HIGH RESOLUTION & CONTRAST Imaging F. Pedichini

PARSEC: 3.26 ly 1 Pc 3 Pc 1 A.U. 1 arcsec 2 arcsec

10 pc 5 A.U. 3 A.U. 1 A.U. 10 pc 100 mas 500 mas 300 mas 1rad = arcsec [1 mas = 1e-3 arcsec]

Airy telescope [mas] : 1.22λ/D Lambda [µm]Mirror 0.1Mirror 1.0Mirror 10Mirror 40Mirror

Airy 8.2 m, high contrast: Sun 10pc = 1.5e9 γ/s [R band] [mas] Peak normalized flux 630 nm ~ 18 mas

Sun 10pc = 1.5e9 γ/s [R band] Jupiter 10pc, 5A.U. = 5.0 γ/s [R band] Jupiter 10pc, 1A.U. = 125 γ/s Jupiter 10pc, 0.5A.U. = 600 γ/s

Planet contrast vs Sun distance: [mas] Diffraction profile for 8.2 m telescope 3e-2 8e-3 8e-4

Detection is not Contrast !

Detection is not Contrast (the Math) !

Airy profile flux normalized Detection ! texp[s]0.5 A.U.1 A.U.5 A.U Sun 10pc = 1.5e9 γ/s Jupiter 10pc, 5A.U. = 5 γ/s Jupiter 10pc, 1A.U. = 125 γ/s

Texp [s] Flux, noise [γ] 5 A.U. 0.5 A.U. 1 A.U. Detection !

Terra, terra…. Jupiter

Simple telescope optics: PUPIL plane IMAGE plane PUPIL plane

Less Simple telescope optics: PUPIL plane IMAGE plane PUPIL plane OCCULTING DISK

Lyot Coronagraph telescope optics: PUPIL plane IMAGE plane PUPIL plane OCCULTING DISK LYOT STOP

Lyot Coronagraph gain 100 in contrast:

Coronagraph ! texp[s]1 A.U.5 A.U.Terra 1A.U Sun 10pc = 5e9 γ/s Jupiter 10pc, 5A.U. = 5 γ/s Terra 10pc, 1A.U. = 1.3 γ/s

Texp [s] Flux, noise [γ] 5 A.U. 1 A.U. Coronagraph Detection

Lyot gaussian Coronagraph gain ~1e4 in contrast:

NO OBSTRUCTION SECONDARY 11% OBSTRUCTION

Detection; FWHM size is crucial ! r=25r=15r=10 r=5 Noise level r.m.s. 33 Integral Signal S/N=4 S/N=34 S/N=1 S/N=17 S/N=0.5 S/N=11 S/N=6 S/N=? S/N [peak] S/N [integral]

8.2 m, low contrast: Flux normalized to 1 [mas] 600 mas FWHM seeing Airy profile Seeing profile FWHM=1”

Strehl, Kolmogorov and Marechal:

the Large Binocular Telescope Aperture diameter [m]2 x 8.4 (f# 15) Wavelenght [µm]0.32 ÷ 10 Mount controlAlt-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 LocationMount Graham (Arizona)3200 m

the Large Binocular Telescope

Adaptive Optics basic: MTF N.C.P.A.

Experimental PSF (LBT FLAO results): H band[1.6µ] Esposito et al. SPIE 2011

Strehl vs guide star (LBT FLAO results): Esposito et al. SPIE 2011

HIP nm-10nm seeing 1” 600 modi no optics -> scale = 7.2mas/pix Ghost E. Pinna, priv. com.

HR 8799 infrared light from ExoPlanets: Esposito et al. A&A 549, 2013

PSF reconstruction… where are the planets here ?

Theoretical limit for 650nm (texp 3600 s + A.O. σ 80 nm + Lyot-coro) 10 pc 5 pc 1 J 4 J 10 J 50 J

Angular Differential Imaging: RA = 0°RA = 20°RA = 45° PA = 0°PA = 20°PA = 45°

V-SHARK-Forerunner: 600nm A.O. at 1600 f.p.s. (goal 16÷17 mas. resolution) Io moons of Jupiter Simulated image of

V-SHARK CORONAGRAPH optical layout

V-SHARK in 3d:

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)

No A.O. at 1.2m telescope! Applied Optics, Vol. 48, Issue 1, pp. A75-A92 (2009) Courtesy of S. Jefferies (Maui Air Force Lab)

Is this possible….? 880 nm 3.6 meter telescope 1.22 λ/D = 61mas km = 36mas

Next future LBTI vs EELT: 21 m baseline 2 x 1000÷4000 actuators Ro=13÷6 cm 37 m baseline 4000 actuators Ro=30 cm

NGS vs LGS :

che la Forza sia con Voi ! grazie per l’attenzione Courtesy of D. Bonaccini (ESO)