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Optical System Design of Telescope Based on Mixed Modulation Diffractive Lens ()

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*Journal of Applied Mathematics and Physics*,

**6**, 2322-2329. doi: 10.4236/jamp.2018.611193.

1. Introduction

Using of diffractive optical elements (DOE) in the Schupmann system offer a new way for the construction of ultra-large aperture telescope [1] [2]. As a key chromatic aberration correction device, Fresnel Corrector, showed in the Schupmann system in Figure 1, is equivalent to a miniature version of Magnifying Glass in the system. Generally, in a large aperture telescope (>20 m), the diameter of the Fresnel Corrector is close to 1 m, while the F number of the Fresnel corrector is close to 1. As a Fresnel Corrector with a small F number and a large aperture is relatively difficult to process, it is necessary to improve it for easier processing. In our previous works, we have studied the theoretical design and simulation process of an amplitude and phase hybrid modulation Fresnel diffractive optical element (APHMFDOE), which is generated by adding a diffraction phase profile to the transparent band of the AFZP. The results showed that APHMFDOE can increase the feature size of the diffractive element without changing its F-number [3]. In theory APHMFDOE can reduce the processing difficulty of the Fresnel Corrector and increase the design freedom of it. In this paper, we consider using it as the Fresnel Corrector.

2. The Design Theory of APHMFDOE

The APHMFDOE is generated by adding a quadratic phase factor to the transparent band of the AFZP. According to the distribution law of the bands in AFZP, we know that the transmittance function of APHMFDOE has periodicity in the R-square coordinate system, and the period is equal to $2{\lambda}_{0}{f}_{0}$ . Suppose the phase factor to be added is $\mathrm{exp}\left(-ipk{r}^{2}/2{f}_{0}\right)$, p is an integer, the transmittance function of APHMFDOE can be described as

$G\left(r\right)=\{\begin{array}{l}\mathrm{exp}\left[i2\pi \alpha p\left(k-\frac{{r}^{2}}{2{\lambda}_{0}{f}_{0}}\right)\right]\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}{r}_{2k}\le r<{r}_{2k+1}\\ 0\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}{r}_{2k+1}\le r<{r}_{2k+2}\end{array}$ (1)

where ${r}_{k}=\sqrt{k{\lambda}_{0}{f}_{0}}$, ${\lambda}_{0}$ is the design wavelength, ${f}_{0}$ is the focal length of the AFZP, and $\alpha $ is a value related to the chromatic dispersion. In order to facilitate comparison with the phase of the spherical wave, we write the Fourier series expansion of $A\left(r\right)$ in Equation (2).

$\begin{array}{c}G\left(r\right)=\underset{m=-\infty}{\overset{+\infty}{{\displaystyle \sum}}}\mathrm{exp}\left(i2\pi \alpha pk\right)\mathrm{exp}\left[-i\pi \left(2k+1.5\right)\left(\alpha p-m\right)\right]\\ \times \frac{1}{2}sinc\left(\frac{\alpha p-m}{2}\right)\mathrm{exp}\left(-i\frac{\pi m{r}^{2}}{{\lambda}_{0}{f}_{0}}\right)\end{array}$ (2)

Figure 1. Schupmann system used in a diffractive telescope [1].

Compared with the standard spherical wave phase factor, the focal length of APHMFDOE corresponding to the design wavelength ${\lambda}_{0}$ can be described as

${{f}^{\prime}}_{0}={f}_{0}/m$ (3)

In addition, we can also obtain from Equation (2) that different diffraction orders have different efficiencies. The efficiency of the m^{th} order diffracted light of APHMFDOE can be written as

${\eta}_{m}=\frac{1}{4}sin{c}^{2}\left(\frac{\alpha p-m}{2}\right)$ (4)

In order to more clearly study the variation of diffraction efficiency with diffraction order, we make the incident light wavelength equal to the design wavelength. Then we obtain that $\alpha $ is equal to 1. Substituting the value of $\alpha $ into Equation (4) and simplifying it, one can obtain

${\eta}_{m}=\{\begin{array}{l}\frac{1}{4}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}m-p=0\\ 0\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.05em}}\text{\hspace{0.05em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}m-p=2k,m-p\ne 0\\ \frac{1}{{\left(2k+1\right)}^{2}{\pi}^{2}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}m-p=2k+1\end{array}$ (5)

It is easy to obtain that the diffraction efficiency of APHMFDOE is the same as the diffraction efficiency of the main diffraction order of AFZP when m = p + 1 [4]. According to Equation (3), the (p + 1)^{th} diffraction order focal length of APHMFDOE corresponding to the design wavelength
${\lambda}_{0}$ is equal to

${{f}^{\prime}}_{0}={f}_{0}/\left(p+1\right)$ (6)

It can be seen from Equation (6) that the focal length of APHMFDOE is less than the main focal length of AFZP if p is a positive integer. However, the feature size of the diffractive element has not changed during the process of generating APHMFDOE. That is to say, APHMFDOE can achieve a larger feature size than AFZP on the premise of the same focal length and diameter. We denote the F-number corresponding to the light of the p + 1 diffraction order by F and the feature size of APHMFDOE by $\omega $ . Using the relationship between the Fresnel zone radius and the focal length and wavelength, it is not difficult to obtain

$\omega =2{\lambda}_{0}\left(p+1\right)F$ (7)

Compared with the Fresnel zone plate and the phase Fresnel lens, the feature size of APHMFDOE is increased by p + 1 times. The increasing of the feature size of the Fresnel Corrector can improve the system design freedom.

