• Publications of The Korean Astronomical Society
• /
• v.19 no.1
• /
• pp.65-70
• /
• 2004

An imaging spectrograph concept optimized for extended far-ultraviolet emission sources is presented. Although the design was originally developed for FIMS aboard the first Korean science satellite STSAT-l launched on September 27, 2003, no rigorous theoretical background of the spectrograph design has been published. The spectrograph design employs an off-axis parabolic cylinder mirror in front of a slit that guides lights to a diffraction grating. The concave grating provides moderate spatial resolution over a large field of view. This mapping capability is absent in most astronomical instruments but is crucial to the understanding of the nature of a variety of astrophysical phenomena. The aberration theory presented in this paper can be extended to holographic gratings in order to improve the spatial as well as the spectral resolutions.

• Proceedings of the Optical Society of Korea Conference
• /
• 2001.02a
• /
• pp.86-87
• /
• 2001

Far-ultraviolet IMaging Spectrograph(이하 FIMS)는 2002년에 발사 예정인 과학위성 1호의 주 탑재체이며, 은하 주변에 분포한 고온의 가스에서 방출되는 자외선 영역 (short wavelength band ： 900-1150 $\AA$, long wavelength band ： 1335-1750$\AA$)의 방출선을 약 2$\AA$의 분광 분해능으로 관측하는 천문학적 목표를 가지고 있다 일반적인 망원경을 사용하는 대신 제한된 위성의 크기 내에서, 넓은 지역에 퍼져 있는 가스의 분포와 특성을 관측하는데 적합하도록, 그림 1과 같이 비축 포물 원통 반사경과 타원형의 substrate를 가진 회절 에돌이발 (grating)의 사용을 고안하였다. (중략)

• Publications of The Korean Astronomical Society
• /
• v.32 no.1
• /
• pp.359-361
• /
• 2017

We report our research on aluminum mirror optics for future infrared astronomical satellites. For space infrared missions, cooling the whole instrument is crucial to suppress the infrared background and detector noise. In this aspect, aluminum is appropriate for cryogenic optics, because the same material can be used for the whole structure of the instrument including optical components thanks to its excellent machinability, which helps to mitigate optical misalignment at low temperatures. We have fabricated aluminum mirrors with ultra-precision machining and measured the wave front errors (WFEs) of the mirrors with a Fizeau interferometer. Based on the power spectral densities of the WFEs, we confirmed that the surface accuracy of all the mirrors satisfied the requirements for the SPICA Coronagraph Instrument. We then integrated the mirrors into an optical system, and examined the image quality of the system with an optical laser. As a result, the total WFE is estimated to be 33 nm (rms) from the Strehl ratio. This is consistent with the WFEs estimated from the measurement of the individual mirrors.

• The Bulletin of The Korean Astronomical Society
• /
• v.36 no.2
• /
• pp.155.1-155.1
• /
• 2011

The Korea Astronomy and Space Science Institute (KASI) and the Department of Astronomy at the University of Texas at Austin (UT) are developing a near infrared wide-band high resolution spectrograph, IGRINS (Immersion Grating Infrared Spectrograph). The white-pupil design of the instrument optics uses 7 cryogenic mirrors including 3 aspherical off-axis collimators and 4 flat fold mirrors. Two of the 3 collimators are H- and K-band pupil transfer mirrors and they are designed as compensators for the system alignment in each channel. Therefore, their mount design will be one of the most sensitive parts in the IGRINS optomechanical system. The other flat fold mirrors are designed within the limited area. Each of those includes the features of 3 axial hard points and 2 radial hard points with one spring plunger in order for the proper deflection of the mirror. The design work will include the computer-aided 3D modeling and finite element analysis (FEA) to optimize the structural stability and the thermal behavior of the mount models. The mount body will also include a tip-tilt and translation adjustment mechanism to be used as the alignment compensators.

• The Bulletin of The Korean Astronomical Society
• /
• v.40 no.1
• /
• pp.82.3-83
• /
• 2015

비축 반사경의 DTM (Diamond Turning Machine) 가공을 하기 전에는 시간 및 비용의 절감을 위해 CNC(Computerized Numerically Controlled Machine Tools)를 이용하여 비축면의 곡률반경과 가장 유사한 형태의 구면으로 1차 가공 후 3축 이상을 제어할 수 있는 MC (Machining Center)를 이용하여 근사한 비축면을 먼저 가공한다. 이후 DTM으로 광학계에서 요구하는 형상 정밀도 및 표면 조도를 만족하는 비축면을 완성한다. 하지만 비축면을 가공하는 경우, 일반적인 축 대칭 광학계와 달리 가공장비에 장착된 기상계측기를 사용할 수 없기 때문에 외부 장비를 이용하여 반사경 표면을 측정해야한다. 이때 측정과 가공 단계 사이에서 정렬오차가 발생하여 반사경의 형상 정밀도 향상을 위한 보상가공에 어려움이 있다. 본 연구에서는 비축면 반사경의 가공과 측정 과정 사이에 발생하는 정렬오차를 최소화 할 수 있는 DTM 가공용 지그를 설계 및 제작하였다. 또, DTM으로 가공한 반사경의 측정값과 설계값을 비교하여 알루미늄 반사경의 광학 성능을 평가하였다. 이러한 성능 평가 결과는 비축면 반사경의 형상 보상가공을 위한 모델링 방법을 고안하는데에 있어 핵심 자료가 될 것이다.

