• 천문학회보
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• 제41권1호
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• pp.57.3-58
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• 2016

We analyze an optical system of a telescope based on Fresnel type objective lens as suggested by Hyde (1999). The Fresnel objective lens can be thin, light-weight and foldable, and therefore it is possible to develop a space telescope with an aperture larger than that of traditional telescopes. Moreover a lens, whatever it is either Fresnel type or conventional, allows much larger fabrication tolerances. We design a medium-sized telescope adopting Fresnel lens as an objective lens for use in space and possibly on the ground. The well-known chromatic aberration of the Fresnel primary lens is corrected by a field lens and another Fresnel lens using Schupmann method. An additional lens is used for forming images. We analyze the chromatic and off-axis aberrations of the proposed system analytically and suggest methods for the minimization of off-axis aberrations and for the operation in wider spectral range. We also conduct ray tracing and optimize the whole optical system with commercial software. Finally we present the design parameters of a telescope with an aperture of 0.5 to 1 meters, enabling diffraction limited operation for a moderate field of view about 10 arc-minutes.

• 우주기술과 응용
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• 제1권1호
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• pp.104-120
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• 2021

Some optical schemes of lenses for spacecraft developed by the author are considered. The main optical characteristics of telescope lenses of various architectures are compared. We propose compact solutions of mirror, lens-mirror, and lens systems with maximum available angular resolutions and other parameters. Examples of calculating the optical systems of lenses used for various tasks both in the field of astronomy and in the field of remote sensing of the Earth and other planets are given. The example of onboard computer system is discussed. Practical recommendations on the development and use of telescope lenses are given.

• 대한전기학회:학술대회논문집
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• 대한전기학회 2005년도 심포지엄 논문집 정보 및 제어부문
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• pp.284-296
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• 2005

Bridge displacement measurement system using image processing is developed to overcome the contact type system inefficiencies such as heavy, expensive property and temporary construction necessity. The system is composed of tablet PC with IEEE1394 digital camera, telescope lens and a designed target mark. The key is projection algorithm where all pixels are added up for each row(column) to find out the center line. The experimental results are shown compared with a contact type system.

• 천문학회보
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• 제35권1호
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• pp.36.2-36.2
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• 2010

The CQUEAN (Camera for QUasars in EArly uNiverse) is an optical CCD camera optimized for observation of high redshift objects. It is going to be attached to the cassegrain focus of 2.1m telescope at McDonald Observatory, USA. We are making a focal reducer for CQUEAN to secure a larger field of view. The focal reducer is composed of four spherical lens, and it reduces the focal length of telescope by one third. We designed the lens configuration, performed tolerance analysis, and estimated the optical performance with ZEMAX. The differences in optical performace with/without filters were also investigated. The result from ZEMAX shows that the system has ample margin of errors for median seeing of 1.2" at McDonald observatory. Even with aberration and alignment tolerance, the performance is better than the original requirement. The lenses are now being made, and the lens barrel and an adapter for assembly of the Andor CCD camera and the filter wheel is now under designing process. We expect that the manufacturing of the focal reducer system as well as its optical test will be finished by April 2010.

• 천문학논총
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• 제30권2호
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• pp.389-392
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• 2015

We identify a strong lensing galaxy in the cluster IRC 0218 that is spectroscopically confirmed to be at z = 1.62, making it the highest-redshift strong lens galaxy known. The lens is one of the two brightest cluster galaxies and lenses a background source galaxy into an arc and a counterimage. With Hubble Space Telescope (HST) grism and Keck/LRIS spectroscopy, we measure the source redshift to be $z_S=2.26$. Using HST imaging, we model the lens mass distribution with an elliptical power-law profile and account for the effects of the cluster halo and nearby galaxies. The Einstein radius is $^{\theta}E=0.38^{+0.02{\prime}{\prime}}_{-0.01}$ ($3.2^{+0.2}_{-0.1}kpc$) and the total enclosed mass is $M_{tot}(<^{\theta}_E)=1.8^{+0.2}_{-0.1}{\times}10^{11}M_{\odot}$. We estimate that the cluster environment contributes ~ 10% of this total mass. Assuming a Chabrier IMF, the dark matter fraction within $^{\theta}E$ is $f^{Chab}_{DM}=0.3^{+0.1}_{-0.3}$, while a Salpeter IMF is marginally inconsistent with the enclosed mass ($f^{Salp}_{DM}=-0.3^{+0.2}_{-0.5}$).

