HIGH RESOLUTION & CONTRAST Imaging F. Pedichini. PARSEC: 3.26 ly 1 Pc 3 Pc 1 A.U. 1 arcsec 2 arcsec.
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Transcript of HIGH RESOLUTION & CONTRAST Imaging F. Pedichini. PARSEC: 3.26 ly 1 Pc 3 Pc 1 A.U. 1 arcsec 2 arcsec.
![Page 1: HIGH RESOLUTION & CONTRAST Imaging F. Pedichini. PARSEC: 3.26 ly 1 Pc 3 Pc 1 A.U. 1 arcsec 2 arcsec.](https://reader036.fdocument.pub/reader036/viewer/2022062307/551a8f68550346b52d8b5d31/html5/thumbnails/1.jpg)
HIGH RESOLUTION & CONTRAST
Imaging
F. Pedichini
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PARSEC: 3.26 ly
1 Pc
3 Pc
1 A.U.1 A.U. 1 A.U.1 A.U.
1 arcsec
2 arcsec
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EXO_Planets @ 10 pc
5 A.U.
3 A.U.
1 A.U.
10 pc100 mas
500 mas
300 mas
1rad = 206265 arcsec[1 mas = 1e-3 arcsec]
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Airy disc @ telescope [mas] :
1.22λ/D
Lambda [µm] Mirror 0.1 Mirror 1.0 Mirror 10 Mirror 40 Mirror 100
0.35 880 88 8.8 2.2 0.8
0.65 1634 163 16.3 4.0 1.6
2.5 6284 628 62.8 15.7 6.3
10 25136 2513 251.3 62.8 25.13
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Airy disc @ 8.2 m, high contrast:
Sun flux @ 10pc = 1.5e9 γ/s [R band]
[mas]
Peak normalized flux
1.22λ/D @ 630 nm ~ 18 mas
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Sun flux @ 10pc = 1.5e9 γ/s [R band]
Jupiter flux @ 10pc, 5A.U. = 5.0 γ/s [R band]
Jupiter flux @ 10pc, 1A.U. = 125 γ/s Jupiter flux @ 10pc, 0.5A.U. = 600 γ/s
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Planet contrast vs Sun distance:
[mas]
Diffraction profile for 8.2 m telescope
3e-2
8e-3
8e-4
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Detection is not Contrast !
𝑆𝑁𝑏
(𝑡)=𝑆 ∙𝑡
√(𝑆+𝑏 ) ∙ 𝑡+𝑅𝑂𝑁S/N is intrinsic in photon statistics
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Detection is not Contrast (the Math) !
( 𝑆𝑁 )𝑓
∝𝑓 ∙𝑡𝑒𝑥𝑝
√ 𝑓 ∙𝑡𝑒𝑥𝑝+𝑅𝑂𝑁2;
⇓
𝑁∝√𝑆 ;𝑆𝑡𝑎𝑟 +𝑝≅ 𝑆𝑡𝑎𝑟 ;
( 𝑆𝑁 )𝑝
∝𝑝 ∙𝑡𝑒𝑥𝑝
√𝑆𝑡 𝑎𝑟 ∙ 𝑡𝑒𝑥𝑝+𝑅𝑂𝑁 2⟹𝑝 ∙√ 𝑡𝑒𝑥𝑝
𝑆𝑡𝑎𝑟
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Airy profile flux normalized
Detection !texp[s] 0.5 A.U. 1 A.U. 5 A.U.
1 707 223 22
10 2236 707 71
100 7071 2236 224
1000 22360 7071 707
Sun flux @ 10pc = 1.5e9 γ/sJupiter flux @ 10pc, 5A.U. = 5 γ/s
Jupiter flux @ 10pc, 1A.U. = 125 γ/s
𝒏𝒐𝒊𝒔𝒆=√𝒔𝒖𝒏𝒇𝒍𝒖𝒙 (𝑨 .𝑼 .) ∙𝒕𝒆𝒙𝒑
1 10 100 10001
10
100
1000
10000
100000
1000000
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Texp [s]
Flux , noise [γ]
5 A.U.
0.5 A.U.
1 A.U.
Detection !
1 10 100 10001
10
100
1000
10000
100000
1000000
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Terra, terra….
Jupiter
𝑟𝐽𝑟𝑇
≅ 10⟹10− 2 𝑓𝑙𝑢𝑥
mag=5
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Simple telescope optics:
PUPIL plane
IMAGE plane IMAGE plane
PUPIL plane
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Less Simple telescope optics:
PUPIL plane
IMAGE plane IMAGE plane
PUPIL plane
OCCULTING DISK
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Lyot Coronagraph telescope optics:
PUPIL plane
IMAGE plane IMAGE plane
PUPIL plane
OCCULTING DISK
LYOTSTOP
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Lyot Coronagraph gain 100 in contrast:
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Coronagraph !texp[s] 1 A.U. 5 A.U. Terra 1A.U.
