• Journal of Astronomy and Space Sciences
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• 제27권2호
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• pp.153-160
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• 2010

We modified the optical system of 500 mm wide-field telescope of which point spread function showed an irregularity. The telescope has been operated for Near Earth Space Survey (NESS) located at Siding Spring Observatory (SSO) in Australia, and the optical system was brought back to Korea in January 2008. After performing a numerical simulation with the tested value of surface figure error of the primary mirror using optical design program, we found that the surface figure error of the mirror should be fabricated less than root mean square (RMS) $\lambda$/10 in order to obtain a stellar full width at half maximum (FWHM) below $28\;{\mu}m$. However, we started to figure the mirror for the target value of RMS $\lambda$/20, because system surface figure error would be increased by the error induced by the optical axis adjustment, mirror cell installation, and others. The radius of curvature of the primary mirror was 1,946 mm after the correction. Its measured surface figure error was less than RMS $\lambda$/20 on the table of polishing machine, and RMS $\lambda$/15 after installation in the primary mirror cell. A test observation performed at Daeduk Observatory at Korea Astronomy and Space Science Institute by utilizing the exiting mount, and resulted in $39.8\;{\mu}m$ of stellar FWHM. It was larger than the value from numerical simulation, and showed wing-shaped stellar image. It turned out that the measured-curvature of the secondary mirror, 1,820 mm, was not the same as the designed one, 1,795.977 mm. We fabricated the secondary mirror to the designed value, and finally obtained a stellar FWHM of $27\;{\mu}m$ after re-installation of the optical system into SSO NESS Observatory in Australia.

• 한국광학회지
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• 제32권6호
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• pp.314-322
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• 2021

일반적인 반사식 망원경은 오목 형태의 주경과 볼록 형태의 부경으로 구성되어 있다. 주경은 크기가 크지만 빛을 모아주는 특성으로 반사경의 파면오차 측정이 비교적 용이하다. 반면에 부경은 빛을 퍼트리기 때문에 주경보다 크기는 작지만 측정의 난이도는 더 높다고 할 수 있다. 특히 코시(Korsch) 형태의 망원경에서는 부경의 가운데 영역도 사용하는데 기존의 힌들(Hindle) 측정법으로는 가운데 부분을 측정할 수 없다. 본 논문에서는 크기가 큰 볼록비구면을 측정하기 위해 힌들 정합법(힌들 측정법과 정합법의 결합)을 적용하여 측정하고 이 측정에서 빠지는 가운데 영역은 일반간섭계의 구면파를 이용해 측정하여 두 결과를 합쳐 전체 형상 오차를 획득하는 방법을 제안하고자 한다. 제안한 방법으로 직경 202 mm, 곡률 반경 499 mm, 비구면상수 -4.613의 볼록 비구면의 형상 오차를 측정한 결과 19.5±1.3 nm rms로 측정되었다. 이 결과는 상용 정합 측정 장비로 측정한 결과와 0.7 nm rms의 근소한 차이를 보였고 반사경의 형상 오차가 45도 방향 비점수차를 가지는 것것도 일치하였다. 따라서 본 논문에서 제안한 방법이 볼록 비구면의 전체 영역을 정밀하게 측정하는데 유용함을 알 수 있었다.

• 한국광학회지
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• 제28권6호
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• pp.290-294
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• 2017

카세그레인 망원경은 오목한 주경과 볼록한 부경으로 이루어져있다. 특히 부경의 경우 크기는 작지만 볼록한 형태로 빛을 모두 퍼트려 파면오차 측정이 어렵다. 본 논문에서는 비구면 계수가 여러 개인 볼록비구면 반사경의 파면오차를 Simpson-Oland-Meckel (SOM) 힌들 테스트를 적용하여 측정하였다. 그리고 실험 구성에서 발생하는 계통오차를 분리해내기 위해 QN 절대측정법을 추가로 적용함으로써 힌들 렌즈 제작 및 정렬 오차를 포함한 계통오차를 보정하고 볼록비구면 반사경만의 파면오차를 구하였다. 이렇게 구한 볼록비구면 반사경의 파면오차와 QED사의 ASI (Aspheric Stitching Interferometer)로 측정한 파면오차와 비교한 결과, 모두 $45^{\circ}$ 방향의 비점수차 형태를 가지며 rms 값의 차이가 약 2.5 nm rms 이내로 매우 작음을 확인하였다.

