United Kingdom Astronomy Technology
Wavefront sensing for adaptive optics
Wavefront sensing for adaptive optics Richard Dekany Caltech Optical Observatories 2009 Thanks to: Acknowledgments Marcos van Dam original screenplay Brian Bauman adapted screenplay Contributors Richard
Keck Telescope Wavefront Errors: Implications for NGAO
Keck Telescope Wavefront Errors: Implications for NGAO KECK ADAPTIVE OPTICS NOTE 482 Christopher Neyman and Ralf Flicker March 13, 2007 ABSTRACT This note details the effect of telescope static and dynamic
The predicted performance of the ACS coronagraph
Instrument Science Report ACS 2000-04 The predicted performance of the ACS coronagraph John Krist March 30, 2000 ABSTRACT The Aberrated Beam Coronagraph (ABC) on the Advanced Camera for Surveys (ACS) has
Fratricide effect on ELTs
1st AO4ELT conference, 04005 (2010) DOI:10.1051/ao4elt/201004005 Owned by the authors, published by EDP Sciences, 2010 Fratricide effect on ELTs DamienGratadour 1,a,EricGendron 1,GerardRousset 1,andFrancoisRigaut
Compact Dual Field-of-View Telescope for Small Satellite Payloads
Compact Dual Field-of-View Telescope for Small Satellite Payloads James C. Peterson Space Dynamics Laboratory 1695 North Research Park Way, North Logan, UT 84341; 435-797-4624 Jim.Peterson@sdl.usu.edu
Enabling Technologies for Visible Adaptive Optics: The Magellan Adaptive Secondary VisAO Camera
Enabling Technologies for Visible Adaptive Optics: The Magellan Adaptive Secondary VisAO Camera Derek Kopon *a, Jared Males a, Laird M. Close a, Victor Gasho a a CAAO, Steward Observatory, University of
Predicting the Performance of Space Coronagraphs. John Krist (JPL) 17 August st International Vortex Workshop
Predicting the Performance of Space Coronagraphs John Krist (JPL) 17 August 2016 1 st International Vortex Workshop Determine the Reality of a Coronagraph through End-to-End Modeling Use End-to-End modeling
Wavefront sensing for adaptive optics
Wavefront sensing for adaptive optics Brian Bauman, LLNL This work performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344.
Exoplanet transit, eclipse, and phase curve observations with JWST NIRCam. Tom Greene & John Stansberry JWST NIRCam transit meeting March 12, 2014
Exoplanet transit, eclipse, and phase curve observations with JWST NIRCam Tom Greene & John Stansberry JWST NIRCam transit meeting March 12, 2014 1 Scope of Talk NIRCam overview Suggested transit modes
ShaneAO Instrument Document
ShaneAO Instrument Document Abstract This document contains a description of the ShaneAO system goals, requirements, and design, and provides the observer s and operator s guides. Version history Version
Shack Hartmann sensor improvement using optical binning
Shack Hartmann sensor improvement using optical binning Alastair Basden,* Deli Geng, Dani Guzman, Tim Morris, Richard Myers, and Chris Saunter Department of Physics, South Road, Durham, DH1 3LE, UK *Corresponding
Matthew R. Bolcar NASA GSFC
Matthew R. Bolcar NASA GSFC 14 November 2017 What is LUVOIR? Crab Nebula with HST ACS/WFC Credit: NASA / ESA Large UV / Optical / Infrared Surveyor (LUVOIR) A space telescope concept in tradition of Hubble
Paper Synopsis. Xiaoyin Zhu Nov 5, 2012 OPTI 521
Paper Synopsis Xiaoyin Zhu Nov 5, 2012 OPTI 521 Paper: Active Optics and Wavefront Sensing at the Upgraded 6.5-meter MMT by T. E. Pickering, S. C. West, and D. G. Fabricant Abstract: This synopsis summarized
CXCI. Optical design of a compact telescope for the next generation Earth Observation system CXCI. Vincent COSTES. Octobre 2012
CXCI Optical design of a compact telescope for the next generation Earth Observation system Vincent COSTES Octobre 2012 CXCI CXCI SUMMARY INTRODUCTION CXCI TECHNOLOGICAL PROGRAM COMPACTNESS REQUIREMENT
Optimization of coupling between Adaptive Optics and Single Mode Fibers ---
Optimization of coupling between Adaptive Optics and Single Mode Fibers --- Non common path aberrations compensation through dithering K. Saab 1, V. Michau 1, C. Petit 1, N. Vedrenne 1, P. Bério 2, M.
