key types introduction
DESCRIPTION
Key Types Introduction. Wesley A. Traub Harvard-Smithsonian Center for Astrophysics. Michelson Summer School on High-Contrast Imaging Caltech, Pasadena 20-23 July 2004. Reminders of main topics. C, IWA, OWA types perturbations. C. K~20 mag Bkgd objects. 7 arcsec wand. J~21 mag - PowerPoint PPT PresentationTRANSCRIPT
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Key Types Introduction
Michelson Summer School on High-Contrast Imaging
Caltech, Pasadena
20-23 July 2004
Wesley A. TraubHarvard-Smithsonian Center for Astrophysics
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• C, IWA, OWA• types• perturbations
Reminders of main topics
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C
Ref: McCarthy & Zuckerman (2004); Macintosh et al (2003)
20 arcsec radius circle
K~20 magBkgd objects
7 arcsec wand
J~21 magBkgd object
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Search space: best to date
AiryHalo
1. Keck2. IRCAL, Lick AO, K3. Ks, AO, NACO, VLTI4. WFPC2, HST, I5. CFHT, AO, H6. Keck NICMOS, 10sig7. 50% det, HST, H8. XAO, 10m, R, 2007
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Earth & Jupiter-Saturn, 100 stars
Simulations by Bob Brown, STScI
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Earth & Jupiter-Saturn Regions
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Radial-velocity Stars
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RV stars and brown dwarfs
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1.8-m range
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TPF-C Range
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C, IWA, OWA
Contrast C: Example: C = 10-10 driven by Earth/Sun = 2x10-10.
Inner working angle IWA:Example: IWA = 3 /D driven by 1 AU/10pc = 0.100 arcsec.
Outer working angle OWA: Example: OWA = 48 /D driven by N = 96 actuator DM.
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Image-plane coronagraph simulation
Ref.: Pascal Borde 2004
1stpupil
1stimagewithAiry rings
mask, centered on starimage
2ndpupil
Lyotstop,blocks bright edges
2nd image,no star,brightplanet
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Wide-band (quadrant-phase) mask
€
π€
π
€
0
€
0
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Shaped-pupil mask
Kasdin, Vanderbei, Littman, & Spergel, preprint, 2004
Pupil: Spergel-Kasdin prolate-spheroidal mask
Image: dark areas < 10-10 transmission
Image: cut along the x-axis
v
u
A(x, 0) = exp(-(πx/)2)
A(0, y) = periodic & messy
x
y
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Discrete-mapped pupil (2): Densification
Entrance pupil, sparsely filled
FOV is small.
Image with many aliases Densified
pupil
Clean image,narrow FOV
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Continuous-mapped pupil
Compact star image, easily blocked
Input wavefront: uniform amplitude.
Mirror 1
Mirror 2
Output wavefront:prolate-spheroidal amplitude.
100 dB = 10-10 = 25 mag
Output image:prolate spheroid
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Nulling-shearing coronagraph
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Phase ripple and speckles
No DM:
With DM:
Phase ripples from primarymirror errors
Polishing errorson primary
Speckles generated by 3 sinusoidalcomponents of thepolishing errors
Pupil plane
Image plane
Image plane
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Phase + amplitude ripple and speckles h(u) = n (an+ian')cos(Knu) + (bn+ibn')sin(Knu) = total ripples
Describes all possible phase and amplitude ripples (= errors).
DM can give
I() = (0) + n [(bn’)2 + (an’)2 ] (k+Kn) bigger speckles
+ [ 0 + 0 ] (k-Kn)] smaller (zero) speckles