• Journal of the Optical Society of Korea
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• 제20권1호
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• pp.94-100
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• 2016

A novel optical design for high resolution, large field of view (FOV) and multispectral remote sensing is presented. An f/7.3 Korsch and two f/17.9 Cook three-mirror optical systems are integrated by sharing the primary and secondary mirrors, bias of the FOV, decentering of the apertures and reasonable structure arrangement. The aperture stop of the Korsch system is located on the primary mirror, while those of the Cook systems are on the exit pupils. High resolution image with spectral coverage from visible to near-infrared (NIR) can be acquired through the Korsch system with a focal length of 14 m, while wide-field imaging is accomplished by the two Cook systems whose focal lengths are both 13.24 m. The full FOV is 4°×0.13°, a coverage width of 34.9 km at the altitude of 500 km can then be acquired by push-broom imaging. To facilitate controlling the stray light, the intermediate images and the real exit pupils are spatially available. After optimization, a near diffraction-limited performance and a compact optical package are achieved. The sharing of the on-axis primary and secondary mirrors reduces the cost of fabrication, test, and manufacture effectively. Besides, the two tertiary mirrors of the Cook systems possess the same parameters, further cutting down the cost.

• 한국정밀공학회지
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• 제23권5호
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• pp.44-50
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• 2006

This paper describs about the technique of ultra-precision machining for an infrared(IR) camera aspheric mirror. A 200 mm diameter aspheric mirror was fabricated by SPDTM(Single Point Diamond Turning Machine). Aluminum alloy as mirror substrates is known to be easily machined, but not polishable due to its ductility. Aspheric large reflector without a polishing process, the surface roughness of 5 nm Ra, and the form error of ${\lambda}/2\;({\lambda}=632.8\;nm)$ for reference curved surface 200 mm has been required. The purpose of this research is to find the optimum machining conditions for cutting reflector using Al6061-T651 and apply the SPDTM technique to the manufacturing of ultra precision optical components of Al-alloy aspheric reflector. The cutting force and the surface roughness are measured according to each cutting conditions feed rate, depth of cut and cutting speed, using diamond turning machine to perform cutting processing. As a result, the surface roughness is good when feed rate is 1mm/min, depth of cut $4{\mu}m$ and cutting speed is 220 m/min. We could machined the primary mirror for IR camera in diamond machine with a surface roughness within $0.483{\mu}m$ Rt on aspheric.

• 항공우주기술
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• 제10권2호
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• pp.101-104
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• 2011

고해상도 전자광학 탑재체의 주 반사경과 제2 반사경 간 조립 정렬은 전체 카메라 시스템의 조립 단계 중 가장 중요한 단계이다. 제 2 반사경의 정렬에는 파면센서와 콜리메이터를 사용하였는데 간섭계 보다는 크기가 작고 다루기가 편하기 때문이다. 본 논문에서는 고해상도 전자광학 탑재체의 제 2 반사경에 대한 정렬 방법과 절차에 대해 소개 하고자 한다.

• 한국군사과학기술학회지
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• 제17권1호
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• pp.142-148
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• 2014

The mirror which is considered in designing a MFD is off-axis primary one and its dimension is wide 556mm height 345mm. The MFD(Mirror Fixation Device) load specification is generated for the high resolution mirror. The optical WFEs for unit loads are calculated from mirror sensitivity analysis and they are compared with allocated allowable optical WFE. The parasite load for the MFD is calculated from their comparison. The MFD compliant with the parasite load is designed.