Detectors that cover a dynamic range of more than 1 million in several dimensions
Detectors that cover a dynamic range of more than 1 million in several dimensions Detectors for Astronomy Workshop Garching, Germany 10 October 2009 James W. Beletic Teledyne Providing the best images
The new CMOS Tracking Camera used at the Zimmerwald Observatory
13-0421 The new CMOS Tracking Camera used at the Zimmerwald Observatory M. Ploner, P. Lauber, M. Prohaska, P. Schlatter, J. Utzinger, T. Schildknecht, A. Jaeggi Astronomical Institute, University of Bern,
RAPID: A Revolutionary Fast Low Noise Detector on Pionier
: A Revolutionary Fast Low Noise Detector on Pionier Sylvain Guieu ESO / IPAG Jean Baptiste Lebouquin Philippe Feautrier Gérard Zins Éric Stadler Pierre Kern Alain Delboulbé Thibault Moulin Sylvain Rochas
NGAO NGS WFS design review
NGAO NGS WFS design review Caltech Optical 1 st April2010 1 Presentation outline Requirements (including modes of operation and motion control) Introduction NGSWFS input feed (performance of the triplet
Corner Rafts LSST Camera Workshop SLAC Sept 19, 2008
Corner Rafts LSST Camera Workshop SLAC Sept 19, 2008 Scot Olivier LLNL 1 LSST Conceptual Design Review 2 Corner Raft Session Agenda 1. System Engineering 1. Tolerance analysis 2. Requirements flow-down
Difrotec Product & Services. Ultra high accuracy interferometry & custom optical solutions
Difrotec Product & Services Ultra high accuracy interferometry & custom optical solutions Content 1. Overview 2. Interferometer D7 3. Benefits 4. Measurements 5. Specifications 6. Applications 7. Cases
Large-Actuator-Count MEMS. Deformable Mirror Development
Large-Actuator-Count MEMS www.irisao.com Deformable Mirror Development Michael A. Helmbrecht Iris AO, Inc. www.irisao.com michael.helmbrecht@irisao.com info@irisao.com NIH/NEI Phase II SBIR: 2 R44 EY015381-02A1
Infrared adaptive optics system for the 6.5 m MMT: system status
Infrared adaptive optics system for the 6.5 m MMT: system status M. Lloyd-Hart, G. Angeli, R. Angel, P. McGuire, T. Rhoadarmer, and S. Miller Center for Astronomical Adaptive Optics, University of Arizona,
Lecture 7: Wavefront Sensing Claire Max Astro 289C, UCSC February 2, 2016
Lecture 7: Wavefront Sensing Claire Max Astro 289C, UCSC February 2, 2016 Page 1 Outline of lecture General discussion: Types of wavefront sensors Three types in more detail: Shack-Hartmann wavefront sensors
PYRAMID WAVEFRONT SENSOR PERFORMANCE WITH LASER GUIDE STARS
Florence, Italy. Adaptive May 2013 Optics for Extremely Large Telescopes III ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13138 PYRAMID WAVEFRONT SENSOR PERFORMANCE WITH LASER GUIDE STARS Fernando Quirós-Pacheco
On-sky performance demonstration of the near infrared SAPHIRA e-apd array and new developments of e-apd technology
On-sky performance demonstration of the near infrared SAPHIRA e-apd array and new developments of e-apd technology Gert Finger * a, Ian Baker b, Domingo Alvarez a, Christophe Dupuy a, Derek Ives a, Leander
Payload Configuration, Integration and Testing of the Deformable Mirror Demonstration Mission (DeMi) CubeSat
SSC18-VIII-05 Payload Configuration, Integration and Testing of the Deformable Mirror Demonstration Mission (DeMi) CubeSat Jennifer Gubner Wellesley College, Massachusetts Institute of Technology 21 Wellesley
HiCIAO for WEB
HiCIAO High Contrast Instrument for the Subaru Next Generation Adaptive Optics 2007.3.21 for WEB HiCIAO development team (starting member) M. Tamura 1, K. Hodapp 2, R. Suzuki 2,H. Takami 3, L. Abe 1, O.