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Nick Kaiser Pan-STARRS, Institute for Astronomy, U. Hawaii Following the Photons Edinburgh, Oct 10, 2011 Configuring the Pan-STARRS Optics - From Simulations.

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Presentation on theme: "Nick Kaiser Pan-STARRS, Institute for Astronomy, U. Hawaii Following the Photons Edinburgh, Oct 10, 2011 Configuring the Pan-STARRS Optics - From Simulations."— Presentation transcript:

1 Nick Kaiser Pan-STARRS, Institute for Astronomy, U. Hawaii Following the Photons Edinburgh, Oct 10, 2011 Configuring the Pan-STARRS Optics - From Simulations to Operational Control System

2 2 Pan-STARRS PS4 Observatory

3 3

4 4 Haleakala Observatories, Maui, HI

5 5 Introduction The Pan-STARRS telescope has to deliver sub-arc- second images over a 3-degree diameter field of view –It has 2 mirrors, 3 lenses (several highly aspheric surfaces) and a focal plane –alt-az design with L3 and the camera behind the instrument rotator –That gives 5x = 27 degrees of freedom (tilts, decenters and despaces) –to be adjusted to get all of the elements collimated and aligned with the rotator axis –Required precision is ~tens of micron –In addition, the primary mirror support system has 12 independently controllable pneumatic axial supports –total of 39 d.o.f. to be controlled

6 6 Pan-STARRS Opical Design

7 7 Mirror Support Systems

8 8 PS-1 Primary Mirror Support System

9 9 How do we configure the PS optics? Advice from experts… not encouraging –Too many parameters –What about “degeneracies”? –Won’t you get stuck in a local minimum? Or crawl along a valley? –Discouraging lessons from megaprime… –Try to “divide and conquer”? Problem: M1/M2 system alone does not deliver images even on axis M1/M2 system has real-time control of all d.o.f Approach adopted (evolved) –1) Solve 8 d.o.f problem of M1, M2 relative to L1+L2 L1+L2 assembled at UW on turntable quite accurately –2) Then fix any tilt of detector plane L3 (dewar window) is relatively weak Rotator allows this to be determined separately from any tilt introduced by M1+M2+L1+L2 system

10 10 Initial configuration: Plan: use auto-reflecting telescope –Mounted on a jig on the back of the telescope –Aligned with rotator axis –Used to align other elements with targets (M2) and fiducial marks (lenses) First light (07/2007) gave ~10” IQ Adjusting mirrors iteratively gave ~2” IQ Field curvature and field dependent astigmatism diagnosed –Attributed to L1, L2 de-space But still IQ was not adequate Exploring 8 parameter M1, M2 til + decenter parameter space infeasible Needed a more methodical approach

11 11 Aberration diagnosis techniques Traditional wave-front sensing approaches: –Shack-Hartmann imaging Implemented in PS GPC1 as deployable probe –Hartman mask imaging –Knife-edge test –Rotational beam-shearing interferometry Claude Roddier thesis Other probes –Ghost image analysis –Direct (e.g. laser) metrology –Analysis of in-focus images Highly non-linear dependence on positional d.o.fs Too hard to explore big parameter space Technique adopted: –Use M2 de-space to generate out-of-focus (a.k.a. donut) images –Thousands of stars per exposure => huge amount of information –At large enough defocus shapes become linearly dependent on misconfiguration parameters (like weak-lensing)

12 12 Wavefront Aberrations from Out-of-Focus Images Perfectly collimated (and designed) telescope gives donut images when defocused that are –Uniformly bright –Circularly symmetric annular because of hole in primary –At large-enough defocus these are well described by geometric optics (images formed by “rays”) Any aberrations (displacement of elements or figure errors) deflect rays and cause distortion of the shape of the out-of-focus image –Crowding or dilution of the density of rays modulated brightness a la Roddier (1990) –Brightness proportional to curvature (Laplacian) of converging wave-front aberration. –Hence “curvature sensing” –Pioneered by Roddier group at IfA for Adaptive Optics

13 13 Illustration of the effect of a localized aberration on out-of-focus images

14 14 Advantages: Linearity and Multiplexing Donut shape statistics are a linear response to causes of aberrations –Linearity breaks down too close to focus. –Shadowing and flat fielding etc. become problematic too far from focus. –`Sweet spot' seems to be around 3mm defocus – may be possible to go closer for more sensitivity But may require `physical optics' modelling Solve a set of linear equations to find mirror displacements and actuator commands to cancel aberration –No iteration (in principal) - one step solution –No local minima - finds unique global minumum –Massively multiplexed - thousands of stars per image

15 15 Separating Seeing and Mirror Wobbling from Aberrations We want to obtain sub-seeing aberrations. But seeing causes wavefront errors of many radians of phase –Causes donuts to wobble around like jello. –Averages out in long exposures –But leads to smearing. Worse still, mirror oscillations will produce persistent anisotropies Fortunately, such affects can be readily distinguished by using both pre- and post-focus image pairs.

