Understanding Speckle Noise and Dynamic Range in Coronagraphic Images
|
|
- Rhoda Garrison
- 5 years ago
- Views:
Transcription
1
2 Understanding Speckle Noise and Dynamic Range in Coronagraphic Images Remi Soummer American Museum of Natural History New York
3 Collaborators University of Nice: Claude Aime, Andre Ferrari AMNH: B. Oppenheimer, A. Sivaramakrishnan, A. Digby, S. Hinkley Cornell J. Lloyd STScI: R. Makidon Berkeley J. Graham, M. Perrin, M. Fitzgerald HIA L. Jolissaint (PAOLA package)
4 55 Cnc Lyot Project Coronagraph first light
5 planet is a faint point-like source over a noisy background Several sources of noise: speckle photon detector etc. The stability and statistical properties of these noise source will define the actual dynamic range
6 Lyot project dynamic range Vega dynamic range, 5 Σ, 3s $m Long exposure 4 sec 35 # "7. 3! "7. 5! "8.! "9. 5! ".! ". 5! ".! " Contrast levels (dynamic range) for a sec exposure Short Exposure ( sec) Short exposure sec 35 Long exposure 4 sec (tip-tilt off) Hinkley etal in prep
7 Lyot project dynamic range Long exposure 4 sec Short Exposure ( sec) Short exposure sec Contrast levels (dynamic range) for a sec exposure Main limitation in this case: Quasi-Static Speckles Long exposure 4 sec (tip-tilt off) Hinkley etal in prep
8 A few questions... What is the statistics of the speckle noise in direct high Strehl images? What is the effect of a coronagraph on the statistics of the noise? What is the interaction between coronagraph, static, quasi-static and residual atmospheric speckles? Need for a statistical model Start with direct images Study the effect of a coronagraph Study the effect of static or quasi-static aberrations
9 Speckle and photon noise in direct images
10 imaging in the presence of wavefront errors Speckle pinning (Bloemof etal, Sivaramakrishnan etal ) Palomar AO juin 4 K band 5. CORRECTOR PROOF-OF-CONCEPT DEMONSTRATION The technical feasibility of correcting the mid-spatial-frequency surface errors in large optical components (primary & secondary mirrors) using a small, microfigured mirror was recently demonstrated by ASML Inc. (previously the precision lithographic optics division of Tinsley SVG). They were contracted to produce a small (7 mm) mirror that would correct a provided wavefront error map to a specified level. They were given a map (Figure 6) based on the surface errors of the Hubble Space Telescope (HST) that was derived from phase retrieval measurements from on-orbit data. This map was chosen because it was readily available and represents a worst-case scenario for a future optical Accurate and stable pointing 4) is critical to maintaining alignment of the beam on the corrector mirror and keeping the system like JPF; the mirrors in a new optical system would be much smoother (Figure and would lackthethe record star centered on the occulting spot. Thermally induced variations in the telescope structure can also alter the optical grove polishing errors seen in the HST maps. alignment. The ISS alt-az mounting from Lockheed used by JPF has a pointing and tracking accuracy of., and finer Simulated AO PSF origin: wavefront errors control is maintained using the FSM. The optical bench is kept at a constant temperature using heating elements and thermal isolators. Pointingsof are time. avoided that ASML was able to create a corrector within spec and within the allotted amount In could the introduce criticalsignificant 4-5 thermal variations (for example, the telescope never points at the Earth, the major source of thermal instability in the Hubble Space Telescope). cycles/aperture range, the best-achieved corrected wavefront error (x effective surface error) was.5 nm RMS (Figure To suppress the diffraction below thefrom expected of scatter 7). The corrector would reduce scattered light by a factor of 5x to x, depending onpattern the radius thelevel star. Withlight, we investigated the performance of not only conventional Lyot coronagraphs but also shaped and apodized apertures, such as the Gaussian-like shaped or apodizedadditional time or a smoother wavefront map, they would be able to produce even better results. square apertures favored by other teams. In the end, the apodized-spot Lyot coronagraph was selected because it atmospheric residuals and/or quasi static aberrations (space & ground) provided the best combination of field-of-view, resolution, and throughput. Apodized spots permit more efficient suppression of the diffracted light while making the system slightly less sensitive to jitter. Such spots, however, are difficult to make accurately. For JPF, we have Gaussian-apodized spots