An Exoplanet Coronagraph on a Stratospheric Science Platform
Application of Coronagraph for Beam halo observation In ...
Transcript of Application of Coronagraph for Beam halo observation In ...
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Application of Coronagraphfor
Beam halo observation In the SuperKEKB
T. Mitsuhashi, KEK
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Everything was start with astronomer’s dream……
Eclipse is rare phenomena, and only few second is available for observation of sun corona, prominence etc.
Artificial eclipse was dream of astronomers, but……..
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The eclipse Inside umbra : total eclipsePenumbra : Partial eclipse
3.84 x 105 km
1.49 x 108 km
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Why we can see the sun corona by eclipse without diffraction fringe?
Because no aperture between sun and moon.It means no strong diffraction source in eclipse.
The area of umbra>>>diameter of objective lens
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Why we can see the sun corona by eclipse without diffraction fringe?
Because no aperture between sun and moon.It means no strong diffraction source in eclipse.
Question is can we make same system with artificial way?
The area of umbra>>>diameter of objective lens
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Diffraction source aperture is in here.
Compare two setup, eclipse and artificial eclipse.
Diffraction source aperture is in here.
The area of umbra>>>diameter of aperture of objective lens
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Diffraction source aperture is in here.
How to eliminate diffraction fringe from aperture.
Diffraction source aperture is in here.
A strong diffraction fringes are surrounding of the image
The area of umbra>>>diameter of objective lens
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Diffraction fringesGaussian profile
Convolution between diffraction fringes and object profile
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Diffraction fringesGaussian profile
Convolution between diffraction fringes and beam profile
Blocked by opaque disk
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The coronagraph to observe sun corona
Developed by B.F.Lyot in 1934 for a observation of sun corona by artificial eclipse.
Special telescope having a “re-diffraction system” to eliminate a diffraction fringe.
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Optical system of Lyot’s corona graph
Objective lens
Field lens
Baffle plate (Lyot stop)
Relay lens
Opaque disk
Anti-reflection disk
Baffle plates to reduce reflection
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3 stages-optical system in the Lyot’scoronagraph
1st stage : Objective lenssystem
2ed stage : re-diffractionsystem
3ed stage :Relay lens
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Re-diffraction optics system to eliminate the diffraction fringe
Detail of the diffraction theory of coronagraph, please see appendix 1
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Opaque disk
Objectivelens
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Opaque disk
Lyot stop
Re-diffractionoptics systemOpaque disk
Field lens
ObjectivelensRe-diffraction optical system
Function of the field lens : make a image of objective lens aperture onto Lyotstop
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Geometrical image of the aperture of objective lens
Intensity distribution of diffraction fringes on focus plane of field lens
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Block the re-diffraction fringes
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Lyot stopBlocking diffraction fringe by
Relay of corona image to final focus point
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Background in classical coronagraph
Re-diffraction intensity on the Lyot stop
Diffraction fringe exists here
This leakage of the diffraction fringe can make background level 10-6-8 (depends on Lyot stop condition).
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Diffraction background at 3ed stageIn Log scale 2x10-6 to 10-7
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Background source in coronagraph
1.Scattering by defects on the lens surface (inside) such as scratches and digs.
2. Scattering from the optical components (mirrors) near by coronagraph.
3. Reflections in inside wall of the coronagraph.
4. Scattering from dust in air.
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1.Scattering by defects on the lens surface (inside) such as scratches and digs.
2. Scattering from the optical components (mirrors) near by coronagraph.
3. Reflections in inside wall of the coronagraph. Cover the inside wall with a flock paper (light trapping material).
4. Scattering from dust in air. Use the coronagraph in clean room.
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Scattering from the optical components (mirrors) in
the coronagraph
Dtail of this subject ,please see appendix 2
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d0 di
P(x, y): pupil function with assembly of diffraction noise sources on the lens
Case 1. Noise source in the entrance pupil of
objective lens
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Digs on glass surface of scratch & dig 60/40The optical surface quality 60/40 guarantees no larger scratches than 6μm width, and no larger dig than 400μm.
5mm
200μm
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400μm200μm
100μm
50μm
Diffraction by objective lens aperture
Simulation result of Background produced by dig on objective surface
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400μm200μm
100μm
50μm
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Comparison between normal optical polish and careful optical polish for coronagraph
S&D 60/40 surface of the lens Surface of the coronagraph lens
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Scattering from the optical components (mirrors) between source point and coronagraph.
