lecture 16 extreme adaptive optics: exoplanets and protoplanetary disksmax/289/lectures 2016/lecture...
TRANSCRIPT
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Lecture 16
Extreme Adaptive Optics:
Exoplanets and Protoplanetary Disks
Claire Max AY 289
March 7, 2016 Based in part on slides from
Bruce Macintosh and Sandrine Thomas
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Outline
• Science parameter space for Exoplanet systems
• Direct imaging of exoplanets with ground-based AO
• Approaches to high-contrast imaging with current telescopes: Angular Differential Imaging
• Coronagraphs to block light from host star
• Gemini Planet Imager: one example of the current state of the art
• Recent scientific results: directly imaged planets and disks
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Exoplanets as of 2015
Now about 20
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Brightness of ExAO targets
Marley et al 2007
Hot start
Low-entropy core accretion models
HR8799
ExAO regime
Normal AO regime
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First images of an extrasolar planetary system (Keck and Gemini AO)
Marois et al. 2008 Science Mag
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Conventional AO limited by scattered light
Strehl ratio S
Halo intensity 1-S
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“Extreme” AO (ExAO)
gain > S/(1-S)
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Image processing to suppress light from host star
Marois et al.
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Keck AO Image of a bright star
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Inner part of image - artifacts due to AO optics
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Image 1 Image 2 (+ 5 minutes)
Subtraction
Angular Differential Imaging
Marois et al 2006
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+
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+ =
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Coronagraphs
• Invented by Bernard Lyot in 1930 for studying the corona of the sun without waiting for an eclipse
• Block the sun’s light with a circular mask in the focal plane
• Problem: diffraction from the sharp edges of the mask
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Cartoon of Lyot Coronagraph
Credit: Subaru website
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How can we control diffraction?
PSF=|FT(A)|2 A
PSF
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Lyot coronagraph (Lyot, 1933)
Starlight
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Lyot coronagraph (Lyot, 1933)
Planet
Sivaramakrishnan et al 2001 has a nice 1-d analysis of how this works
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Explosion of new coronagraph ideas in recent years • Lyot family:
– Basic: Lyot 1939 MNRAS 99, 538; Sivaramakrishnan et al 2001 – Band-limited: Kuchner & Traub 2003 – Apodized: Soummer 2005 Ap.J. 618, L161
• Apodizers: – Shaped-pupil: Kasdin et al 2003, Kasdin et al 2005 Applied Optics
44 1177, etc. – Phase-induced apodizer: Guyon et al 2005 Ap.J. 622, 744
• Interference / wave-optics – 4-quadrant phase mask: Rouan et al 2000 PASP 777 1479 – Nulling interferometer/coronagraphs: Mennesson et al. 2004 Proc.
SPIE 4860, 32
• Optical Vortex Coronagraphs
• Most practical coronagraphs only work at > 3-5 λ/D
• Control of phase errors is as important as controlling diffraction
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Page 23 Phase
Spatial frequency
Power spectrum
Spatial frequency
Spatial frequency
NO CORONAGRAPH CORONAGRAPH
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Shaped-pupil coronagraphs (Kasdin et al. 2003)
Pupil PSF
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WFS measurement
Inner working distance ~ 3-5 λ/D
Fitting error
Outer working distance ~ N λ/D
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Random intensity of all the Fourier components produces speckles
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As speckles average out (t ~ D/vwind) planets can be detected
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Must get rid of static errors as well
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ExAO 0 nm static errors, 5 MJ/500 MYr planet, 15 minute integration
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ExAO 1 nm static errors, 5 MJ/500 MYr planet, 15 minute integration