3. Design and Simulation of Optical System

3.1. Design of Optical System

The Schupmann system could eliminate chromatic dispersion accurately and completely for all wavelengths received by the Eyepiece in principle, and many people have proved this theory [5] [6].The most important condition in ensuring system achromaticity is

${f}_{FC}=-{\eta}^{2}{f}_{MG}$ (8)

where ${f}_{MG}$, ${f}_{FC}$ are the focal lengths of Magnifying Glass and Fresnel Corrector, respectively, $\eta $ is the magnification of the Reimager. So far, many diffraction devices, including Fresnel Zone Plate, phase Fresnel lens and photon sieves, have been used as Magnifying Glass [6] [7] [8]. Similarly, the main focal length of these devices are all inversely proportional to the wavelength showed in Equation (8).

${f}_{MG}=\frac{{\lambda}_{0}{f}_{MG0}}{\lambda}$ (9)

where ${f}_{MG0}$ is the focal length of Magnifying Glass corresponding to the design wavelength ${\lambda}_{0}$, and $\lambda $ is the wavelength of the incident light. In addition, people often use phase Fresnel lens as the Fresnel Corrector in the existing research. As the focal length of the Fresnel Corrector also satisfies the Equation (9), it is easy to prove that their focal length at any wavelength satisfies Equation (8), if the design focal length of Magnifying Glass and Fresnel Corrector meets Equation (8). Here we are going to use APHMFDOE as the Fresnel Corrector, so the most important thing is also that the focal length of APHMFDOE at any wavelength satisfies Equation (8).

From Equation (2), we can obtain the focal length of APHMFDOE corresponding to the wavelength $\lambda $, showed in Equation (10).

$f=\frac{{\lambda}_{0}{f}_{0}}{m\lambda}$ (10)

Substituting Equation (6) into Equation (10), one can obtain

${f}_{FC}=\frac{{\lambda}_{0}\left(p+1\right){f}_{FC0}}{m\lambda}$ (11)

where ${f}_{FC0}$ and ${f}_{FC}$ are equal to ${{f}^{\prime}}_{0}$ and $f$, and are the focal lengths of Fresnel Corrector corresponding to the design wavelength ${\lambda}_{0}$ and incident light wavelength. In general, it is easy to make the focal lengths corresponding to the design wavelength satisfy the achromatic condition by controlling the shape and structure of the Magnifying Glass and APHMFDOE, which is showed in Equation (12).

${f}_{FC0}=-{\eta}^{2}{f}_{MG0}$ (12)

Simultaneous Equations (9), (11) and (12), one can obtain

${f}_{FC}=-{\eta}^{2}\frac{\left(p+1\right)}{m}{f}_{MG}$ (13)

It can be seen from Equation (13) that there is always a diffraction order m = p + 1 that makes the system satisfy the achromatic condition. That is to say, APHMFDOE can be used as the Fresnel Corrector in theory.

However, APHMFDOE increases the feature size of the Fresnel Corrector at the expense of diffraction efficiency, and the diffraction efficiencies of different wavelengths of light are different. According to Equation (4), the diffraction efficiency of p + 1 diffractive order light of different wavelengths can be described as

${\eta}_{p+1}=\frac{1}{4}sin{c}^{2}\left(\frac{\alpha p-p-1}{2}\right)$ (14)

In order to understand the effect of APHMFDOE on the diffraction efficiency more clearly, we plot the diffraction efficiency as a function of the wavelength at different p values, which is showed in Figure 2.

It can be seen from Figure 2 that the relationship between diffraction efficiency and wavelength is very complex, and is quite different under different values of p. However, the diffraction efficiency decreases with the increase of wavelength, when the wavelength is near the design wavelength. Although the feature size of the Fresnel Corrector increases as the value of p increases, we cannot blindly increase the value of p. We must consider the effect of p value on the diffraction efficiency in the specific design.

3.2. Simulation Results of Optical System

In general, the F-number of the Fresnel Corrector should be greater than 1 or 2 due to the feature size. Based on this principle, Roderick A. Hyde gave two specific design examples in his paper showed in Table 1 [1]. The design wavelength is 0.5 μm, while the spectral range is from 0.48 to 0.52 μm.