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da did0
U0 Ua Ul U’l UiU’aPa Pl
Noise source to objective lens Fresnel like diffraction Then this input is re-diffracted by objective lens pupil
da is shorter : out of focus image of noise source +Fresnel like diffractionda is longer : quasi-focused image of noise source +Fraunhofer like diffraction
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Intentionally spread some dust on the mirror in 2m front of the coronagraph
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Scattering background from mirrors near by coronagraph will not acceptable!
Use same quality of optical polishing for mirrors! Clean optical elements are necessary for optical beam transport line.
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Observation of beam halo at the Photon Factory, KEK
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Beam profile
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Beam halo
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Observation inPF,KEK 2005Beam core (superimposed) + haloObservation with better than 6 order of magnitude
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65.8mA 61.4mA 54.3mA
45.5mA 35.5mA 396.8mAMulti-bunchbunch current 1.42mA
Beam tail images in the single bunch operation at the KEK PF measured at different current
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Single bunch 65.8mAExposure time of CCD : 3msec
Exposure time of CCD : 100msec
Intensity in here : 2.05x10-4
of peak intensity
2.55x10-6
Background leavel : about 6x10-7
Halo in deep outside
Observation for the more out side
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Coronagraph for SuperKEKB
1. Optical design
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Optical configuration of SR monitor line in SuperKEKB total optical path=60m
Polycrystal Diamond extraction mirror 20mm x 30mm
Coronagraph objective
Mirrors D=150mm
Mirrors D=150mm
23.6m 0.7m 1.3m 9.9m
4.5m 14.5m 3.3m 3m 0.5m
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Optical configuration of SR monitor line in SuperKEKB
Polycrystal Diamond extraction mirror 20mm x 30mm
Coronagraph objective
Mirrors D=150mm
High quality Mirrors D=150mm will replace in future
24m 0.3m 1.3m 7.5m
7.5m 12m 5m 3m 0.5m
Aperture here
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Design of the objective1. Due to diffraction theory of the coronagraph, leakage background in 3ed stage is roughly proportional to transverse magnification of the objective system.Large transverse magnification will necessary
long focal length
2. Diamond mirror aperture must set at the front principal point of Objective
Use the telephoto system
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Detail of optical design of telephoto-objective system,Please see appendix 3
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Optical design of Gregorian system for SuperKEKB
R2=-410mmC.P.=-0.502
R1=2400mmC.P.=-1
M2=1440mm
M1=240mm
Bf= -34.3mm
Gregorian extension ratio=5.857
mm70282
RMf 1 ==
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Magnification=0.574Distance between H and H’ is 24608mm
ff=7028X=12235 X’=4037
h h’
H H’
ff=7028
54936
24608
Relation of conjugation points (between source point and beam image)
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Relation between source point and beam image
ff=7028X=12235 X’=4037
h h’
H H’
ff=7028
54936
24608
Set diamond mirror aperture at here
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Designed magnification 0.574Measurement 0.606Error is about 5% Majority source should be Focal length error (2% each) and distance error.
Wonderful agreement!
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Observed beam image and diffraction fringes
Higher order fringes are clealy observed
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35.6m
2ed stage, Re-diffraction system
Big problem is long distance between aperture and field lens
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Design of re-diffraction system
35.6m
Big problem is long distance between aperture and field lensDifficult to obtain enough size of aperture image on Lyot stop!
Lyot stop
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Use Kepler system for obtain enough magnification
Expected problemFocusing system has all + , +, + powerEnhancing the aberrationEspecially for field flatness
35.6mF=500mm High-quality Apochromat
F=50mm3 groups, 5 lenses
Lyot stop
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Observation Graphical indication of double peaked diffraction pattern
Diffraction image on Lyot stop
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Adding 3ed stage,Relay optics
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F=250mm High-quality Apochromat
35.6m
F=500mm F=50mmLyot stop
Lyot stop
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Results of observation from last operation
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Stored beam with total optics
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5mm opaque disk is applied
2 x 10-2
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Close horizontal Lyot stop
vertical Lyot stop is slightly closed
2.8 x 10-4
6,6 x 10-6
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Scattering noise or something beam origin??
