Experimental Sensitivity Table Method for Precision Alignment of Amon-Ra Instrument
Experimental Sensitivity Table Method for Precision Alignment of Amon-Ra Instrument
Journal of Astronomy and Space Sciences. 2014. Sep, 31(3): 241-246
Copyright © 2014, The Korean Space Science Society
This is an Open Access article distributed under the terms of the Creative Commons Attribution Non-Commercial License ( which permits unrestricted non-commercial use, distribution, and reproduction in any medium, provided the original work is properly cited.
  • Received : June 02, 2014
  • Accepted : September 04, 2014
  • Published : September 15, 2014
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About the Authors
Eunsong, Oh
Space Optics Laboratory, Dept. of Astronomy, Yonsei University, 134 Sinchon-dong, Seodaemun-gu, Seoul, 120-749, Korea
Ki-Beom, Ahn
Space Optics Laboratory, Dept. of Astronomy, Yonsei University, 134 Sinchon-dong, Seodaemun-gu, Seoul, 120-749, Korea
Sug-Whan, Kim
Space Optics Laboratory, Dept. of Astronomy, Yonsei University, 134 Sinchon-dong, Seodaemun-gu, Seoul, 120-749, Korea

The Amon-Ra instrument is the main optical payload of the proposed EARTHSHINE satellite. It consists of a visible wavelength instrument and an IR energy channel instrument to measure a global Earth albedo. We report a new sensitivity technique for efficient alignment of the visible channel instrument. Whilst the sensitivity table method has been widely used in the alignment process, the straightforward application of the method tends to produce slow process convergence because of shop floor alignment practice uncertainties. We investigated the error sources commonly associated with alignment practices and used them when estimating the Zernike polynomial coefficients. Aided with single center field wavefront error (WFE) measurements and their corresponding Zernike polynomial coefficients, the method involves the construction and use of an experimental, instead of simulated, sensitivity table to be used for alignment state estimations. A trial alignment experiment for the Amon Ra optical system was performed and the results show that 71.28 nm in rms WFE was achieved only after two alignment iterations. This tends to demonstrate its superior performance to the conventional method.
The Albedo Monitor and Radiometer (Amon-Ra) instrument is the primary payload of the proposed EARTHSun-Heliosphere Interactions Experiment (EARTHSHINE) satellite (Park et al. 2007, Lee et al 2005a, 2005b). The goal of the instrument is to measure the Earth albedo variation. The instrument consists of two optical systems. The first is a visible channel instrument to observe both the Earth and Sun alternately over the wavelength range of 0.4 ~ 0.75 μm. The other is an energy channel for bolometric measurement of the incident solar and Earth reflected shortwave radiations over 0.4 ~ 4.0 μm in wavelength. The observation concept of Amon-Ra is such that it is designed to share the same optical train as much as possible, when viewing the Earth and Sun as the spacecraft rotates (Park et al. 2007, Lee et al 2005a, 2005b). Therefore, the accurate alignment of the instrument optical system is crucial for achieving the science goal. We studied the precision optical alignment of the Amon-Ra visible channel system and report the new sensitivity table alignment technique and its alignment performance in this paper.
Over the past few decades, several computer aided alignment (CAA) methods based on the Zernike polynomials have been developed to ensure the efficient alignment of optical systems (Jeong et al. 1987, Rimmer 1990, Chapman & Sweeney 1998, Zhang et al. 2000, Kim et al. 2007, Lee et al 2007). Among them, the sensitivity table technique is arguably the most widely used method to align two-mirror and threemirror systems (Jeong et al. 1987, Rimmer 1990, Chapman & Sweeney 1998, Zhang et al. 2000, Kim et al. 2007, Bin et al. 2010, Kea et al. 2008, Zhao et al. 2010, Kim et al. 2005, Yang et al. 2004).
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The technique uses Eq. 1, where [ Z11 , ⋯ , Zm1 ] form the Zernike polynomials representing the measured system wavefront errors (WFE) at the arbitrary alignment state. The D matrix describes the alignment deviation of the optical element parameters, such as decenter and tilt, from those of the ideal alignment state. [ A11 , ⋯ , Amn ] form the Zernike sensitivity table constructed from changes in Zernike coefficients corresponding to alignment parameter variations.
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Typically, Eq. 2 is required to build a sensitivity table ( A mn ), where Δ Zm represents the changes in the Zernike coefficient caused by variations in the alignment parameters (Δ Dn ) such as decenter and tilt. The conventional method used to obtain A mn is to compute Δ Zm while adjusting Δ Dn in ray tracing simulation using software such as Code V and ZEMAX.
However, it is well known that resulting A mn tends to produce its nonlinearity to Δ Dn and it needs lengthy multifield measurements to improve the estimation accuracy of Δ Zm (Kim et al. 2007, Kim et al. 2009, Oh et al. 2010). In addition, the technique also tends to ignore measurement field pointing uncertainties, apparatus control uncertainties, and part surface form accuracy. These contribute to increasing differences between simulated and measured Zernike coefficients [ Z 11 , ⋯ , Z m1 ] and their variations Δ Zm and, therefore, the resulting sensitivity table A mn .