with half-widths-at-half-maximum of.4 and.8. Because they are tapered in transmission, imaging is possible within the spot. Target -Corrector Residual Figure 4. This is the surface error map of a. meter diameter mirror produced by ASML (formerly Tinsley) for UV photolithography. It has an RMS midfrequency surface (/ wavefront) error of.5 nm. It demonstrates the current state-ofthe-art in optical surface figuring. A version of this map was used as the assumed residual wavefront error pattern in JPF optical simulations. Compare the smoother surface of this mirror with that of the HST primary (of which a modified form is shown in Figure 4). HST (Krist) TINSLEY (Krist) 7 mm 3. MICROFIGURED WAVEFRONT Figure 6. (Left) Modified surface amplitude map derived from HST phase retrieval measurements that was provided to ASML as the CORRECTOR AO simulation using PAOLA
11 Speckles Two complementary approaches: Wavefront propagation using Tayor expansion (Sivaramakrishnan etal., Perrin etal. 3). Statistical optics approach (Aime & Soummer 4, Soummer & Aime 4)
12 Statistical model: pupil plane Wave amplitude at the pupil plane: Ψ (x, y) = [A + a(x, y)] P (x, y) Plane wave uncorrected part of the wavefront Phase simulation Amplitude (scintillation)
13 Statistical model: pupil plane Wave amplitude at the pupil plane: Ψ (x, y) = [A + a(x, y)] P (x, y) Plane wave uncorrected part of the wavefront Im pupille avec phase seule This decomposition is also valid in space Complex PDF AO simulation phase + amplitude Re Phase simulation Amplitude (scintillation)
14 Statistical model: focal plane Ψ (x, y) = [A + a(x, y)] P (x, y) Ψ (x, y) = A F[P (x, y)] + F[a(x, y) P (x, y)] C (r) S(r) Constant deterministic term Speckle random term P(ξ, η) = exp π < S(r) >! (ξ Re[C (r)]) + (η Im[C (r)]) < S(r) > decentered gaussian statistics (complex amplitude in the focal plane) same solution as for holographic speckle (Goodman 975) "
15 Statistical model: focal plane P(ξ, η) = exp π < S(r) >! (ξ Re[C (r)]) + (η Im[C (r)]) < S(r) > " decentered gaussian statistics (complex amplitude in the focal plane) same solution as for holographic speckle (Goodman 975)
16 Statistical model: focal plane!! # (ξ I + IcRe[C (r)]) I +Ic PI (I) = exp exp I P(ξ, η) = Is Is Is π < S(r) > < S(r) " Statistics of the intensity in the focal plane: modified Rice distribution! " I + Ic PI (I) = exp Is Is. Ic and Is r "arcsec# # $ I Ic I Is. Ic and Is r "arcsec# ".5 ".5 "5. - "5. - "7.5 "7.5 "Log# -4 ". -6 "5. ".5 "#m# "Log# -4 ". -6 "5. ".5 "#m# "7.5 "7.5 ". -8 ". -8 ".5 ".5 Λ!D r "Λ!D# "5. Λ!D Ic = C (r). Λ!D r "Λ!D# "5. Λ!D Is =< S(r) >
17 Statistical model: focal plane Modified Rice distribution! I + Ic PI (I) = exp Is Is " # $ I Ic I Is
18 Photon counting statistics Poisson Mandel Transformation! P(n) = n! PI (I)I n exp( I)dI Photon counting statistics:! n Ic P(n) = ( + ) exp Is + Is Is P(n) " F! Ic n + ; ; Is + Is P(n).35 Ic= Is=..3.5 Ic=4 Is= n n "
19 Mean and Variance Mean intensity: diffraction pattern + halo < Ψ (x, y) >= C(x, y) + < S(x, y) >= Ic + Is Variance speckle: σi = Is + Is Ic
20 Mean and Variance Mean intensity: diffraction pattern + halo < Ψ (x, y) >= C(x, y) + < S(x, y) >= Ic + Is Variance speckle: σi = Is + Is Ic Variance speckle + photon noise: σ = Is + Is Ic + Ic + Is Same variance expression used in the TPF error budget by Shaklan 4
21 Explanation of speckle pinning P(I) P(I).35.5 σi = Is + Is Ic.3 P(I).5.35 P(I)..3 High continuous value amplification of the fluctuation C(r) I P(I) A C(r) 4 4 B C r(λ/d) r(λ/d). 8 6 r(λ/d).5.3 zero of the PSF exponential statistics P(I) ! I PI (I) = exp Is Is I.5 r(λ/d) I I..8 P(I) P(I).5.6 A B C P(I).8.4 low value of the continuous level I. P(I) I C(r) P(I) C(r). I..5. P(I) I I. I "
22 Lick ao data Lick AO First verification on sky of speckles rician statistics: Fitzgerald & Graham (5)
23 Palomar ao data Palomar AO single point statistics through the data cube Exposure time ms in K band, need for a model of integrated speckles $ " # # $!!" M c) I + I c M (i+i I I M i i i M c c PI (I) = exp Iis IM e Iiss ic Is Is is Non central chi square distribution of order M Soummer etal in prep
24 Palomar ao data Maximum Likelihood: Non central chi square vs. data!ic!" 59.58, Is!" 6.635".5 Kolmogorov Smirnoff test i.e. lifetime of 3ms consistent with K band M= 3 4 M=4 3 4 M=6 3 4 dark rings pixels fail the KS test need to include detector noise in the model... work in progress Soummer etal in prep
25 Effect of a coronagraph on the speckle and photon noise
