Lecture 12: Revision Flashcards

(24 cards)

1
Q

star

A

point source at infinity

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2
Q

plane-parallel waves brought to focus to

A

form image of star

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3
Q

aperture does not cover entire wavefront radiated by star - leads to

A

diffraction at apperture

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4
Q

angular resolution

A

a=1.22 lambda/D

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5
Q

actual image is

A

the convolution of the ideal image predicted by geometrical optics with the PSF

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6
Q

strehl ratio

A

I_psf(0) / I_airy(0)

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7
Q

planar wavefronts from the distant source are distorted by

A

turbulent layers of the atmosphere

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8
Q

phase variation across wavefront described by

A

phase structure function D(r)

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9
Q

by applying Kolomogorv model, one can derive the

A

dependence of the structure function on atmospheric parameters, specifically structure parameter Cn^2

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10
Q

Cn^2 characterises

A

the strength of fluctuations in refractive index

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11
Q

knowing phase structure function, can derive

A

the optical transfer function of the atmosphere

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12
Q

taking inverse FT of OTF

A

point spread func due to atmos

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13
Q

fried parameter

A

indication of the strength of phase fluctuations

integrate CN^2 wrt height

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14
Q

atmospheric seeing

A

angular size of PSF due to atmos

B=0.98 lambda /ro

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15
Q

guide stars

A

reference source of light within the isoplanatic patch
theta0=r0/h

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16
Q

sodium beacon

A

laser light used to excite sodium atoms in the upper atmos

17
Q

strehl ratio used to quantify

A

the performance of an adaptive optics system

18
Q

in corrected images,, what can be used

A

marechal approx
s approx e^-<E^2>

19
Q

marechal approx allows one to

A

predict strehl ratio from known errors in wavefront sensing scheme

20
Q

total residual phase variance is equal to

A

the sum of phase variances from all sources

21
Q

etendue equ

A

G approx A omega

22
Q

etendue remains

A

unchanged as light is transformed by lenses, mirrors, apertures etc

23
Q

width of entrance slit

A

delta xi

= dx/dlambda dleta lambda_bp

linear disp x bandpass