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John O’Byrne School of Physics University of Sydney Adaptive Optics 1 What is AO? Adaptive Optics: fast image correction (f 1 Hz), primarily to correct atmospheric wavefront distortions Active Optics: slow image correction (f 1 Hz), to correct mirror and structural deflections Adaptive Optics 2 Why do we need AO? Scintillation - describes random amplitude fluctuations of wavefront (twinkling) Seeing - describes random phase fluctuations of wavefront (image motion and blurring) AO aims to correct seeing effects - i.e. sharpen images Science objectives - e.g. GEMINI http://www.gemini.anu.edu.au/sciops/instruments/adaptiveOptics/Science_drivers.html Adaptive Optics 3 Where does Seeing arise? Turbulence in the atmosphere leads to refractive index variations. Contributions are concentrated into layers at different altitudes. Adaptive Optics 4 Scidar measurements at SSO 10 minutes of data refractive index structure constant (Cn2 ) v. altitude Adaptive Optics 5 Seeing parameters - 1 Fried parameter ro(l,z) = 0.185l6/5cos3/5z(Cn2dh)-3/5 Seeing disk FWHM without AO l/ro for large telescopes So at ~500nm, ro 10 cm for 1 arcsec FWHM seeing At 2.5mm, this corresponds to ro 70 cm and 0.7 arcsec seeing Adaptive Optics 6 Seeing parameters - 2 If seeing is dominated by a layer at altitude H: Isoplanatic angle (for wavefront distortion) qo 0.314 ro/H - typically a few arcsec in visible Isokinetic angle (for image motion) qk 0.314 Dtel/H - typically ~100 arcsec in visible Timescale for wavefront distortion to 0.314 ro/Vwind - typically ~ few ms Timescale for image motions tk 0.314 Dtel/Vwind - typically ~ 100 ms Adaptive Optics 7 What can we expect from AO? Improvement depends on Dtel relative to ro (R/Rmax is Strehl resolution normalised by exposure resolution of an infinte aperture) AO is easier in the infrared ro is larger qo is larger to is longer Also easier if H is lower Vwind is lower Adaptive Optics 8 Essentials of an AO system Wavefront sensor Computer Phase modulator Adaptive Optics 9 WFS - Shearing interferometer The Wavefront Sensor (WFS) may be Shearing interferometer (uncommon) Shears the wavefront to measure tilt in the shear direction Adaptive Optics 10 WFS - Shack-Hartmann Sensor Shack-Hartmann sensor (the usual choice) Uses lenslets to sub-divide the aperture and measures image motion in each sub-aperture. Adaptive Optics 11 WFS - Curvature Sensor Wavefront Curvature Sensor Uses lenslets to sub divide the aperture and measures curvature of the wavefront in each sub-aperture. Adaptive Optics 12 Phase Modulator The phase modulators are always a deformable mirror - usually tip-tilt and higher order separately. Actuators used: piezoelectric (PZT) electrostrictive voice-coil electrostatic But other technologies are possible Liquid Crystal phase screen devices More actuators => better correction. Adaptive Optics 13 Tit-tilt correction Tip-tilt mirror mounted on 4 piezoelectric stacks. Segmented surface deformable mirrors use tip-tilt on individual segments Adaptive Optics 14 Stacked-array Mirrors Continuous faceplates attached to piezoelectric stacks Visible on the edges of each mirror are the PZT actuators. Adaptive Optics 15 Bimorph mirrors Bimorph mirror made from piezoelectric wafers (sometimes one piezo and one glass) with an electrode pattern to control deformation Adaptive Optics 16 Membrane Mirrors Continuous faceplates deformed electrostatically by an underlying electrode pattern. Adaptive Optics 17 Sample of an AO result - 1 Adaptive Optics 18 Sample of an AO result - 2 Core diameter is recovered with low order correction, but a surrounding halo remains Adaptive Optics 19 AO limitations AO systems have limitations (e.g. light loss, IR emissivity driven by the large number of optical surfaces) but more fundamental are limits imposed by the guiding star, which is monitored by the wavefront sensor, and is likely to be different from the science target Adaptive Optics 20 Natural Guide Stars (NGS) temporal anisoplanatism - delays introduced by the servo loop angular anisoplanatism - NGS is usually offset from science target, but can't be too far away or it lies outside isoplanatic patch angle (qo) - can be improved by making the WFS conjugate to the primary turbulence layer (or multiple layers in multi-conjugate AO [MCAO]) WFS sensitivity limit => limited sky coverage Adaptive Optics 21 Laser Guide Stars (LGS) - 1 Use a laser to generate a ‘star’ in the atmosphere, very close to the science target’s light path through the atmosphere. This may be a Rayleigh guide star at 7-20 km or a Sodium guide star at 90 km. Overcomes NGS sky coverage limitation Adaptive Optics 22 Laser Guide Stars (LGS) - 2 Provides no tip-tilt information Cost! Problem to other telescopes on the site caused by back-scattered light Sodium guide star and Rayleigh back-scatter Adaptive Optics 23 Laser Guide Stars (LGS) - 3 Focus anisoplanatism the laser does not fully sample the stars light path through the atmosphere worse for a Rayleigh guide star provide multiple LGS? Adaptive Optics 24 AO Projects - 1 Australian projects RSAA 2.3m tip-tilt system Anglo-Australian Telescope International projects (e.g. see University of Durham list of links to other projects http://aig-www.dur.ac.uk/fix/adaptive-optics/area_main_ao.html) GEMINI http://www.gemini.anu.edu.au/sciops/instruments/adaptiveOptics/AOIndex.html AO at ESO / VLT http://www.eso.org/projects/aot/ Adaptive Optics 25 AO Projects - 2 Keck II and now Keck I http://www2.keck.hawaii.edu:3636/realpublic/inst/ao/ao.html University of Durham (UK) http://aig-www.dur.ac.uk/fix/adaptive-optics/area_main_ao.html University of Hawaii most recently Hokupa’a on GEMINI http://www.ifa.hawaii.edu/ao/ Earlier PUEO on CFHT http://www.cfht.hawaii.edu/Instruments/Imaging/AOB/ Adaptive Optics 26 Hokupa’a images - 1 CFHT Adaptive Optics 27 Hohupa’a Images - 2 QSO PG1700+518 and its companion starbust galaxy. These deep (2hr.) images were made by guiding on the 16th mag QSO itself. Raw AO PSF subtr. Deconlv. CFHT J H Adaptive Optics 28 Hohupa’a Images - 3 GEMINI Adaptive Optics 29 Keck Keck I AO image in H band taken during the first Keck I AO night (Dec.12,2000). Io angular size: 1.23 arcsecond Spatial resolution: 120 km Adaptive Optics 30 Starfire Optical Range (SOR) Adaptive Optics 31 References Information on AO projects can be obtained from their web sites or from the Proceedings of the (all too frequent) AO conferences (e.g. SPIE, OSA or ESO). A few other useful references: Popular level: Sharper Eyes on the Sky - Sky & Space, 9, 30 (1996) Untwinkling the Stars - Sky & Telescope, 87, May 24 & Jun 20, (1994) Adaptive Optics - Scientific American, Jun (1994) Reviews: Young, A.T. (1974), ApJ, 189, 587 Roddier, F. (1981), Progress in Optics, 19, 281 Coulman ARAA (1985), 23, 19 Beckers, J.M. (1993), ARAA 31, 13 Wilson, R.W.,Jenkins C.R. (1996), MNRAS, 268, 39 Adaptive Optics 32