In this paper, we improve the technique with a simple and practical conceptual shift to the use of experimental sensitivity table, being away from the simulated one. Section 2 describes the theoretical method, the target optical system characteristics used and the application of the new experimental sensitivity table method. Alignment simulations and experimental results are described in Section 3, demonstrating its superior performance to that of the conventional method. In Section 4, the implications of the new experimental sensitivity method are summarized.
- 2.1 Theoretical method
The experimental sensitivity table can be constructed by replacing the simulated A mn with the experimental A mn obtained from multiple center field, as opposed to multi-field, WFE measurements (Δ Zm ) while the alignment parameters associated with each optical component are changed in known steps Δ Sn’ , as in Eq. 3. In this way, the experimental sensitivity table is built while reflecting the sum of all aforementioned uncertainties.
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Once it has been built, solving Eq.1 requires for an inverse matrix A + mn of A mn . The singular value decomposition (SVD) was used to derive A + mn as in Eq.4, where D 3×1 means the deviations of the alignment parameter such as Decenter X, Decenter Y, and Tilt Y in this study. Z 4×1 is fringe Zernike coefficients from the 5 th to the 8 th term when measuring at the center field. For the alignment case study described in Section 2.2, SVD of an 4×3 matrix A is transformed to the inverse matrix ( A + ) consisting of three matrix. UT is an 4×4 unitary matrix, V is an 3×3 unitary matrix, and Σ + is an 4×3 diagonal matrix having singular values of A in the diagonal entries (Σ + 11 : 2.9009, Σ + 22 : 0.0341, Σ + 33 : 0.0016). We then computed and traced the alignment state of the optical system for each step alignment experiment.
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- 2.2 Target optical system: Two-mirror system with high obscuration
To experimentally verify the performance increase resulting from such a simple yet practical conceptual shift, we used a catadioptric optical system of high obscuration from the relatively large secondary mirror of 38 mm in diameter as shown in Table 1 . Its optical system consists of two mirrors and four corrector lenses. Incident light rays are reflected from the system’s primary mirror (M1) that is 76 mm in diameter and −1.0 in conic constant, and then from its secondary mirror (M2). The M2 alignment tolerance was computed to ± 140.0 μm in decenter and ± 100.0 arcsec in tilt ( Fig. 1-(a) ). The system alignment was required to meet the requirement of 126.56 nm in rms WFE (Lee et al. 2005b). The alignment test configuration has the target optical system sandwiched in between a phase-shifting interferometer and a reference flat mirror, as shown in Fig. 1 . M1 and the corrector lens barrel were already aligned and fixed to each other via the M1 support plate within the predetermined tolerance level. The despace between M1 and M2 was also aligned for the minimum spherical aberration value so that it was not regarded as the alignment parameter that can affected by the lens barrel states. M2 decenter and tilt are the two alignment variables that need to be controlled in order to achieve alignment, and this paper is focusing at the M2 precise alignment.
Measured specification of optical elements of target optical system (Park et al. 2007).
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a Conic Constant of Primary Mirror is −1.0, and other elements are spherical (conic =0.0). b (F) means a front surface, and (R) is a rear surface of lens respectively.
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(a) 2-D layout of Amon-Ra, (b) Alignment set-up environment.
- 2.3 Simulations and experiments with experimental sensitivity table method
First, the experimental sensitivity table was constructed from a series of wavefront measurement at the center field. From the approximated alignment status, M2 was moved 5 μm for decenter and 0.18 arcmin for tilt in a sampling step. The system WFE was then measured, and its corresponding Zernike polynomial coefficients were obtained three times at each measurement location for decenter and tilt for x and y axes, respectively. The resulting Zernike coefficient variation trends for the y-axis tilt are shown in Fig. 2 as an example.
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Fringe Zernike sensitivity variations when (a) decentering to x-axis, (b) decentering to y-axis, and (c) tilting to y-axis tilt parameter of M2.
Once all the measurements were completed, we then polynomial-fit the Zernike coefficient variation over the decenter and tilt ranges used. In the polynomial fitting, we used the linear fitting equation which is the same process with Eq. 1. and 2. The final sensitivity table was then constructed, as shown in Table 2 where the resulting sensitivities from both conventional and experimental methods are compared. We note that the experiment to determine Zernike coefficients for x axis tilt was not performed because of the inaccurate goniometer tilt X motion caused by its unpredictable backlash characteristics.
Sensitivity table from the conventional simulation and from this experiment using M2 (i.e., on-axis center field measurement only).
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Sensitivity table from the conventional simulation and from this experiment using M2 (i.e., on-axis center field measurement only).