1 87 4 1.25
10 274 12 12.5
100 866 39 125
1000 2739 122 1250
Sun flux @ 10pc = 5e9 γ/sJupiter flux @ 10pc, 5A.U. = 5 γ/s
Terra flux @ 10pc, 1A.U. = 1.3 γ/s
√𝒔𝒖𝒏𝒇𝒍𝒖𝒙 (𝑨 .𝑼 .)
1 10 100 10001
10
100
1000
10000
100000
1000000
𝒏𝒐𝒊𝒔𝒆=√𝒔𝒖𝒏𝒇𝒍𝒖𝒙 (𝑨 .𝑼 .) ∙𝒕𝒆𝒙𝒑
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Texp [s]
Flux , noise [γ]
5 A.U.
1 A.U.
Coronagraph Detection
1 10 100 10001
10
100
1000
10000
100000
1000000
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Lyot gaussian Coronagraph gain ~1e4 in contrast:
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NO OBSTRUCTION
SECONDARY 11%OBSTRUCTION
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Seeing @telescope:
ℱ (𝑟 )=𝑒−( 𝑟𝜃 )𝛾
𝛾≅ 2 𝜃=𝐹𝑊𝐻𝑀2.3 𝐹𝑊𝐻𝑀≫600𝑚𝑎𝑠
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Detection; FWHM size is crucial !
r=25 r=15 r=10
r=5
Noise levelr.m.s. 33
Integral Signal10000
S/N=4S/N=34
S/N=1S/N=17
S/N=0.5S/N=11S/N=6
S/N=?
S/N [peak]S/N [integral]
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Seeing @ 8.2 m, low contrast:
Flux normalized to 1
[mas]
600 mas FWHM seeing
Airy profile
Seeing profile FWHM=1”
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Strehl, Kolmogorov and Marechal:
𝑆=𝑒−(2 𝜋𝜎 (𝐶𝑛❑
2 )
𝜆 )2
𝜎=0 ;𝑆=1 𝜎=107 ;𝑆=0.32
𝜆=630 [𝑛𝑚 ] 𝜆=630 [𝑛𝑚 ]
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the Large Binocular Telescope• Aperture diameter [m] 2 x 8.4 (f# 15)• Wavelenght [µm] 0.32 ÷ 10• Mount control Alt-Az on oil pad• Lens profile error[nm] <50 (active and adaptive optic )• Image blurring [arcsec] 0.3 ÷ 0.9 (0.015 diff. limit)• Adaptive optics facility embedded in the secondary mirror• Location Mount Graham (Arizona) 3200 m
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the Large Binocular Telescope
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Adaptive Optics basic:MTF
N.C.P.A.
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Experimental PSF (LBT FLAO results):
H band[1.6µ]
Esposito et al. SPIE 2011
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Strehl vs guide star (LBT FLAO results):
Esposito et al. SPIE 2011
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HIP76041 750nm-10nm seeing 1” 600 modino optics -> scale = 7.2mas/pix
Ghost
E. Pinna, priv. com.
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HR 8799 infrared light from ExoPlanets:
Esposito et al. A&A 549, 2013
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PSF reconstruction… where are the planets here ?
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Theoretical limit for 8.2m @ 650nm(texp 3600 s + A.O. σ 80 nm + Lyot-coro)
10 pc 5 pc
1 J
4 J
10 J
50 J
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Angular Differential Imaging:RA = 0° RA = 20° RA = 45°
PA = 0° PA = 20° PA = 45°
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V-SHARK-Forerunner: 600nm A.O. at 1600 f.p.s. (goal 16÷17 mas. resolution)
Io moons of Jupiter
Simulated image of
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X
Y
Z
V-SHARK CORONAGRAPH optical layout
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V-SHARK in 3d:
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Hot Stuff (Advanced Adaptive Optics)
Adaptive Optics can work at visible; running fast,saving the errors and doing blind de-convolution you get this…!
Courtesy of S. Jefferies (Maui Air Force Lab)
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No A.O. at 1.2m telescope!
Applied Optics, Vol. 48, Issue 1, pp. A75-A92 (2009)http://dx.doi.org/10.1364/AO.48.000A75
Courtesy of S. Jefferies (Maui Air Force Lab)
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Is this possible….?
880 nm3.6 meter telescope1.22 λ/D = 61mas
10 cm @ 560 km = 36mas
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Next future LBTI vs EELT:
21 m baseline2 x 1000÷4000 actuators
Ro=13÷6 cm
37 m baseline4000 actuators
Ro=30 cm
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NGS vs LGS :
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che la Forza sia con Voi !
grazie per l’attenzioneCourtesy of D. Bonaccini (ESO)