Stored beam (superimposed)
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Conclusions1. We design Gregorian objective
having a diffraction limited quality for SuperKEKB.
2. A Kepler type re-diffraction system is applied.
3. With third relay system, we got beam image and we established basic function of coronagraph with Lyot stop (elimination of diffraction fringe).
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ProblemsKepler style re-diffraction system enhanced the field distortion.Difficult to reach more large transverse magnification in total system.Difficult to further elimination of diffraction fringe.
To solve these problems, Galileo type re-diffraction system will test in next operation
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Galileo type re-diffraction system
Focusing system has all + , +, - power
35.6m
Lyot stop
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Learned from SuperKEKB
1. High quality (low noise) Optical beam line is necessary to coronagraph.
2. New polycrystal Diamiond mirror can establish perfect wavefront transfer withour significant distortion.
3. Using Gregorian objective, we can optimize coronagraph design for long optical beam line (60m in the Super KEKB).
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Application of coronagraph objective for turn by turn
observation of injected beam profile
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Appendix 1
Diffraction theory for the Coronagraph
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Opaque disk
Objectivelens
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( ) ( ) ( )
21
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Instantaneous diffraction pattern at focus point of Objective lens is given by,
Apparent diffraction pattern on focus point is given by integrating instantaneous diffraction pattern in incoherent manner , ( ) ( ) θθ d ,y,xy,x objobjobjobj = 2FIobj
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Opaque disk
Lyot stop
Re-diffractionoptics systemOpaque disk
Field lens
ObjectivelensRe-diffraction optical system
Function of the field lens : make a image of objective lens aperture onto Lyotstop
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ξ1
ξ2
The integration performs ξ1 and ξ1
ξ1: radius offield lens
ξ2: radius ofopaque disk
Field lens diffraction
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ξ
⋅λξ⋅⋅π⋅⋅−ξ
⋅λ⋅=
ξ
⋅λξ⋅⋅π⋅⋅−ξ+ξ
⋅λξ⋅⋅π⋅⋅−ξ
⋅λ⋅=
ξ
⋅λξ⋅⋅π⋅⋅−ξ−ξ
⋅λξ⋅⋅π⋅⋅−ξ
⋅λ⋅=
ξ
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df
xiexp)(Ffi
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Disturbance of light on Lyot’s stop by re-diffraction system is given by;
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Geometrical image of the aperture of objective lens
Intensity distribution of diffraction fringes on focus plane of field lens
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Corse period correspond to inner aperture diameter
Fine period correspond to outer aperture diameter
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0.162mm
0.6mm
1.0mm
dependence of diffraction width for different diameter of oparque disk
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diffraction fringe on Lyot stop
0.162mm
0.6mm
1.0mmLarger opaque disk has small diffraction widthEasy to eliminate
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Block the re-diffraction fringes
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Lyot stopBlocking diffraction fringe by
Relay of corona image to final focus point
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ξ1
The integration performs η1
η1: radius ofLyot stop
Relay lens diffraction
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dxx2iexp)x(ui
1)(V1
0φ
⋅λ⋅φ⋅π⋅⋅−
⋅λ⋅=φ
relayrelay ff
Disturbance of light on final focus point V(x) is given by;
U(x) is still not 0 inside of relay lens pupil!
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Background in classical coronagraph
Re-diffraction intensity on the Lyot stop
Diffraction fringe exists here
This leakage of the diffraction fringe can make background level 10-8 (depends on Lyot stop condition).
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Diffraction background at 3ed stageIn Log scale 2x10-6 to 10-7
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Appendix 2
Mie scattering,
it’s diffraction treatment
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d0 di
P(x, y): pupil function with assembly of diffraction noise sources on the lens
Case 1. Noise source in the entrance pupil of
objective lens
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Digs on glass surface of scratch & dig 60/40The optical surface quality 60/40 guarantees no larger scratches than 6μm width, and no larger dig than 400μm.