26 ExAOC CODD Figure 8 Left: Gemini pupil without spiders. Right: An optimized shaped pupil that allows for geometry, and provides a -7 contrast floor in a wedge with 5!/D `waist ! Figure 8 Left: perfect PSF of the pupil in Figure 8, with no residual WFE. The green line c contour of -6 relative to the bright central peak. The waist of suppression correspondi peak s PSF is approximately 5!/D across horizontally. Right: The same pupil, with a 96 SFWFS AO-corrected wave front, produces a PSF which is brighter than -6 everywhere w area of the AO system and deformable mirror. The -6 contour lies completely outside the p!/d on a side !"#$%&'()'*+,--"."/,"'.'/%#%,34"/'//&3-5' Phase Masks (PM) 4.4. Systematic Classification of Approaches OPD (x ) OPD (x ) Simple Phase Mask (PM) coronagraphs modify the wave front at the image plane b regions of " radians of phase difference between different parts of the image to crea interference of on-axis light. Recent advances in PM coronagraphy (Soummer et a more sophisticated phase masks to create achromatic (i.e. exact at two wavelengths apochromatic cancellation over wide bandpasses. While recent work on the PM co has indeed shown progress, we have rejected this design, citing three major concern manufacturability, chromatic effects with wide bandwidths, and residual image mo requirements. $!%&'()*'+)(!,(*)-.!)(/(*%,!*!-3-(4',!&!-3)335)*4.6!$!,.3)'!7(,-)&4'&3!*7!38 (-%*'+)(!&,!,.39!&!:*;%(!"<!9&'.!)(=()(-(,!'3!&')37+-'3)!*)'&-%(,!*7!*!*''(4'!'3! 73-+('!'.(!*/*&%*;%(!7&,-+,,&3!3=!'.(!-3-(4'!&!'.(!%&'()*'+)(6!$!4)(%&&*)!-%*,,&=&8 -*'&3!3=!'.(!=*&%&(,!3=!-3)335)*4.,!'.*'!.*/(!7(/(%34(7!&,!4)(,('(7!&!>&5+)(!?6!:.&,! ')((8;*,(7! -%*,,&=&-*'&3! -*4'+)(,!,(/()*%!,*%&('! 7&==()(-(,! ;('9((! -3)335)*4.! 7( D - February 5, 5 D ICD.9.x Page 7
27 Effect of a coronagraph The direct focal plane amplitude is: Ψ (r) = Cd (r) + S(r) Static direct response Speckle term
28 Effect of a coronagraph The direct focal plane amplitude is: Ψ (r) = Cd (r) + S(r) Static direct response Speckle term The coronagraphic focal plane amplitude is: Ψ4 (r) = Cc (r) + S(r) Static coronagraph response Speckle term A coronagraph has a no effect on the speckle term outside the mask area
29 Suppression of speckle amplification Speckle term: (not affected by a coronagraph)..4 Ic and Is r "arcsec# Ic and Is r arcsec " " "7.5 "Log# ".5 "#m# " ". -4 Log "7.5 " ".5 Λ!D Ic without coronagraph Λ!D r "Λ!D# "5. 3 Λ!D.4 Λ D Λ D r Λ D 3 Λ D 5. Ic with coronagraph Suppression of the speckle amplification due to the Ic term Dm
30 Suppression of speckle amplification A coronagraph can suppress the speckle noise coherent amplification (speckle pinning) Direct coronagraphic gain where Ic>Is σ = (Is Ic + Ic ) + Can be removed by a coronagraph (Is + Is ) = σc Unaffected by a coronagraph + σs
31 Semi-analytical method Ic and Is from simulations Variance from analytical expressions..4.6 r(arcsec) (Log) -7 Dynamic Range (Δm) Photons Speckle r (λ/d) 3 4
32 Static aberrations The static coronagraph response includes the static aberrations Ψ4 (r) = Cc (r) + S(r) Residual pinning amplification by static aberrations through the coronagraph! space observations like TPF
33 Static + Quasi-static Quasi-static speckles can also be included Decomposition into: perfect, static, quasi static and atmospheric terms: Ψ = A + As (x) + a (x) + a (x) Ψ4 = C + S (x) + S (x)! " σ = N τ Is + kis + I c (Is + kis ) + Is Is
34 Conclusions (I) The speckle statistics of direct and coronagraphic images is given by a modified Rice distribution Ground based: (static + ao) Space: (static + quasi static) Generalization possible for the ground (static + ao + quasi static) Model consistent with real data
35 Conclusions (II) Semi-analytical method to study/predict dynamic range Speckle calibration/cancellation (slow) necessary to reach the atmospheric variance level Performance of the speckle reduction can be derived from the analysis of the limiting noise contribution
36
The Lyot Project Status and Results
The Lyot Project Status and Results Anand Sivaramakrishnan American Museum of Natural History NSF Center for Adaptive Optics Stony Brook University 941-channel AO on 3.6m AEOS telescope FPM 0.35 in H-band
More informationChristian Marois Lawrence Livermore National Laboratory
Christian Marois Lawrence Livermore National Laboratory -Detecting Exoplanets -Speckle noise attenuation techniques with specialized observation schemes and post-processing algorithms -Current On-sky performances
More informationTechniques for direct imaging of exoplanets
Techniques for direct imaging of exoplanets Aglaé Kellerer Institute for Astronomy, Hawaii 1. Where lies the challenge? 2. Contrasts required for ground observations? 3. Push the contrast limit Recycle!