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ExAO 2 nm static errors, 5 MJ/500 MYr planet, 15 minute integration
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ExAO 5 nm static errors, 5 MJ/500 MYr planet, 15 minute integration
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Schematic of Gemini Planet Imager
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Comparison of original Keck AO and GPI AO parameters
Keck AO (1999) GPI (2010)
Deformable mirror 349 actuators(240 active)
4096 actuators(1809 active)
Subaperture 56 cm 18 cm
Control rate 670 Hz 2000 Hz
Wavefront sensor Shack-Hartmann400 – 1000 nm
Spatially-filtered Shack-Hartmann700-900 nm
Strehl @ 1.65 mm 40% > 90%
Guide star mag(NGS only)
R < 13.5 mag. I < 9 mag. ( V < 11)
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GPI Integral field spectrograph (James Larkin, UCLA)
Detector Lenslet Array
Collimator Optics Camera Optics
Focal Plane
Pupil Plane
Rotating ColdPupil Stop
Filters
R.I. TelephotoCamera
Lenslet
Spectrograph
Collimated lightfrom Coronagraph
Prism
Window
Low spectral resolution (R~50)
High spatial resolution (0.014 arcsec)
Wide field of view (3x3 arcsec)
Minimal scattered light
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Data pipeline assembles cubes: image of planet as function of wavelength
Christian Marois, HIA
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GPI mechanical design
GPI enclosure
Electronics
Gemini Cassegrain support structure
Optics structure
Gort
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Inner working distance (IWD) ~2-4 l/D
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Extrasolar planets
H=8-11 mag
H=5-8 mag
H=4-6 mag
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Directly imaged planets: HR 8799 System
Marois and colleagues, Gemini and Keck
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HR 8799: greater contrast with parent star at 3.3 microns
Hinz and colleagues, LBT
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Beta Pictoris b: a planet within a disk
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51 Eri b: from GPI (Macintosh et al. 2015)
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ROXs 42b (Currie et al. 2015)
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References, part 1
Angel, R, “Ground based imaging of extrasolar planets using adaptive optics’, 1994 Nature 368, 203 (Original exoplanet paper)
Burrows, A., et al., “A nongray theory of extrasolar planets and brown dwarfs”, 1997 Ap.J 491, 856 (Planet models)
Sivaramakrishnan, A., et al., “Ground-based coronagraphy with High-Order Adaptive optics”, 2001 Ap.J. 552, 397 (Lyot coronagraphs)
Kasdin, N.J., et al, 2003, “Extrasolar planet finding via optimized apodized pupil and shaped pupil coronagraphs”, Ap.J. 582, 1147
Kuchner, M, and Traub, W., “A Coronagraph with a Band-limited Mask for Finding Terrestrial Planets” 2002 Ap.J. 570, 200 (improved Lyot coronagraph)
Sivaramakrishnan, A., et al, “Speckle decorrelation and dynamic range in speckle noise limited imaging”, 2002 Ap.J. 581, L59 (2nd-order PSF expansion)
Perrin, M., et al. “The structure of the High Strehl Ratio Point-Spread Functions”, 2003, Ap.J. 596, 702 (high-order PSF expansion)
Poyneer, L, and Macintosh, B., “Spatially-filtered wavefront sensor for high-order adaptive optics”, 2004, JOSA A 21, 810 (aliasing + WFS)
Guyon, O., et al. “Theoretical Limits on Extrasolar Terrestrial Planet Detection with Coronagraphs”, 2006 Ap.J.S. 167, 81
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References, part 2
LaFreniere, D., et al., “A new algorithm for point-spread function subtraction for high-contrast imaging”
Macintosh, B., et al, “The Gemini Planet Imager: From Science to Design to Construction”, 2008 Proc. SPIE 7015-18
Marois, C., et al., 2000, “Efficient Speckle Noise Attenuation in Faint Companion Imaging”, 2000 Proc. SPIE 767, 91
Marois, C., et al., 2006, “Angular Differential Imaging: A Powerful High-Contrast Technique”, 2006 Ap.J. 6541, 556
Marois, C., Macintosh, B., Barman, T., et al, “Direct Imaging of Multiple Planets Orbiting the Star HR8799”, 2008 Science 5906, 1348
Poyneer, L., Macintosh, B., and Veran, J-P., “Fourier transform wavefront control with adaptive prediction of the atmosphere”, 2007 JOSA A 24, 2645
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