• 한국광학회지
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• 제7권3호
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• pp.183-190
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• 1996

적외선, 가시광선 겸용의 3반사망원경계를 설계하기 위하여 형상설계법 및 3차수차의 보정방법이 연구되었다. 적외선용의 광학계는 3반사경계만으로 구성되었으며 원추곡면화를 통하여 구면수차, 코마, 비점수차를 보정하였다. 가시광선용의 광학계는 적외선용의 3반사경계의 상면앞에 보정렌즈를 추가하여 상면만곡을 보정하였다. 설계된 3반사망원경계는 파장 10.mu.m에서는 시계 2.4.deg. 내에서 회절한계의 결상성능을 가지고 있다. 가싣광선대역의 단파장에 대한 rms spot size는 3.deg. 시계내에서 25.mu.m이하이며, CCD의 사용에 적합하도록 flat field 조건을 만족하고 있다.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 2005년도 Proceedings of ISRS 2005
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• pp.213-216
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• 2005

A novel hyperspectral imaging spectrometer controlling spatial and spectral resolution individually has been proposed. This imaging spectrometer uses a zoom lens as a telescope and a focusing element. It can change the spatial resolution fixing the spectral resolution or the spectral resolution fixing the spatial resolution. Here, we report the concept of the hyperspectral imaging spectrometer with the novel zooming function and the optical design of a zoom lens as the focusing element. By using lens module and third-order aberration theory, we have presented the initial design of four-group zoom lens with external entrance pupil. And the optimized zoom lens with a focal length of 50 to 150 mm is obtained from the initial design by the optical design software. As a result, the designed zoom lens shows satisfactory performances in wavelength range of 450 to 900 nm as a focusing element in an imaging spectrometer. Furthermore, the collimator lens of the imaging spectrometer is designed through the third-order aberration correction by using an iterative process.

• 한국지구과학회지
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• 제30권7호
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• pp.855-868
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• 2009

본 연구의 목적은 망원경에서 별빛이 결상되는 원리를 교사들이 어떻게 이해하고 있는지를 알아보고자 하는 것이다. 경기도와 서울지역의 지구과학 교사 101명을 대상으로 설명식 지필문항 검사를 수행하고, 지구과학교육 전공자 3명이 교차분석을 실시하였다. 대부분의 교사들이 볼록렌즈에서 상이 형성되는 과정에 대한 체계적인 개념을 가지고 있지 않았고, 특히 상의 개념과 스크린의 역할에 대한 이해가 많이 부족하였다. 또한 망원경에서 별빛이 결상되는 원리에 대한 과학적 개념을 가지고 있는 교사는 참여교사의 3%로 극히 낮았으며 거의 대부분의 교사들이 볼록렌즈나 빛의 단편적인 성질을 이용하여 별빛의 결상을 이해를 시도하는 비과학적 혹은 대체개념을 가지고 있는 것으로 나타났다.

• 천문학논총
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• 제22권4호
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• pp.201-209
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• 2007

We have preliminarily designed two infrared optical systems of the multi-purpose infrared camera system (MIRIS) which is the main payload of STSAT-3. Each optical system consists of a Cassegrain telescope, a field lens and a 1:1 re-imaging lens system that is essential for providing a cold stop. The Cassegrain telescope is identical for both of two infrared cameras, but the field correction lens and re-imaging lens system are different from each other because of different bands of wavelength. The effective aperture size is 100mm in diameter and the focal ratio is f/5. The total length of the optical system is 300mm and the position of the cold stop is 25mm from the detector focal plane. The RMS spot size is smaller than $40{\mu}m$ over the whole detector plane.

• 한국광학회지
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• 제7권3호
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• pp.191-195
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• 1996

대기오염 연구용 이동형 라이다의 광계통을 설계하였다. 대기오염이나 오종층의 측정을 위해 라이다를 사용하며 군에서는 화생방 오염 측정에도 사용된다. 역 Cassegrain형의 시준기로 평행광을 만들어 평면경에 의해 전송하는 레이저광속과 수신 망원경의 광축이 일치하게 된다. 레이저광속은 대기로 향하여 전송되며 측정하고자 하는 물질에 의해 산란되어 수신 망원경으로 되돌아 온다. 주사반사경은 수직으로 60.deg. 수평으로 180.deg.회전되며 주사한다. 주사반사경은 수신망원경과 분리되어 자동차 지붕위에 설치된다. 수신된 레이저광은 공간주파수 여과기에 의해 여과되고, fabri렌즈에 의해 평행광으로 되어 광속분리기에 의해 2개의 광속으로 나뉘어 검출된다. 각 레이저광은 PM관에 의해 검출되어 증폭되고 분석된다.