More informationHigh Dynamic Range and the Search for Planets
Brown Dwarfs IAU Symposium, Vol. 211, 2003 E. L. Martín, ed. High Dynamic Range and the Search for Planets A. T. Tokunaga, C. Ftaclas, J. R. Kuhn, and P. Baudoz Institute for Astronomy, Univ. of Hawaii,
More informationEPICS: A planet hunter for the European ELT
EPICS: A planet hunter for the European ELT M. Kasper, C. Verinaud, J.L. Beuzit, N. Yaitskova, A. Boccaletti, S. Desidera, K. Dohlen, T. Fusco, N. Hubin, A. Glindemann, R. Gratton, N. Thatte 42-m E-ELT
More informationApplication of Precision Deformable Mirrors to Space Astronomy
Application of Precision Deformable Mirrors to Space Astronomy John Trauger, Dwight Moody Brian Gordon, Yekta Gursel (JPL) Mark Ealey, Roger Bagwell (Xinetics) Workshop on Innovative Designs for the Next
More informationError Budgets, and Introduction to Class Projects. Lecture 6, ASTR 289
Error Budgets, and Introduction to Class Projects Lecture 6, ASTR 89 Claire Max UC Santa Cruz January 8, 016 Page 1 What is residual wavefront error? Telescope AO System Science Instrument Very distorted
More informationComparative Exoplanetary Science
Comparative Exoplanetary Science A Technical Challenge Now, A Galaxy of Worlds Later! Ben R. Oppenheimer Assistant Curator of Astrophysics American Museum of Natural History & Adjunct Assistant Professor
More informationSuppressing stellar residual light on extremely large telescopes by aperture modulation
1st AO4ELT conference, 09002 (2010) DOI:10.1051/ao4elt/201009002 Owned by the authors, published by EDP Sciences, 2010 Suppressing stellar residual light on extremely large telescopes by aperture modulation
More informationTHE CHALLENGES OF CORONAGRAPHIC ASTROMETRY 1
The Astrophysical Journal, 650:484Y496, 2006 October 10 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. A THE CHALLENGES OF CORONAGRAPHIC ASTROMETRY 1 Andrew P. Digby,
More informationCoronagraphic Imaging of Exoplanets with NIRCam
Coronagraphic Imaging of Exoplanets with NIRCam C. Beichman NASA Exoplanet Science Institute, Jet Propulsion Laboratory, California Institute of Technology For the NIRCam Team September 27, 2016 Copyright
More informationStatistics of undeveloped speckles in partially polarized light
1st AO4ELT conference, 09006 (2010) DOI:10.1051/ao4elt/201009006 Owned by the authors, published by EDP Sciences, 2010 Statistics of undeveloped speckles in partially polarized light Natalia Yaitskova
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationSpeckles and adaptive optics
Chapter 9 Speckles and adaptive optics A better understanding of the atmospheric seeing and the properties of speckles is important for finding techniques to reduce the disturbing effects or to correct
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationADVANCING HIGH-CONTRAST ADAPTIVE OPTICS
ADVANCING HIGH-CONTRAST ADAPTIVE OPTICS S. Mark Ammons LLNL Bruce Macintosh Stanford University Lisa Poyneer LLNL Dave Palmer LLNL and the Gemini Planet Imager Team ABSTRACT A long-standing challenge has
More informationActive wavefront control for high contrast exoplanet imaging from space
Active wavefront control for high contrast exoplanet imaging from space John Trauger Spirit of Lyot Conference U.C. Berkeley 6 June 2007 Testbed operations and modeling at JPL: John Trauger, Brian Kern,
More informationIntroduction to Interferometer and Coronagraph Imaging
Introduction to Interferometer and Coronagraph Imaging Wesley A. Traub NASA Jet Propulsion Laboratory and Harvard-Smithsonian Center for Astrophysics Michelson Summer School on Astrometry Caltech, Pasadena
More information1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO?
Astronomy 418/518 final practice exam 1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO? b. Describe the visibility vs. baseline for a two element,
More informationThe Lyot Project: Status and Deployment Plans
The Lyot Project: Status and Deployment Plans Ben R. Oppenheimer, Andrew P. Digby, Laura Newburgh, Douglas Brenner, Michael Shara Department of Astrophyics American Museum of Natural History 79th Street
More informationHigh Contrast Imaging: Direct Detection of Extrasolar Planets
High Contrast Imaging: Direct Detection of Extrasolar Planets James R. Graham University of Toronto Dunlap Institute and Astronomy & Astrophysics September 16, 2010 Exoplanet Science How and where to planets
More informationAn Introduction to. Adaptive Optics. Presented by. Julian C. Christou Gemini Observatory
An Introduction to Adaptive Optics Presented by Julian C. Christou Gemini Observatory Gemini North in action Turbulence An AO Outline Atmospheric turbulence distorts plane wave from distant object. How
More informationADAPTIVE PHASE MASK CORONAGRAPH
Florence, Italy. May 2013 ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13183 ADAPTIVE PHASE MASK CORONAGRAPH Pierre Haguenauer 1,a, Pierre Bourget 1, Dimitri Mawet 1, and Nicolas Schuhler 1 1 European
More informationHigh contrast imaging at 3-5 microns. Philip M. Hinz University of Arizona Matt Kenworthy, Ari Heinze, John Codona, Roger Angel
High contrast imaging at 3-5 microns Philip M. Hinz University of Arizona Matt Kenworthy, Ari Heinze, John Codona, Roger Angel University of Arizona ABSTRACT The 6.5 m MMT with its integrated deformable
More informationExoplanet High Contrast Imaging: Space
Exoplanet High Contrast Imaging: Space Eric Cady Jet Propulsion Laboratory, California Institute of Technology KISS Short Course: Mastering the Wave The Whys and Hows of Exoplanet Imaging August 22, 2016
More informationResponse of DIMM turbulence sensor
Response of DIMM turbulence sensor A. Tokovinin Version 1. December 20, 2006 [tdimm/doc/dimmsensor.tex] 1 Introduction Differential Image Motion Monitor (DIMM) is an instrument destined to measure optical
More informationPAPER 338 OPTICAL AND INFRARED ASTRONOMICAL TELESCOPES AND INSTRUMENTS
MATHEMATICAL TRIPOS Part III Monday, 12 June, 2017 1:30 pm to 3:30 pm PAPER 338 OPTICAL AND INFRARED ASTRONOMICAL TELESCOPES AND INSTRUMENTS Attempt no more than TWO questions. There are THREE questions
More informationThe WFIRST Coronagraphic Instrument (CGI)
The WFIRST Coronagraphic Instrument (CGI) N. Jeremy Kasdin Princeton University CGI Adjutant Scientist WFIRST Pasadena Conference February 29, 2016 The Coronagraph Instrument Optical Bench Triangular Support