We replace the conventional Fresnel Corrector with an APHMFDOE, and list the design parameters of the new system here in Table 2.

Comparing Table 1 and Table 2, we find that the Fresnel Corrector in the new system have a larger rim feature size under the same Eyepiece. In other words, it means that the new system can further reduce the length of the Eyepiece

Figure 2. Diffraction efficiency varies with wavelength at different p values, the design wavelength is 0.5 μm.

under the same rim feature size. Therefore, on the one hand, APHMFDOE can increase the feature size of the Fresnel Corrector and reduce the processing difficulty of the Fresnel Corrector to some extent; On the other hand, it can reduce the length of the eyepiece and make the Eyepiece system more compact.

In order to better verify the reliability of APHMFDOE as a Fresnel Corrector, we simulate done of the new systems with $\eta =0.01$ showed in Table 2. Since there is no APHMFDOE surface type in the conventional optical design software, we wrote a program in Matlab to simulate the system, among which the physical propagation method was used. However, the simulation of the entire system requires a very large storage space and a very long running time due to the large aperture of the components of the system. So we only simulated the system in one direction, and then obtained the normalized intensity of the system at the image plane at different wavelengths showed in Figure 3.

It can be seen from the simulation results in Figure 3 that the system has better focusing characteristics for different wavelengths of light at the same image

Table 1. Roderick A. Hyde’s design examples.

Table 2. Design parameters of the new system.

Figure 3. Normalized intensity of the system at the image plane at different wavelengths.

Figure 4. The diffraction efficiency of the scaled down system.

plane, and the focused spot size is basically the same. That is to say, the chromatic aberration introduced by Magnifying Glass is well compensated by APHMFDOE. So we get a conclusion that APHMFDOE is feasible and reliable for use as a Fresnel Corrector. In addition, in order to explore the effect of APHMFDOE on the diffraction efficiency of the system, we need to know the intensity distribution of the whole image surface. Due to the large size of the telescope, the simulation of the entire optical plane requires a lot of sampling points, resulting in a large amount of computer-calculated data and a very long running time. So we simulated a scaled down system, which is equivalent to 10,000 times smaller than the original system. The diffraction efficiency of this system at different wavelengths was obtained and showed in Figure 4. The results showed that the diffraction efficiency of the system decreases with the increasing of the wavelength, which is consistent with the theoretical effect of APHMFDOE on the diffraction efficiency of the system.

4. Conclusion

We have studied the theoretical design and simulation process of APHMFDOE as a Fresnel Corrector. The results show that APHMFDOE can be used as a Fresnel Corrector to compensate for the chromatic aberration introduced by Magnifying Glass. Its advantage is that it can increase the feature size of the Fresnel Corrector. However, these benefits do come at the expense of the diffraction efficiency of the system. The diffraction efficiencies of the incident light of all the wavelengths are reduced, in addition, they are different at different wavelengths.

Conflicts of Interest

The authors declare no conflicts of interest.

[1] | Hyde, R.A. (1999) Eyeglass. 1. Very Large Aperture Diffractive Telescopes. Applied optics, 38, 4198-4212. https://doi.org/10.1364/AO.38.004198 |

[2] | Hinglais, E. (2011) A Space Fresnel Imager Concept Assessment Study Led by CNES for Astrophysical Applications. Exp Astron, 30, 85. https://doi.org/10.1007/s10686-011-9218-5 |

[3] | Li, F., Cheng, J., Wang, M., Jin, X. and Wang, K. (2018) An Amplitude and Phase Hybrid Modulation Fresnel Diffractive Optical Element. Opt Commun, 413, 44-47. https://doi.org/10.1016/j.optcom.2017.12.023 |

[4] | Arsenault, H. (1968) Diffraction Theory of Fresnel Zone Plates. JOSA, 58, 1536-1536. https://doi.org/10.1364/JOSA.58.001536 |

[5] | Koechlin, L., Rivet, J.-P., Deba, P., Serre, D., Raksasataya, T., Gili, R. and David, J. (2012) First High Dynamic Range and High Resolution Images of the Sky Obtained with a Diffractive Fresnel Array Telescope. Exp Astron, 33, 129-140. https://doi.org/10.1007/s10686-011-9277-7 |

[6] | Hyde, R.A., Dixit, S.N., Weisberg, A.H. and Rushford, M.C. (2002) Eye-glass: A Very Large Aperture Diffractive Space Telescope. Highly Innovative Space Telescope Concepts (International Society for Optics and Photonics 2002), 28-40. https://doi.org/10.1117/12.460420 |

[7] | Serre, D., Koechlin, L. and Deba, P. (2011) The Fresnel Imager: Learning from Ground-Based Generation I Prototype. Exp Astron, 30, 137-147. https://doi.org/10.1007/s10686-010-9201-6 |

[8] | Andersen, G., Dearborn, M. and McHarg, G. (2010) Photon Sieve Space Telescope. Air Force Academy Colorado Springs Co. |

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