• Journal of Astronomy and Space Sciences
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• 제29권3호
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• pp.321-328
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• 2012

We have designed a 30 cm cryogenic space infrared telescope for astronomical observation. The telescope is designed to observe in the wavelength range of 0.5~2.1 ${\mu}m$, when it is cooled down to 77 K. The result of the preliminary design of the support structure and support method of the mirror of a 30 cm cryogenic space infrared telescope is shown in this paper. As a Cassegrain prescription, the optical system of a 30 cm cryogenic space infrared telescope has a focal ratio of f/3.1 with a 300 mm primary mirror (M-1) and 113 mm secondary mirror (M-2). The material of the whole structure including mirrors is aluminum alloy (Al6061-T6). Flexures that can withstand random vibration were designed, and it was validated through opto-mechanical analysis that both primary and secondary mirrors, which are assembled in the support structure, meet the requirement of root mean square wavefront error < ${\lambda}/8$ for all gravity direction. Additionally, when the M-1 and flexures are assembled by bolts, the effect of thermal stress occurring from a stainless steel bolt when cooled and bolt torque on the M-1 was analyzed.

• 대한물리의학회지
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• 제5권3호
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• pp.395-404
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• 2010

Purpose : The object of this study was to examine the effect of motor learning on brain activation depending on the method of motor learning. Methods : The brain activation was measured in 9 men by fMRI. The subjects were divided into the following groups depending on the method of motor learning: actually practice (AP, n=3) group, action observation (AO, n=3) group and motor imagery (MI, n=3) group. In order to examine the effect of motor learning depending on the method of motor learning, the brain activation data were measured during learning. For the investigation of brain activation, fMRI was conducted. Results : The results of brain activation measured before and during learning were as follows; (1) During learning, the AP group showed the activation in the following areas: primary motor area located in precentral gyrus, somatosensory area located in postcentral gyrus, supplemental motor area and prefrontal association area located in precentral gyrus, middle frontal gyrus and superior frontal gyrus, speech area located in superior temporal gyrus and middle temporal gyrus, Broca's area located in inferior parietal lobe and somatosensory association area of precuneus; (2) During learning, the AD groups showed the activation in the following areas: primary motor area located in precentral gyrus, prefrontal association area located in middle frontal gyrus and superior frontal gyrus, speech area and supplemental motor area located in superior temporal gyrus and middle temporal gyrus, Broca's area located in inferior parietal lobe, somatosensory area and primary motor area located in precentral gyrus of right cerebrum and left cerebrum, and somatosensory association area located in precuneus; and (3) During learning, the MI group showed activation in the following areas: speech area located in superior temporal gyrus, supplemental area, and somatosensory association area located in precuneus. Conclusion : Given the results above, in this study, the action observation was suggested as an alternative to motor learning through actual practice in serial reaction time task of motor learning. It showed the similar results to the actual practice in brain activation which were obtained using activation of mirror neuron. This result suggests that the brain activation occurred by the activation of mirror neuron, which was observed during action observation. The mirror neurons are located in primary motor area, somatosensory area, premotor area, supplemental motor area and somatosensory association area. In sum, when we plan a training program through physiotherapy to increase the effect during reeducation of movement, the action observation as well as best resting is necessary in increasing the effect of motor learning with the patients who cannot be engaged in actual practice.

• Journal of the Optical Society of Korea
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• 제13권2호
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• pp.178-183
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• 2009

At the time that the Keck-I 10m telescope was constructed in 1993, the era of Very Large Telescopes (VLTs) was opened. Now thirteen VLTs are in operation, and the largest of the monolithic mirrors is 8.4 m in diameter. Such monolithic mirrors are mostly aspheric and require high accuracies on the surface figures, reaching up to the diffraction limit. At present, next generation telescopes, Giant telescopes, are being developed. One is the GMT (Giant Magellan Telescope) whose size is 25.4 m in diameter. The primary mirror consists of seven segments figuring elliptical shapes on the surface. The surrounding six segments are off-axis and the edges are steep, as the fast focal ratio is adopted. It means that testing of the mirrors is a challenging task. In this paper, testing methods for the GMT primary mirror are reviewed, and accuracy of measuring devices is assessed. Results and discussions follow.