1. Improved Tilt Sensing in an LGS-based Tomographic AO System Based on Instantaneous PSF Estimation Jean-Pierre Véran AO4ELT3, 27-31 May 2013

2. AO fields (NFIRAOS) 17”x17” science field 70” diameter LGS asterism 120” diameter “technical” field To pick-off NGS sources Used to sense tip, tilt and tilt anisoplanatism (NGS modes) All LGS-based MCAO, LTAO MOAO systems have a similar arrangement

3. NGS modes in a tomographic LGS system NGS modes = tip, tilt and tilt anisoplanatism How well we can correct the NGS modes sets the sky coverage For NFIRAOS, 3 NGSs (2 T/T and 1 2x2 Shack-Hartmann) Problem: NGSs are usually far away from the science field and are therefore poorly corrected (even if MCAO is implemented) Spot centroiding error –Decreases with sharper core –Decreases with higher number of photons in the core Spot centroiding error propagates to reduce NGS mode correction

4. Mitigation #1 Improved control A more sophisticated control strategy allows increasing the exposure time (so more photons in the core) without being severely penalized by the increase in servo-lag error Increased sky coverage with optimal correction of tilt and tilt- anisoplanatism modes in laser-guide-star multiconjugate adaptive optics, Correia, Carlos; Véran, Jean-Pierre; Herriot, Glen; Ellerbroek, Brent; Wang, Lianqi; Gilles, Luc, JOSA A, vol. 30, issue 4, p. 604, 2013 –Uses LQG control of all the NGS modes –Improves the sky coverage by ~20% on NFIRAOS, compared to simple type-I control

5. Mitigation #2 Image sharpening Use a DM in each of the NGS WFS paths to sharpen the NGS spots The DM is driven based on a wave-front estimate in the direction of the NGS, derived from the current 3D estimate of the turbulence obtained from the LGSs Pros: –Potential for spectacular improvements in sky coverage Cons: –DM is driven in open-loop –Significant increase in cost and in complexity (opto-mechanics + software)

6. NGS sharpening on NFIRAOS Lianqi Wang, TMT

7. Spot centroiding using long exposure reference NFIRAOS baseline: unconstrained matched filters, based on Gaussian fit to long exposure spot image. Example: H-band, WFE=600nm RMS (SR=0.4%), PDE=600, rn=3e-, TT=0mas RMS, 100 uncorrelated spot images, 8x8 pixels, 5.5mas/pixel (Nyquist) X-filter Y-filter Average spot image Gaussian fit Examples of instantaneous spot images Corresponding instantaneous PSFs

8. Spot centroiding using short exposure reference Short exposure spot image (instantaneous PSF) can be estimated from the tomographic estimate of the turbulence volume obtained from the LGSs. –Similar process to estimating the DM drive commands for image sharpening The estimate of the instantaneous PSF can be used for better centroiding Matched filter are no longer attractive because no analytical model for instantaneous PSF. However, other centroiding techniques can be used such as: –Correlation –PSF fitting

9. Inspiration Deconvolution from wave-front sensing (DWFS) –Deconvolution from wave-front sensing: a new technique for compensating turbulence-degraded images, J. Primot, G. Rousset, and J. C. Fontanella, JOSA A, Vol. 7, Issue 9, pp. 1598-1608 (1990) –Use WFS measurements to aid speckle imaging –Improves performance of traditional speckle imaging techniques –Early days of AO

10. PSF fitting Find (a,b,c) that minimize: Where: I(x,y) is the recorded spot image, PSF(x,y) is the estimated instantaneous PSF, and σ x,y is the noise at each pixel. Carry out the minimization in the Fourier domain, using the Levenberg-Marquardt algorithm for quick convergence Trivial case of finding the photometry and astrometry of a stellar field image knowing the PSF (only one star here!)

11. Simulation Step 1: Creation Create 100 random phase screens with spatial frequency distribution f^[-2,-3] For each screen –Remove P/T/T and renormalize to RMS=[100,300,600] –Create instantaneous PSF –Scale total to [100,200,300,400,500,600] PDE (store S1) –Apply tilt=N(0,[0,0.1,0.2,0.3,0.4,0.5])pix –Apply [8x8,4x4] window (store S2) –Apply photon + readout noise (3e-) (store S3) Compute: –Long exposure PSF (from S3) –Unconstrained matched filters (from LEPSF + 3e- noise)

12. Simulation Step 2: Processing For each image: –Apply matched filter –Correlate with long exposure PSF and find maximum of correlation function –Correlate with instantaneous PSF and find maximum of correlation function –Apply PSF fitting using long exposure PSF –Apply PSF fitting using instantaneous PSF

13. Preliminary results NFIRAOS pure tilt residual ~ 1mas RMS or 0.2pix RMS

14. Conclusion Improved centroiding using an estimate of the instantaneous PSF might be an interesting alternative to image sharpening –Implementation only requires a bit of additional software Work in progress Preliminary results are encouraging PSF fitting could probably be improved by not trying to estimate the amplitude of the PSF from each image –Use amplitude of long exposure PSF instead Errors in estimating the instantaneous PSF needs to be addressed