• Journal of Information Technology Applications and Management
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• 제12권1호
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• pp.231-239
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• 2005

This paper describes a new algorithm for pixel-based skin color detection to differentiate human form in color images by the ratio of R to H. In order to detect skin color efficiently, we examine the distribution of the R, G and B color elements combining to constitute the skin color in various color images. It shows that R is located in a narrower area than G and B on the RGB color space. And skin color is more related to R than G and B. Meanwhile, when the color image is transformed to the HSI color space, the S is variously changed in accordance with skin colors. The I is changed in accordance with the quantity and angle of light. But the H is less influenced by other conditions except for color. On the basis of the aforementioned study, we propose that the threshold for skin color detection is decided by the ratio of R to H. The proposed method narrows down the range of threshold, detects more skin color and reduces mis-detection of skin color in comparison to detection by R or H. In experimentation. it shows that the proposed algorithm overcomes changes of brightness and color to detect skin color in color images.

• 천문학회보
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• 제44권2호
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• pp.58.1-58.1
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• 2019

We have developed Ground Software (GSW) of BITSE. The ground software includes mission operation software, data visualization software and data processing software. Mission operation software is implemented using COSMOS. COSMOS is a command and control system providing commanding, scripting and data visualization capabilities for embedded systems. Mission operation software send commands to flight software and control coronagraph. It displays every telemetry packets and provides realtime graphing of telemetry data. Data visualization software is used to display and analyze science image data in real time. It is graphical user interface (GUI) and has various functions such as directory listing, image display, and intensity profile. The data visualization software shows also image information which is FITS header, pixel resolution, and histogram. It helps users to confirm alignment and exposure time during the mission. Data processing software creates 4-channel polarization data from raw data.

• 천문학회보
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• 제39권1호
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• pp.52.2-52.2
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• 2014

The Immersion Grating Infrared Spectrometer (IGRINS) is an unprecedentedly minimized infrared cross-dispersed echelle spectrograph with a high-resolution and high-sensitivity optical performance. A silicon immersion grating features the instrument for the first time in this field. IGRINS will cover the entire portion of the wavelength range between 1.45 and $2.45{\mu}m$ accessible from the ground in a single exposure with spectral resolution of 40,000. Individual volume phase holographic (VPH) gratings serve as cross-dispersing elements for separate spectrograph arms covering the H and K bands. On the 2.7m Harlan J. Smith telescope at the McDonald Observatory, the slit size is $1^{\prime\prime}{\times}15^{\prime\prime}$. IGRINS has a $0.27^{\prime\prime}$ pixel-1 plate scale on a $2048{\times}2048$ pixel Teledyne Scientific & Imaging HAWAII-2RG detector with SIDECAR ASIC cryogenic controller. The instrument includes four subsystems; a calibration unit, an input relay optics module, a slit-viewing camera, and nearly identical H and K spectrograph modules. The use of a silicon immersion grating and a compact white pupil design allows the spectrograph collimated beam size to be 25mm, which permits the entire cryogenic system to be contained in a moderately sized rectangular vacuum chamber. The fabrication and assembly of the optical and mechanical hardware components were completed in 2013. In this presentation, we describe the major design characteristics of the instrument and the early performance estimated from the first light commissioning at the McDonald Observatory.

• 천문학회지
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• 제42권3호
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• pp.61-69
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• 2009

Transverse velocity vectors can be determined from a pair of images successively taken with a time interval using an optical flow technique. We have tested the performance of the new technique called NAVE (non-linear affine velocity estimator) recently implemented by Chae & Sakurai using real image data taken by the Narrowband Filter Imager (NFI) of the Solar Optical Telescope (SOT) aboard the Hinode satellite. We have developed two methods of estimating the errors in the determination of velocity vectors, one resulting from the non-linear fitting ${\sigma}_{\upsilon}$ and the other ${\epsilon}_u$ resulting from the statistics of the determined velocity vectors. The real error is expected to be somewhere between ${\sigma}_{\upsilon}$ and ${\epsilon}_u$. We have investigated the dependence of the determined velocity vectors and their errors on the different parameters such as the critical speed for the subsonic filtering, the width of the localizing window, the time interval between two successive images, and the signal-to-noise ratio of the feature. With the choice of $v_{crit}$ = 2 pixel/step for the subsonic filtering, and the window FWHM of 16 pixels, and the time interval of one step (2 minutes), we find that the errors of velocity vectors determined using the NAVE range from around 0.04 pixel/step in high signal-to-noise ratio features (S/N $\sim$ 10), to 0.1 pixel/step in low signa-to-noise ratio features (S/N $\sim$ 3) with the mean of about 0.06 pixel/step where 1 pixel/step corresponds roughly to 1 km/s in our case.

• Journal of Astronomy and Space Sciences
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• 제40권4호
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• pp.149-171
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• 2023

ShadowCam is a National Aeronautics and Space Administration Advanced Exploration Systems funded instrument hosted onboard the Korea Aerospace Research Institute (KARI) Korea Pathfinder Lunar Orbiter (KPLO) satellite. By collecting high-resolution images of permanently shadowed regions (PSRs), ShadowCam will provide critical information about the distribution and accessibility of water ice and other volatiles at spatial scales (1.7 m/pixel) required to mitigate risks and maximize the results of future exploration activities. The PSRs never see direct sunlight and are illuminated only by light reflected from nearby topographic highs. Since secondary illumination is very dim, ShadowCam was designed to be over 200 times more sensitive than previous imagers like the Lunar Reconnaissance Orbiter Camera Narrow Angle Camera (LROC NAC). ShadowCam images thus allow for unprecedented views into the shadows, but saturate while imaging sunlit terrain.