• Bulletin of the Korean Space Science Society
• /
• 2011.04a
• /
• pp.30.4-31
• /
• 2011

The Korea Astronomy and Space Science Institute (KASI) and the Department of Astronomy at the University of Texas at Austin (UT) are developing a near infrared wide-band high resolution spectrograph, IGRINS (Immersion Grating Infrared Spectrograph). The white-pupil design of the instrument optics uses 7 cryogenic mirrors including 3 aspherical off-axis collimators and 4 flat fold mirrors. Two of the 3 collimators are H- and K-band pupil transfer mirrors and they are designed as compensators for the system alignment in each channel. Therefore, their mount design will be one of the most sensitive parts in the IGRINS optomechanical system. The design work will include the computer-aided 3D modeling and finite element analysis (FEA) to optimize the structural stability of the mount models. The mount body will also include a tip-tilt and translation adjustment mechanism to be used as the alignment compensators.

• Publications of The Korean Astronomical Society
• /
• v.15 no.spc1
• /
• pp.119-126
• /
• 2000

The BOES (BOAO Echelle Spectrograph), a fiber-fed echelle spectrograph of the BOAO 1.8 m telescope, has been designed and now is being manufactured. The BOES follows a white pupil design collimated with two off-axis parabolic mirrors. The 136mm collimating beam leaving the 41.59 grooves/mm R4 echelle grating is refocused near the narrow folding mirror. Through the two cross-disperser prisms and $\phi250 mm(f/1.5)$ transmission camera, the beam images on EEV $2k\times4k$ CCD. The BOES can take the wavelength range of 3700 to $10100{\AA}$ at a single spot with spectral resolution R = 20000 to 40000 depending on the fiber set employed. We describe the key sciences and performance, current status of construction, and future plan of the BOES.

• The Bulletin of The Korean Astronomical Society
• /
• v.35 no.2
• /
• pp.61.2-61.2
• /
• 2010

CQUEAN (Camera for Quasars in EArly uNiverse) is an optical CCD camera system which has its own auto-guiding system. Guiding system consists of a 1k*1k CCD camera, FLI PL1001E, a flat mirror to feed the image of an off-axis field to the camera and baffle. The whole system lies on a moving arm which rotates 90 degree effectively to enlarge the field of view. A motor, IMS MDRIVE 34, and a differential decelerator, APEX AD140-050, are used for the moving mechanism. Auto-guiding is controlled by Agdr program. We had a first light from Aug. 10 to Aug 17, 2010 at McDonald Observatory, USA. In this presentation, we describe about the auto-guiding system for CQUEAN and its performance on the 2.1m telescope.

• The Bulletin of The Korean Astronomical Society
• /
• v.36 no.2
• /
• pp.87.1-87.1
• /
• 2011

Since early 90's, the solar X-ray telescopes such as Yohkoh SXT and Hinode XRT have observed coronal magnetic structures on the Sun's surface in the range of about $40'{\times}40'$ field-of-view (FOV) covering the full solar disk. Thus it has been stressed by the scientists that the optical structure of solar telescopes should be designed with care for improving the uniformity over a wide FOV. There would be, however, no unique solution in designing the optical system of a telescope for overcoming perfectly the problem of off-axis response variation. As a consequence, the correction of optical imperfectness of telescopes has become an important calibration step that should be performed beforehand when the observed images are to be used for photometric purposes. In particular, a special care should be taken when performing the temperature analysis with thin and thick filters for flaring activities observed at the periphery of the full FOV. From the analyses of both pre-launch calibration and in-flight observation data, the optical characteristics for describing the performance of solar X-ray telescopes, especially in view of their energy dependence, will be introduced and discussed in our presentation.

• Current Optics and Photonics
• /
• v.2 no.4
• /
• pp.348-355
• /
• 2018

How to measure the creepage distance of an insulator quickly and accurately is a problem for the power industry at present, and the noticeable concern is that the high voltage insulation equipment cannot be measured online in the charged state. In view of this situation, we develop an on-line measurement system of creepage distance for high voltage insulators based on binocular stereo vision. We have proposed a method of generating linear structured light using a conical off-axis mirror. The feasibility and effect of two ways to solve the interference problem of strong sunlight have been discussed, one way is to use bandpass filters to enhance the contrast ratio of linear structured light in the images, and the other way is to process the images with adaptive threshold segmentation and feature point extraction. After the system is calibrated, we tested the measurement error of the on-line measurement system with a composite insulator sample. Experimental results show that the maximum relative error is 1.45% and the average relative error is 0.69%, which satisfies the task requirement of not more than 5% of the maximum relative error.