More informationAdaptive Optics for the Giant Magellan Telescope. Marcos van Dam Flat Wavefronts, Christchurch, New Zealand
Adaptive Optics for the Giant Magellan Telescope Marcos van Dam Flat Wavefronts, Christchurch, New Zealand How big is your telescope? 15-cm refractor at Townsend Observatory. Talk outline Introduction
More informationarxiv: v1 [astro-ph.im] 22 Mar 2012
Astronomy & Astrophysics manuscript no. SpeckleStability c ESO 2018 October 30, 2018 Speckle temporal stability in XAO coronagraphic images P. Martinez 1, C. Loose 2, E. Aller Carpentier 2, and M. Kasper
More informationPoint spread function reconstruction at W.M. Keck Observatory : progress and beyond
Point spread function reconstruction at W.M. Keck Observatory : progress and beyond Olivier Beltramo-Martin Aix-Marseille Univ., LAM, A*MIDEX, Extra November 9th, 217 - LAM Olivier Beltramo-Martin (LAM)
More informationRoadmap for PCS, the Planetary Camera and Spectrograph for the E-ELT
Florence, Italy. Adaptive May 2013 Optics for Extremely Large Telescopes III ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.12804 Roadmap for PCS, the Planetary Camera and Spectrograph for the E-ELT Markus
More informationHigh Contrast Imaging: New Techniques and Scientific Perspectives for ELTs
High Contrast Imaging: New Techniques and Scientific Perspectives for ELTs Is there a path to life What game changing finding with ELTs? technologies can get us there? Olivier Guyon Subaru Telescope &
More informationThe Nulling Coronagraph Using a Nulling Interferometer for Planet Detection in Visible Light with a Single Aperture Telescope
Terrestrial Planet Finder The Nulling Coronagraph Using a Nulling Interferometer for Planet Detection in Visible Light with a Single Aperture Telescope Michael Shao, B. Martin Levine, Duncan Liu, J. Kent
More informationAtmospheric dispersion correction for the Subaru AO system
Atmospheric dispersion correction for the Subaru AO system Sebastian Egner a, Yuji Ikeda b, Makoto Watanabe c,y.hayano a,t.golota a, M. Hattori a,m.ito a,y.minowa a,s.oya a,y.saito a,h.takami a,m.iye d
More informationHigh-contrast STScI activities in the context of US spatial missions. Marie Ygouf - Journées Haute Dynamique - ONERA 20 Janvier 2015
High-contrast STScI activities in the context of US spatial missions Marie Ygouf - Journées Haute Dynamique - ONERA 20 Janvier 2015 1 Exoplanet Exploration Program Analysis Group (ExoPAG) meeting Can we
More informationDesigning a Space Telescope to Image Earth-like Planets
Designing a Space Telescope to Image Earth-like Planets Robert J. Vanderbei Rutgers University December 4, 2002 Page 1 of 28 Member: Princeton University/Ball Aerospace TPF Team http://www.princeton.edu/
More informationFully achromatic nulling interferometer (FANI) for high SNR exoplanet characterization
Fully achromatic nulling interferometer (FANI) for high SNR exoplanet characterization François Hénault Institut de Planétologie et d Astrophysique de Grenoble Université Joseph Fourier Centre National
More informationWavefront errors due to atmospheric turbulence Claire Max
Wavefront errors due to atmospheric turbulence Claire Max Page 1 Kolmogorov turbulence, cartoon solar Outer scale L 0 Inner scale l 0 h Wind shear convection h ground Page Atmospheric Turbulence generally
More informationWebster Cash University of Colorado. X-ray Interferometry
Webster Cash University of Colorado X-ray Interferometry Co-Investigators Steve Kahn - Columbia University Mark Schattenburg - MIT David Windt - Lucent (Bell-Labs) Outline of Presentation Science Potential
More information1. INTRODUCTION ABSTRACT
Simulations of E-ELT telescope effects on AO system performance Miska Le Louarn* a, Pierre-Yves Madec a, Enrico Marchetti a, Henri Bonnet a, Michael Esselborn a a ESO, Karl Schwarzschild strasse 2, 85748,
More informationWavefront Sensing using Polarization Shearing Interferometer. A report on the work done for my Ph.D. J.P.Lancelot
Wavefront Sensing using Polarization Shearing Interferometer A report on the work done for my Ph.D J.P.Lancelot CONTENTS 1. Introduction 2. Imaging Through Atmospheric turbulence 2.1 The statistics of
More informationGemini Planet Imager. Raphaël Galicher from presentations provided by James Graham and Marshall Perrin
Gemini Planet Imager from presentations provided by James Graham and Marshall Perrin Outline Ojectives The instrument Three examples of observations The GPI Exoplanet Survey 2 Objectives Radial velocity
More informationHigh-contrast Coronagraph Development in China for Direct Imaging of Extra-solar Planets
High-contrast Coronagraph Development in China for Direct Imaging of Extra-solar Planets Jiangpei Dou 1, Deqing Ren 1,2, Yongtian Zhu 1, Xi Zhang 1 1 Astronomical Observatories/Nanjing Institute of Astronomical
More informationarxiv: v1 [astro-ph.im] 10 Oct 2017
Experimental parametric study of the Self-Coherent Camera arxiv:1710.03520v1 [astro-ph.im] 10 Oct 2017 Johan Mazoyer a, Pierre Baudoz a, Marion Mas ab, Gerard Rousset a,raphaël Galicher cd a LESIA, Observatoire
More informationTHE SUBARU CORONAGRAPHIC EXTREME AO HIGH SENSITIVITY VISIBLE WAVEFRONT SENSORS
Florence, Italy. May 2013 ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13398 THE SUBARU CORONAGRAPHIC EXTREME AO HIGH SENSITIVITY VISIBLE WAVEFRONT SENSORS Christophe Clergeon 1a, Olivier Guyon 1, Frantz
More informationThe SPICA Coronagraph
The SPICA Coronagraph 2007, Jun 7 th, UC BERKELEY K. Enya 1, L. Abe 2, S. Tanaka 1, T. Nakagawa 1, M. Tamura 2, H. Kataza 1, O. Guyon 3, SPICA Working Group ( 1: ISAS/JAXA, 2: NAOJ, 3: NAOJ/SUBARU observatory)
More informationControl of the Keck and CELT Telescopes. Douglas G. MacMartin Control & Dynamical Systems California Institute of Technology
Control of the Keck and CELT Telescopes Douglas G. MacMartin Control & Dynamical Systems California Institute of Technology Telescope Control Problems Light from star Primary mirror active control system
More informationDiffraction model for the external occulter of the solar coronagraph ASPIICS
Diffraction model for the external occulter of the solar coronagraph ASPIICS Raphaël Rougeot OCA, Nice 14/05/2018 14/05/2018 R.Rougeot 1 Outline 1) Proba-3 mission and ASPIICS 2) Diffraction from external
More informationProximity Glare Suppression for Astronomical Coronagraphy (S2.01) and Precision Deployable Optical Structures and Metrology (S2.
