the self-coherent camera: a focal plane wavefront sensor for epics
DESCRIPTION
typical distance : few 10’s mas Context : Exoplanets Exoplanet detection is simple Potter et al., 2002, ApJ HD 130948 d=17.9 pcs 300 Myrs < 75 & 65 MJ @ 50 AU typical distance : few 10’s mas There See faint objects (M 30)TRANSCRIPT
The Self-Coherent Camera: a focal plane wavefront sensor for
EPICS
P. Baudoz R. Galicher, M. Mas, J. Baudrand, G. Rousset, A.
Boccaletti, F. Assemat typical distance : few 10s mas
Context : Exoplanets Exoplanet detection is simple Potter et al.,
2002, ApJ HD d=17.9 pcs 300 Myrs < 75 & 65 MJ@ 50 AU typical
distance : few 10s mas There See faint objects (M 30) Need for High
Contrast Imaging
For Disks : Disk morphology: warp, spirals, offsets, brightness
assymetry, clumps Removing SED ambiguities For Planets : Spectral
characterization Temporal variability (atmosphere) Orbital
parameters EPICS - Planet Finder of the E-ELT
Lessons learned from SPHERE and GPI studies (still to be confirmed)
: If XAO is working as expected (raw contrast 104 to 106) Need
calibration (102 to 103) but limitations: => residual speckles
from static aberrations => residual speckles are chromatic (2nd
order if careful optical design) Need : Phase measurement from
final science focal plane. Need : Separate post-processing data
reduction for each spectral bandwidth Self-Coherent Camera
Instrument Self-Coherent Camera (SCC)
Self-Coherent Camera : Principle Telescope Slow Servo-loop
(quasi-static aberrations) XAO (DM) Self-Coherent Camera (SCC) Beam
splitting Spatial Filter Coronagraph Beam recombining (Fizeau
Fringes) Image Processing Planet Detection Image Simple set-up :
SCC + Four Quadrant Phase Mask coronagraph (FQPM)
= Intensity in focal plane
The SCC in 3 Planes coronagraphic pupil reference pupil D DR a
Pupil plane Optical propagation + Intensity in focal plane FFT
Pupil correlation Plane a The SCC image processing
I- = TF-1[P ** PR ] FFT-1 Ic = I + IR + Iplanet FFT-1 I+ = TF-1[ P
* PR* ] FFT-1 Use I+ to mesure phase (hidden in P ) (I+ is almost a
linear function of for small phase) Focal plane wavefront
sensor(Galicher et al. 2008) Use I+ and Ic to detect Iplanet (Ic
codes I and IR but not Iplanet) Planet detection instrument (not
described here) (Baudoz et al. 2006, Galicher & Baudoz 2007)
Where is the phase in SCC image ?
For coronagraphic image : P = ei - with pupil function and ~1 The
phase is almost a linear function of the imaginary parts With small
phase defects : P = i linear function of P imaginary part real part
Simulation: FQPM +SCC + phase only Is SCC a real wavefront sensor
?
No it is much better than that : It measures directly the complex
amplitude of the field in the focal plane (including amplitude
effects). BUT : Phase estimation at high frequency rate (exposure
time shorter than coherent time) : Not competitive compared to
other WFS (chromaticity) Long exposure time : Blurring of fringes
for the residual speckles after XAO Only static speckles are
fringed. E-ELT (infinite exposure time)
SCC + E-ELT (infinite exposure time) ELT 42m DSP (20 cm pitch -
64nm residual) 10 nm static defects Infinite exposure time +
perfect coronagraph SCC Phase versus time 10 ms 100 ms 1 s 10 s
Static phase
ELT 42m +perfect coronagraph DSP (20 cm pitch - 64nm residual) 10
nm static defects coherent time = 10 ms in H SCC Phase versus time
10 ms 100 ms 1 s 10 s Static phase Noise level in the corrected
area
E-ELT 42m +perfect coronagraph DSP (20 cm pitch - 64nm residual) 10
nm static defects coherent time = 10 ms in H 90% of the corrected
area 0.1 nm level These levels depends linearly on coherent time
(10 ms) and quadratically on residual turbulent level (64 nm RMS) 1
nm level Time evolution 2 layers, only temporal error = 1ms
Fixed aberrations =5 nm 2 layers, only temporal error = 1ms 40x40
actuators, m, L0=20m, V0=10m/s About 35 nm on pupil And if static
are not static
Quasi-static aberrations: fully decorrelated after 20s 4.6 nm
Simulation XAO sampling 1ms Sampling of SCC 1s 0.45 nm 0.25 nm
Limitations 1: Chromatism
1% 2% 5% bandwidth=15% Solution 1: Wynne corrector bandwidth=15%
same +Wynne corrector effective bandwidth =0.75% Solution 2 :
Chromaticity of residual speckles requires spectral resolution SCC
coupled with IFS Limitations 2: Reference Zeroeffect Limitations 3:
Coronagraph effects
FQPM+SCC Matrix Zernikes Zernikes Phase measurement with a
Prototype
FQPM SCC detector Pupil plane Lyot plane Defocus of the source to
test the SCC with a theoretical amplitude of 1.8 nm Phase
difference image for 1.8 nm Test Bench Development
Integration started in May 09 See Marion Mas (poster yesterday !!!)
Conclusion Phase estimation:
Optimized for long exposure time (10s seconds to mesure 1nm level-
EPICS case) Simple set-up with Lyot and phase mask coronagraph To
be coupled with IFS because of chromatism (or need more advanced
estimator) Deeper study on-going (closed loop, chromatism,)
Coupling with planet detection to be studied in more details
(especially for the long exposure time case) Need more laboratory
test