The fringe Zernike coefficients from the 5 th to the 8 th term representing high order aberrations are listed in Table 2 . In general, the 7 th term Zernike coefficient is closely related to the x-axis decenter and the y-axis tilt, while the 8 th term is sensitive to the y-axis decenter and the x-axis tilt. From Table 1 , it is clear that the y-axis tilt plays the most significant role in the Zernike coefficients’ sensitivity.
Calculated inverse matrix (A+) of using SVD technique from the sensitivity table inTable 2.
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Calculated inverse matrix (A+) of using SVD technique from the sensitivity table in Table 2.
The conventional method shows ~10 −10~−12 in the 5 th and 6 th term Zernike coefficients, illustrating the negligible effects of decenter and tilt variations on the on-axis field measurement. We note that, whilst their magnitude is somewhat smaller than the others, the 7 th and 8 th term coefficients also show increasing sensitivity trends similar to those of the 5 th and 6 th terms as well. These prove that the aforementioned measurement field positioning and apparatus control error significantly influence the resulting sensitivities.
Second, using the sensitivities in Table 2 and Eq. 4, we computed and compared the inverse sensitivity tables ( A + ) between the conventional simulation method and the new experimental method. With these inverse matrixes of sensitivity table, we performed two simulations and one experiment that is described in section 3.
Fig. 3 shows the results from two alignment simulations and one experiment. Fig. 3-(a) illustrates the results from using the target optical system design without any additional errors included. We note that, in this ideal case, both conventional and experimental sensitivity methods are capable of producing the alignment state estimation (i.e., solution) after the first iteration.
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Alignment performance results from two methods (blue dotted line : conventional sensitivity table, red line : experimental sensitivity table). (a) is the simulation results for the the optical system without fabrication error. (b) is the simulation results for the de designed optical system with surface fabrication WFE errors included and (c) is resulted from the actual alignment experiment.
The results in Fig. 3-(b) were obtained with 82.264 nm rms WFE in surface fabrication error introduced to M2. Both methods show similar performance in decreasing the simulated system wavefront below the requirement, although the experimental sensitivity method shows marginally better estimation after the 1 st iteration.
The results of the real alignment experiment appear in Fig. 3-(c) . The conventional method shows an alignment divergence, even for the 1 st alignment correction, which was caused by an incorrect estimation of Zernike fringe coefficients. On the other hand, the experimental sensitivity table method estimated the alignment state accurately and is capable of reducing the system’s wavefront to make it lower than the requirement in just two iterative alignment actions.
In Fig. 4 and Table 4 , he initial alignment state at the center field is 362.71 nm rms WFE, where the new method’s estimate for the system’s misalignment is 0.0395 mm in the x-axis decenter, −0.0124 mm in the y-axis decenter, and −2.5472 arcmin in the y-axis tilt parameter. We adjusted the M2 location by the same amounts but to the opposite direction from the misalignment computed above. Then the alignment state improved to 192.15 nm rms WFE. After iterating one more similar alignment action with using Table 4 , the optical system rms WFE became 71.28 nm in the onaxis field, excluding the masked area, which is better than the requirement, as shown in Fig. 4 .
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Evolution of the WFE map after the experimental sensitivity table method shown in Fig. 3-(c) was used. (a) shows WFE map of the initial misaligned state, (b) was obtained after 1st alignment iteration, and (c) is the final WFE map after 2nd alignment iteration.
The measurement results of alignment state using the experimental sensitivity table.
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The measurement results of alignment state using the experimental sensitivity table.
We performed the alignment experiment for the visible channel optical system of Amon-Ra instrument successfully using the new experimental sensitivity table method. The resulting optical alignment performances between the conventional and the new technique are compared. In summary, the target optical system has technical difficulty when measuring a wavefront map because of the high obscuration (of 79.40%) caused by M2 (Park et al. 2007) and the support structure. The conventional (i.e., simulated sensitivity from the optical design) method produces an incorrect estimation of its alignment state in real experiments, largely due to the measurement uncertainties. On the other hand, the new and improved (i.e., experimentally obtained sensitivity with the on-axis center field measurement) method is capable of satisfying the WFE requirement in just two alignment actions. This proves that the experimental sensitivity method studied here would offer considerable efficiency and accuracy to the shop floor alignment process with its simplicity and high degree of practicality.
This work is supported by “Geostationary earth orbit Korea Multi-Purpose Satellite Ocean Monitoring Payload Development” funded by the Ministry of Land, Transport and Maritime Affairs of Korean government and “Optical Performance Simulation of Geostationary Ocean Color Imager” (PE99241) of the Korea Institute Ocean Science and Technology. The manuscript preparation is also supported in part by SRC program (2010-0027910) from Center for Galaxy Evolution Research (CGER). This research was also supported by the Korea Astronomy and Space Science Institute under the R&D program (Project No. 2014-9-710- 03) supervised by the Ministry of Science, ICT and Future Planning.
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