Proximity Glare Suppression for Astronomical Coronagraphy (S2.01) and Precision Deployable Optical Structures and Metrology (S2.02) Mirror Tech Days 2015 Annapolis, MD Nov 10, 2015 Stuart Copyright 2015.
More informationAdaptive Optics Lectures
Adaptive Optics Lectures 1. Atmospheric turbulence Andrei Tokovinin 1 Resources CTIO: www.ctio.noao.edu/~atokovin/tutorial/index.html CFHT AO tutorial: http://www.cfht.hawaii.edu/instruments/imaging/aob/other-aosystems.html
More informationDiffraction modelling for solar coronagraphy
Diffraction modelling for solar coronagraphy Application to ASPIICS Raphaël Rougeot Laboratoire Lagrange, Nice 12/02/2018 12/02/2018 R.Rougeot 1 Outline 1) Proba-3 mission and ASPIICS 2) Diffraction from
More informationPupil mapping Exoplanet Coronagraph Observer (PECO)
Pupil mapping Exoplanet Coronagraph Observer (PECO) Olivier Guyon University of Arizona Subaru Telescope Thomas Greene (NASA Ames), Marie Levine (NASA JPL), Domenick Tenerelli (Lockheed Martin), Stuart
More informationx Contents Segmented Mirror Telescopes Metal and Lightweight Mirrors Mirror Polishing
Contents 1 Fundamentals of Optical Telescopes... 1 1.1 A Brief History of Optical Telescopes.................... 1 1.2 General Astronomical Requirements..................... 6 1.2.1 Angular Resolution.............................
More informationarxiv:astro-ph/ v1 2 Oct 2002
**TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** The Extra-Solar Planet Imager (ESPI) arxiv:astro-ph/0210046v1 2 Oct 2002 P. Nisenson, G.J. Melnick, J. Geary,
More informationSearching for Earth-Like Planets:
Searching for Earth-Like Planets: NASA s Terrestrial Planet Finder Space Telescope Robert J. Vanderbei January 11, 2004 Amateur Astronomers Association of Princeton Peyton Hall, Princeton University Page
More informationExoplanet High Contrast Imaging Technologies Ground
Exoplanet High Contrast Imaging Technologies Ground KISS Short Course: The Hows and Whys of Exoplanet Imaging Jared Males University of Arizona Telescope Diameter (Bigger is Better) Diameter: Collecting
More informationSurvey of Present and Future Ground-Based Imaging Systems
Survey of Present and Future Ground-Based Imaging Systems Olivier Guyon (guyon@naoj.org) University of Arizona Subaru Telescope With material from : Rich Dekany, Ben Oppenheimer (Palm 3000, P1640) Bruce
More informationImage requirements for the detection and caracterisation of Earth-like planets and hot Jupiter s
Image requirements for the detection and caracterisation of Earth-like planets and hot Jupiter s Alain Chelli Laboratoire d Astrophysique de Grenoble & Jean-Marie Mariotti Center Content The Optical system
More informationCheapest nuller in the World: Crossed beamsplitter cubes
Cheapest nuller in the World: François Hénault Institut de Planétologie et d Astrophysique de Grenoble, Université Joseph Fourier, CNRS, B.P. 53, 38041 Grenoble France Alain Spang Laboratoire Lagrange,
More informationNICMOS Status and Plans
1997 HST Calibration Workshop Space Telescope Science Institute, 1997 S. Casertano, et al., eds. NICMOS Status and Plans Rodger I. Thompson Steward Observatory, University of Arizona, Tucson, AZ 85721
More informationFundamental Limits to Wavefront Sensing in the Submillimeter
Fundamental Limits to Wavefront Sensing in the Submillimeter E. Serabyn Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, USA 91109 Copyright 2006 Society
More informationOptical/IR Observational Astronomy Telescopes I: Telescope Basics. David Buckley, SAAO
David Buckley, SAAO 27 Feb 2012 1 Some other Telescope Parameters 1. Plate Scale This defines the scale of an image at the telescopes focal surface For a focal plane, with no distortion, this is just related
More informationHunting Planets and Observing Disks with the JWST NIRCam Coronagraph
Hunting Planets and Observing Disks with the JWST NIRCam Coronagraph John E. Krist a, Charles A. Beichman a, John T. Trauger a, Marcia J. Rieke b, Steve Somerstein c, Joseph J. Green a, Scott D. Horner
More informationPhase-Referencing and the Atmosphere
Phase-Referencing and the Atmosphere Francoise Delplancke Outline: Basic principle of phase-referencing Atmospheric / astrophysical limitations Phase-referencing requirements: Practical problems: dispersion
More informationAstronomical Seeing. Northeast Astro-Imaging Conference. Dr. Gaston Baudat Innovations Foresight, LLC. April 7 & 8, Innovations Foresight
Astronomical Seeing Northeast Astro-Imaging Conference April 7 & 8, 2016 Dr. Gaston Baudat, LLC 1 Seeing Astronomical seeing is the blurring of astronomical objects caused by Earth's atmosphere turbulence