5mm
200μm
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( ) ),,(,, 00 iii yxrcircyxrP =
Let us approximate i-th noise source in the pupil as a opaque disk having a diameter of r0 , Using the Babinet’s principle,
( ) ( ) ( ))(exp,,, ,0 iii
i yxikyxrPyxrP +−⋅=
Then pupil function having many noise source is given by,
i-th noise source which spread in the aperture
=
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When the mean distance of noise source is longer than 1st
order transverse coherent length , pupil function with noise sources is simply given by,
( ) ),,(,, 0 yxrPyxrPi
i=
( ) ( ) ( )[ ]
+++−= dxdyyMyyxMxxd
iyxrPdd
yxyxh iiii
ii 000
002exp),,(1,;,λ
πλ
Then the impulsive response on the image plane is given by,
( )00 ,;, yxyxh ii
in here, M=di /d0 denotes geometrical magnification.
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The intensity of diffraction from noise sources is inverse-proportional to extinction rate,
Extinction rate = entrance pupil aperture area
/ total area of noise source
To escape from noise produced by the objective lens is most important issue
in the coronagraph!!
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Diffraction by objective lens aperture
40μm60μm
80μm
100μm
Simulation result of Background produced by dig on objective surface
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400μm200μm
100μm
50μm
Diffraction by objective lens aperture
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400μm200μm
100μm
50μm
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How to eliminate Mie scattering??
1. A careful optical polishing for the
objective lens.
2. Reduce number of glass surface.
use a singlet lens for the objective lens.
3. No coating (Anti-reflection, Neutral density etc.) for objective
lens
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A careful optical polishing for the objective lens
5mm
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Comparison between normal optical polish and careful optical polish for coronagraph
S&D 60/40 surface of the lens Surface of the coronagraph lens
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da did0
U0 Ua Ul U’l UiU’a
Case 2. Noise source in front of the objective lens
Pa Pl
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da did0
U0 Ua Ul U’l UiU’a
Noise source in front of the lens
Pa Pl
Free space propagation
Fresnel transfer
Lens transfer
Fresnel transfer
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( ) ( ) ( )
( ) ( )
( )
dydxy yx xdkiexp
yx fdd
kiexp y xP
dydxydy
ddyx
dx
ddxikexp
yx ddd
kiexp y xPyxU
lllilii
llil
lll
aaaa
l
aa
a
l
a
aaaa
aaaiii
+−⋅
+
−+⋅
+
−+
+
−−⋅
+
−
−=
22
0
0
0
0
22
0
1112
,
112
,,
After tired calculations,
0ddd here, in al +=
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( ) ( ) ( )
( ) ( )
( )
dydxy yx xdkiexp
yx fdd
kiexp y xP
dydxydy
ddyx
dx
ddxikexp
yx ddd
kiexp y xPyxU
lllilii
llil
lll
aaaa
l
aa
a
l
a
aaaa
aaaiii
+−⋅
+
−+⋅
+
−+
+
−−⋅
+
−
−=
22
0
0
0
0
22
0
1112
,
112
,,
Diffraction by lens pupil
Diffraction by noise sourceAfter tired calculations,
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da did0
U0 Ua Ul U’l UiU’a
Noise source in front of the lens
Pa Pl
Noise source Fresnel diffraction
Then re-diffracted by lens pupil
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da did0
U0 Ua Ul U’l UiU’aPa Pl
Noise source to objective lens Fresnel like diffraction Then this input is re-diffracted by objective lens pupil
da is shorter : out of focus image of noise source +Fresnel like diffraction
da is longer : quasi-focused image of noise source +Fraunhofer like diffraction
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Intentionally spread some dust on the mirror in 2m front of the coronagraph
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Appendix 3
Telephoto system
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Hbfb
Two kinds of telephoto lens
No.1
Hbfb
No.2
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Where is front principal point for No.1?Analyze opposite side
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Hf
Retro focus lens
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All together,
Hfff Hb
fb
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Hfff Hb
fb
H’
Hf Hb
ff
Equal to following lens