• 한국정보기술응용학회:학술대회논문집
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• 한국정보기술응용학회 2005년도 6th 2005 International Conference on Computers, Communications and System
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• pp.153-156
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• 2005

Skin region detection in images is an important process in many computer vision applications targeting humans such as hand gesture recognition and face identification. It usually starts at a pixel-level, and involves a pre-process of color spae transformation followed by a classification process. A color space transformation is assumed to increase separability between skin classes and other classes, to increase similarity among different skin tones, and to bring a robust performance under varying imaging conditions, without any complicated analysis. In this paper, we examine if the color space transformation actually brings those benefits to the problem of skin region detection on a set of human hand images with different postures, backgrounds, people, and illuminations. Our experimental results indicate that color space transfomation affects the skin detection performance. Although the performance depends on camera and surround conditions, normalized [R, G, B] color space may be a good choice in general.

• 천문학회보
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• 제39권1호
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• pp.71.1-71.1
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• 2014

To investigate physical properties of Solar pores, we use SDO/HMI data from 2010 to 2013. For this, we select single and isolated pores from the active region (Axx, Bxo, Bxi and Bxc-type) listed in Solar Region Summary. Pore is defined by connected pixels satisfying the intensity threshold from pixel of minimum intensity. We try to obtain area, intensity, magnetic field, and Doppler velocity of pores from HMI data. After removing the effects of orbital motion of the SDO satellite and differential rotation of the Sun, we identify that significant daily variations of Doppler velocity with non-zero ordinates still remain in the umbral region, and the artifact is quite dependent on the strength of magnetic field and radial component of velocity of SDO satellite. In this study we develope empirical model to remove the artifact. A preliminary result on the elimination of the artifact will be presented.

• 전자공학회논문지
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• 제53권5호
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• pp.132-140
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• 2016

본 논문에서는 신뢰 영역을 검출하고 이를 이용하여 미스 매치된 영역에 대한 홀을 채우고 적응적으로 시차 지도를 조정하여 경계를 보존하는 스테레오 정합 방법을 제안한다. 초기 시차 지도 추정을 위해 비용 계산은 색상(CIE Lab)과 경사도(Gradient)를 결합하여 이용하였고, 두 번의 비용 결합 함수를 적용 하여 시차 지도를 추정 하였다. 화소 불일치 영역을 검출하기 위해 왼쪽/오른쪽 교차 검사를 수행 하였다. 두 픽셀 위치에서의 차이가 1보다 크면 폐색 영역이거나 잘못된 매칭으로 판단하고 왼쪽 시차 지도에 표시 하였다. 초기 시차 지도에서 깊이 불연속성으로 인한 에러값을 구별하기 위해 Mean-shift segmentation을 사용하여 신뢰 지도를 구하고 초기 시차 지도 영상에서의 에러값을 줄이기 위해 신뢰 지도 결과를 이용하여 시차 지도 조정을 수행한다. 실험 결과 제안하는 방법이 기존의 다른 방법들과 비교하여 비교적 높은 정확도를 보이는 시차 지도를 생성 하는 것을 보였다.

• Journal of Astronomy and Space Sciences
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• 제19권1호
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• pp.39-46
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• 2002

보현산천문대의 1.8m 망원경과 CCD 측광장치를 이용하여 1999년 10월 20일 밤에 얻은 V523 Cas 근처의 약 $12'{\times}12'$ 시야를 찍은 124장의 이미지를 처리하여 측광 정밀도를 계산하는 과정에서 ${\Delta}m$ 광도곡선의 기울기가 별 마다 다르다는 사실을 발견하였다. 관련 여러 항목들 간의 인자분석을 함으로서, 그 기울기가 CCD프레임 상의 위치와 관련성이 높음을 알아 내고, 그 결과 CCD의 우하부에서 좌상부 쪽으로 감광감도를 저하시키는 요인이 시간이 흐름에 따라 점점 심하게 작용했다고 보고, 이의 원인으로 CCD 냉각이 균질하지 못하여 서리 같은 것이 서서히 우하부로 부터 좌상부 쪽으로 진행해서 생겼다는 시나리오를 제시했다.

• Journal of Astronomy and Space Sciences
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• 제11권2호
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• pp.320-326
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• 1994

한국과학기술원 인공위성 연구센터에서는 1992년 8월과 1993년 9월에 마이크로 위성인 우리별 1호와 2호를 발사, 운용중이다. 두 위성 모두에는 지표면을 촬영하기 위한 CCD 카메라가 실려있다. 이들 카메라에 쓰여진 렌즈(촛점거리: 50mm)를 평가하기 위해 MTF(Modulation Transfer Function) 측정을 하였다. 실험을 위해 표준과학연구소의 MTF 측정장치를 사용하였으며, f-number와 field angle을 변화시켜 가면서 측정하였다. 측정 결과로부터 f-number가 4.0 보다 작을때, 점광원으로부터 나온 빛이 CCD 칩의 한 화소(pixel) 안으로 들어 간다는 사실을 알 수 있었으며, field angle을 변화시켜가면서 tangential MTF와 sagital MTF를 측정한 결과, field angle이 증가함에 따라 MTF 값이 떨어짐을 알 수 있었다.