More informationExtreme Optics and The Search for Earth-Like Planets
Extreme Optics and The Search for Earth-Like Planets Robert J. Vanderbei November 21, 27 ORFE 522 Fun (Pre-Thanksgiving) Lecture Work supported by ONR and NASA/JPL http://www.princeton.edu/ rvdb ABSTRACT
More informationExoplanet Instrumentation with an ASM
Exoplanet Instrumentation with an ASM Olivier Guyon1,2,3,4, Thayne Currie 1 (1) Subaru Telescope, National Astronomical Observatory of Japan (2) National Institutes for Natural Sciences (NINS) Astrobiology
More informationEngineering Specifications derived from Science Requirements for the Advanced Mirror Technology Development (AMTD) Project
Engineering Specifications derived from Science Requirements for the Advanced Mirror Technology Development (AMTD) Project H. Philip Stahl, NASA MSFC Marc Postman, STScI W. Scott Smith, NASA MSFC Reviewers:
More informationAchieving high resolution
Achieving high resolution Diffraction-limited performance with single telescopes with Adaptive Optics Or sparse aperture masking Use masks to sub-divide telescope primary into a numnber of subapertures
More informationDirect imaging and characterization of habitable planets with Colossus
Direct imaging and characterization of habitable planets with Colossus Olivier Guyon Subaru Telescope, National Astronomical Observatory of Japan University of Arizona Contact: guyon@naoj.org 1 Large telescopes
More informationImaging polarimetry of exo-planets with the VLT and the E-ELT Hans Martin SCHMID, ETH Zurich
Imaging polarimetry of exo-planets with the VLT and the E-ELT Hans Martin SCHMID, ETH Zurich Collaborators: ETH Zurich: E. Buenzli, F. Joos, C. Thalmann (now at MPIA) VLT SPHERE: J.L. Beuzit, D. Mouillet,
More informationOptical/IR Observational Astronomy Telescopes I: Telescope Basics. David Buckley, SAAO
David Buckley, SAAO 17 Feb 2010 1 Some other Telescope Parameters 1. Plate Scale This defines the scale of an image at the telescopes focal surface For a focal plane, with no distortion, this is just related
More informationThe Principles of Astronomical Telescope Design
The Principles of Astronomical Telescope Design Jingquan Cheng National Radio Astronomy Observatory Charlottesville, Virginia,.USA " 4y Springer Fundamentals of Optical Telescopes 1 1.1 A Brief History
More informationPolarimetry and spectral imaging of mature Jupiter and super-earth with SEE-COAST
Polarimetry and spectral imaging of mature Jupiter and super-earth with SEE-COAST Jean Schneider, A. Boccaletti, P. Baudoz, R. Galicher, R. Gratton, D. Stam et al. & E. Pantin, Complementarity of techniques
More informationCanariCam-Polarimetry: A Dual-Beam 10 µm Polarimeter for the GTC
Astronomical Polarimetry: Current Status and Future Directions ASP Conference Series, Vol. 343, 2005 Adamson, Aspin, Davis, and Fujiyoshi CanariCam-Polarimetry: A Dual-Beam 10 µm Polarimeter for the GTC
More informationEXPOSURE TIME ESTIMATION
ASTR 511/O Connell Lec 12 1 EXPOSURE TIME ESTIMATION An essential part of planning any observation is to estimate the total exposure time needed to satisfy your scientific goal. General considerations
More informationAS750 Observational Astronomy
Lecture 9 0) Poisson! (quantum limitation) 1) Diffraction limit 2) Detection (aperture) limit a)simple case b)more realistic case 3) Atmosphere 2) Aperture limit (More realistic case) Aperture has m pixels
More informationIntroduction to exoplanetology
Introduction to exoplanetology Lesson #6: Direct exoplanet detection methods (1/2) Olivier Absil absil@astro.ulg.ac.be Outline I. Direct detection: why and how? II. High contrast imaging from the ground
More informationImaging Survey for Faint Companions with Shaped Pupil Masks 1
Imaging Survey for Faint Companions with Shaped Pupil Masks 1 Jian Ge, John Debes, Anne Watson & Abhijit Chakraborty 55 Davey Lab, Department of Astronomy & Astrophysics, Penn State University, University
More informationAstronomie et astrophysique pour physiciens CUSO 2015
Astronomie et astrophysique pour physiciens CUSO 2015 Instruments and observational techniques Adaptive Optics F. Pepe Observatoire de l Université Genève F. Courbin and P. Jablonka, EPFL Page 1 Adaptive
More informationKeck Adaptive Optics Note 1069
Keck Adaptive Optics Note 1069 Tip-Tilt Sensing with Keck I Laser Guide Star Adaptive Optics: Sensor Selection and Performance Predictions DRAFT to be updated as more performance data becomes available
More informationAdaptive Optics Overview Phil Hinz What (Good) is Adaptive Optics?