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Corresponding reflective system is Cassegrain system
Second mirror is hyperbolic
First mirror is parabolic
f1 f2
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Where is front principal point for No.2?Analyze opposite side
fH
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H Hf Hb
fbff
All together,
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Hf Hb
ff
Hf Hb
fbff
Equal to following lens
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Corresponding reflective system Gregory system
F1 F2Second mirror is elliptic
First mirror is parabolic
f2f1
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Difference between Cassegrain and Gregory
f2f1
f1 f2
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Optical design of Cassegrain objective in Supper B factory
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Existing Cassegrain system f=5000mm for streak camera
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R1=2000mm, M=4, Cf=5000mm, R2=500mm1
2
mbfmM +=
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Hf Hb
Fb=5000mmFf=5000mm
21000mm
11000mm
Front focus point
Back focus point
Corresponding conjugation points
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Hf Hb
Fb=5000mmFf=5000mm
21000mm
11000mm
Front focus point
Back focus point
29818mm
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fx'
xf −=
ffX fbX’
h h’
H H’
With geometrical optics
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fx'
xf −=
f = 5000mm
x=9018mm
x’=2772
Transverse magnification=0.554
Using the Newton’s equation,
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M1=400mm
M2=1600mm Bf=7.5mm
R2=1065mmC.P.=-2.680
R1=4000mmC.P.=-1.0
Optical design of Cassegrenobjective in Super B factory
Cassegrain focal length=8038mmCassegrain extension ratio=4.018
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カセグレンsuperB07.ZMXコンフィグレーション 1 / 1
3D レイアウト
2019/05/12
X
Y
Z
![Page 126: Application of Coronagraph for Beam halo observation In ...](https://reader033.fdocuments.us/reader033/viewer/2022050214/626e68933e58524a544c9e53/html5/thumbnails/126.jpg)
0 6.8 13.6 20.4 27.2 34 40.8 47.6 54.4 61.2 68
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.0
空間周波数(cycles/mm)
TS 回折限界TS 0.0000, 0.0000 (度)
カセグレンsuperB07.ZMXコンフィグレーション 1 / 1
OTF の絶対値
多色回折 MTF
2019/05/120.5500 から 0.5500 µm までのデータです。面 : 像面
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面 : 像-100 -50 0
<- デフォーカス(µm 単位)->50 100
0.0000, 0.0000 (度) 5.00
カセグレンsuperB07.ZMXコンフィグレーション 1 / 1
スルーフォーカス スポットダイアグラム
2019/05/12 単位は µm です。視野 : 1RMS 半径 : 0.604GEO 半径 : 0.863スケールバー : 5 基準 : 主光線
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ff=8038X=19420 X’=3327
h h’
H H’
Magnification=0.414Distance between H and H’ is 16113mm
ff=8038
54936
Relation between source point and beam image
16113
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Optical design of Gregory system for SuperKEKB
R2=-410mmC.P.=-0.502
R1=2400mmC.P.=-1
M2=1440mm
M1=240mm
Bf= -34.3mm
Gregorian extension ratio=5.857
mm70282
RMf 1 ==
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Hf Hb
Fb=7028mmFf=7028mm 24608mm
Front focus point
Back focus point
Corresponding conjugation points
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Gregorian superB12 fine.ZMXコンフィグレーション 1 / 1
3D レイアウト
2019/05/12
X
Y
Z
![Page 132: Application of Coronagraph for Beam halo observation In ...](https://reader033.fdocuments.us/reader033/viewer/2022050214/626e68933e58524a544c9e53/html5/thumbnails/132.jpg)
面 : 像-100 -50 0
<- デフォーカス(µm 単位)->50 100
0.0000, 0.0000 (度) 5.00
Gregorian superB12 fine.ZMXコンフィグレーション 1 / 1
スルーフォーカス スポットダイアグラム
2019/05/12 単位は µm です。視野 : 1RMS 半径 : 0.011GEO 半径 : 0.020スケールバー : 5 基準 : 主光線
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0 7.8 15.6 23.4 31.2 39 46.8 54.6 62.4 70.2 78
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.0
空間周波数(cycles/mm)
TS 回折限界TS 0.0000, 0.0000 (度)
Gregorian superB12 fine.ZMXコンフィグレーション 1 / 1
OTF の絶対値
多色回折 MTF
2019/05/120.5500 から 0.5500 µm までのデータです。面 : 像面
![Page 134: Application of Coronagraph for Beam halo observation In ...](https://reader033.fdocuments.us/reader033/viewer/2022050214/626e68933e58524a544c9e53/html5/thumbnails/134.jpg)
Magnification=0.574Distance between H and H’ is 24608mm
Relation between source point and beam image
ff=7028X=12235 X’=4037
h h’
H H’
ff=7028
54936
24608