16 16 Symmetries Between Pre- and Post-Focus Image Statistics 1) Focus aberration

17 17 Symmetries Between Pre- and Post-Focus Image Statistics 2) Comatic (cos phi) aberration

18 18 Symmetries Between Pre- and Post-Focus Image Statistics 3) Astigmatic (cos 2 phi) aberration

19 19 Symmetries and anti-symmetries Even angular harmonic change sign passing through focus, while the odd harmonics do not If we rotate the post focus images by 180 degrees the sign always changes This is the characteristic of wave-front phase errors But wavefront amplitude errors have opposite symmetry –Easily distinguished –Can construct combinations of pre- and post focus image statistics that are blind to effects of telescope wobble, obscurations etc.

20 20 What about “degeneracies”? `Degeneracy' here means combinations of displacements that do not cause any measurable aberration –Terminology is sloppy: Technically, `degeneracy' means non-distinct eigenvalues –Here all decenter/tilts are degenerate in the proper sense. `Quasi-degeneracy' arises if there are combinations that produce almost zero measurable effect. –These cause the linear equation solution (inversion of matrix) to be singular or ill conditioned. –Example: An exact degeneracy arises because IQ only depends on relative positioning of optical elements –But is easy to deal with –Quasi-degeneracies are a little more tricky.

21 21 Dealing with quasi-degeneracies Example: decenters and/or tilts of M1 nearly degenerate with decenter of M2 Similar degeneracies for L3/focal-plane system But quasi-degeneracies are not to be feared; they are our friends –Can be identified using elementary linear algebraic techniques –They allow one to correct for one misalignment that is difficult to cure by moving another element or combination of elements that are easier –Fundamental to Pan-STARRS design real-time control over the configuration of the mirrors but not of the other elements -- which will surely flex/expand etc

22 22 Donut finding/analysis pipeline The goal is to obtain, from an out of focus gigapixel camera image, a grid of donuts covering the focal plane. –Step 1: Determine the size of the donuts Generate cleaned log-scaled image Compute the autocorrelation function Cross-correlate with theoretical model in log(r) space –Step 2: Determine location of the donuts Generate an analytic model for the 2-D donut image. Construct a regularized deconvolution filter Apply to image to obtain the locations of candidate donuts Filter candidates catalog to obtain tens of good donuts per OTA –Step 3: Generate robust (median) average Candidates include some overlaps, cell boundaries etc. Take median to get clean donut image Result is a grid of 60 donuts per focal plane

23 23 Log-scaled image

24 24 Donut model and regularised deconvolution filter

25 25 Deconvolved OTA Image

26 26 Donut locations - one OTA

27 27 Donuts sample - 1 OTA

28 28 Median donuts grid - full field - one per OTA

29 29 Donut shape statistics We need to quantify the distortion of donuts and how this varies across the field. What is a good set of statistics? It is traditional to use Zernike polynomials –see Knoll, JOSA 66, p207 We use something similar: angular Fourier expansion of radius, width and brightness of donuts –We first compute the centroid of the light in a postage stamp containing the donut –From the pixel locations, relative to the centroid, we define a radius r and azimuthal angle –Compute moments of donut radius, width and brightness Typically cos 2, cos 3, cos 4 theta modes –Exploit symmetries in pre- and post-focus images to generate combined statistic that is independent of actual focus –Results in ~100 statistics for each of ~60 donuts across the focal plane.

30 30 M1, M2 tilts and decenters

31 31 M1, M2 strongest eigenmodes

32 32 Donuts - observed vs model

33 33 PS1 Residual Aberration Analysis

34 34 PS1 Residual Aberration Analysis

35 35 PS1 Residual Aberration Analysis

36 36 PS1 Residual Aberration Analysis

37 37 PS1 Residual Aberration Analysis

38 38 PS1 Residual Aberration Analysis

39 39 U NIVERSITY OF H AWAII I NSTITUTE FOR A STRONOMY Project Proprietary Data – For Internal Use Only 39 PS1 IQ – Smallest Image Median FWHM to Date NK FWHM = 0.69", JT FWHM = 0.63  q = measure of circularity of 2D PSF

40 40

41 41

42 42

43 43 PS1 y-band – first 1 micron image of the sky

44 44 PS1 z, i, r, g band coverage

45 45 PS1 3pi survey – 15 to 20 images in five bands, building astrometric catalog for re- processing

46 46 PS1+2

47 47

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