Adaptive Optics Overview Phil Hinz (phinz@as.arizona.edu) What (Good) is Adaptive Optics? System Overview MMT AO system Atmospheric Turbulence Image Structure References: Adaptive Optics for Astronomical
More informationThe Potential of Ground Based Telescopes. Jerry Nelson UC Santa Cruz 5 April 2002
The Potential of Ground Based Telescopes Jerry Nelson UC Santa Cruz 5 April 2002 Contents Present and Future Telescopes Looking through the atmosphere Adaptive optics Extragalactic astronomy Planet searches
More informationProblem Solving. radians. 180 radians Stars & Elementary Astrophysics: Introduction Press F1 for Help 41. f s. picture. equation.
Problem Solving picture θ f = 10 m s =1 cm equation rearrange numbers with units θ factors to change units s θ = = f sinθ fθ = s / cm 10 m f 1 m 100 cm check dimensions 1 3 π 180 radians = 10 60 arcmin
More informationScientific context in 2025+
Outline Scientific context and goals O 2 detection on an Exoplanet with the E-ELT? PCS concept and technological challenges Timeframe for E-ELT high-contrast imaging Scientific context in 2025+ GAIA: Know
More informationAstronomy 203 practice final examination
Astronomy 203 practice final examination Fall 1999 If this were a real, in-class examination, you would be reminded here of the exam rules, which are as follows: You may consult only one page of formulas
More informationKeck Adaptive Optics Note #385. Feasibility of LGS AO observations in the vicinity of Jupiter. Stephan Kellner and Marcos van Dam
Keck Adaptive Optics Note #385 Feasibility of LGS AO observations in the vicinity of Jupiter Stephan Kellner and Marcos van Dam Version 2: 25 July 2006 1 Introduction It has been proposed by Imke De Pater
More informationHIGH-PRECISION ASTROMETRY WITH A DIFFRACTIVE PUPIL TELESCOPE
C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. doi:10.1088/0067-0049/200/2/11 HIGH-PRECISION ASTROMETRY WITH A DIFFRACTIVE PUPIL TELESCOPE Olivier Guyon 1,2, Eduardo
More informationsolar telescopes Solar Physics course lecture 5 Feb Frans Snik BBL 707
Solar Physics course lecture 5 Feb 19 2008 Frans Snik BBL 707 f.snik@astro.uu.nl www.astro.uu.nl/~snik solar vs. nighttime telescopes solar constant: 1.37 kw/m 2 destroys optics creates seeing solar vs.
More informationAnalysis of the Sequence Of Phase Correction in Multiconjugate Adaptive Optics
Analysis of the Sequence Of Phase Correction in Multiconjugate Adaptive Optics Luzma Montoya, Iciar Montilla Instituto de Astrofísica de Canarias Edinburgh, 25-26/03/2014 AO Tomography Workshop The EST
More informationDirect detection: Seeking exoplanet colors and spectra
Direct detection: Seeking exoplanet colors and spectra John Trauger, JPL / Caltech Keck Institute for Space Studies Workshop Caltech -- 10 November 2009 (c) 2009 California Institute of Technology. Government
More informationExoPlanets Imaging Camera Spectrograph for the European ELT Simulations
ExoPlanets Imaging Camera Spectrograph for the European ELT Simulations Christophe Vérinaud,Visa Korkiakoski Laboratoire d Astrophysique - Observatoire de Grenoble, France and EPICS consortium EPICS for
More informationDeformable mirror fitting error by correcting the segmented wavefronts
1st AO4ELT conference, 06008 (2010) DOI:10.1051/ao4elt/201006008 Owned by the authors, published by EDP Sciences, 2010 Deformable mirror fitting error by correcting the segmented wavefronts Natalia Yaitskova
More informationMAORY (Multi conjugate Adaptive Optics RelaY) for E-ELT. Paolo Ciliegi. On behalf of the MAORY Consortium
MAORY (Multi conjugate Adaptive Optics RelaY) for E-ELT Paolo Ciliegi INAF Osservatorio Astronomico di Bologna On behalf of the MAORY Consortium Science ELT Workshop Team Meeting ESO Garching, MPE Garching,
More informationTelescopes, Observatories, Data Collection
Telescopes, Observatories, Data Collection Telescopes 1 Astronomy : observational science only input is the light received different telescopes, different wavelengths of light lab experiments with spectroscopy,
More informationResidual phase variance in partial correction: application to the estimate of the light intensity statistics
3 J. Opt. Soc. Am. A/ Vol. 7, No. 7/ July 000 M. P. Cagigal and V. F. Canales Residual phase variance in partial correction: application to the estimate of the light intensity statistics Manuel P. Cagigal
More information7. Telescopes: Portals of Discovery Pearson Education Inc., publishing as Addison Wesley
7. Telescopes: Portals of Discovery Parts of the Human Eye pupil allows light to enter the eye lens focuses light to create an image retina detects the light and generates signals which are sent to the
More informationLaboratory Emulation of Observations from Space
Science with a Wide-field Infrared Telescopes in Space, Pasadena, Feb 13, 2012 of Observations from Space Roger Smith -- Caltech Jason Rhodes, Suresh Seshadri -- JPL Previous culture, friendly collaboration
More informationGPI Feasibility and P2 Checks
GPI Feasibility and Phase II Checks The goal of this presentation is to be able to do a proper technical asessment of a GPI proposal and spot the most common GPI Phase II issues. It should be noted that
More information