논문에서는 하천 수위 감지용 CCD카메라에서 입력된 동영상에서 다리 기둥 영역과 물 영역을 구분하여 수위를 감지하는 방법을 제안한다. 하천 영상에서는 다리 기둥이 있고 그 사이로 강물이 흐르기 때문에, 물이 흐르는 부분에서만 강한 움직임이 발생하게 된다. 따라서, 본 논문에서는 optical flow를 사용하여 강물의 움직임을 감지하고 움직임이 감지된 픽셀들을 Y축으로 투영시켜 움직임 누적 히스토그램을 생성한다. 이후, 생성된 움직임 누적 히스토그램에 대해 K-means 군집화를 적용 시킨다. 단순히 기둥 영역과 물 영역을 구분하기 위해서는 K=2인 K-means 군집화를 수행하면 되지만, 기둥 영역과 물보라가 심한 부분, 물이 잔잔하게 흐르는 부분으로 나누기 위해서 K=3인 K-means 군집화를 수행한다. K-means 군집화에 의해 3개의 군집으로 나뉜 히스토그램에서 위쪽 첫 번째 군집과 두 번째 군집의 경계를 검출하면 그 부분이 곧 하천의 수위가 된다. 본 논문에서는 K=2, K=3일 경우의 K-means 군집화를 사용한 방법과 기존의 CCD카메라 기반의 수위감지알고리즘을 비교 실험하였고, 실험 결과 기존의 연구보다 움직임백터와 K-means 군집화 방법을 결합한 방법이 가장 좋은 성능을 보여 주었다.

본 논문은 움직이는 객체를 지속적으로 감시관찰하는 CCD 카메라의 자동 제어를 위한 신호 생성 알고리즘을 제시하고 있다. 제안된 알고리즘은 검출된 객체 위치와 영상 중심 사이의 수평 수직 변위들을 계산하고 변위들을 각으로 변환한다. 최종적으로 팬/틸트 신호가 변위각으로부터 생성된다. 제안된 알고리즘의 성능 평가를 위해 자동 제어에서 생성된 데이터와 수동 제어에서 측정된 데이터가 비교되고, 단순한 객체를 이용한 추적 실험이 수행되었다. 실험 결과는 두 데이터의 차이는 무시할 수 있을 정도이고, 팬/틸트 ±52o/±40o 영역에서 움직이는 객체가 ±13o/±10o 영역에 유지되는 것을 보여주고 있다.

We have been developing a solar observing system based on a fast CCD camera 1M30P made by the DALSA company. Here we examine and present the characteristics and performance of the camera. For this we have analyzed a number of images of a flat wall illuminated by a constant light source. As a result we found that in the default operating mode 1) the mean bias level is 49 ADU/pix, 2) the mean dark current is about 8 ADU /s/pix, 3) the readout noise is 1.3 ADU, and 4) the gain is about 42 electrons/ ADU. The CCD detector is found to have a linearity with a deviation smaller than 6%, and a uniform sensitivity better than 1%. These parameters will be used as basic inputs in the analysis of data to be taken by the camera.

The characteristics of the BOES (Bohyunsan Observatory Echelle Spectrograph) CCD camera is presented. In order to get optimum gain and readout noise of the CCD, we examine the variation of the gain and readout noise by changing the value of output drain voltage of the CCD and measuring the gain using transfer curve, which is defined as the plot of variance versus mean exposure level of a homogeneous light onto the CCD surface. The gain and readout noises are optimised to be 0.5e −/ADU and 3e−, which is good for highest signal-to-noise ratio and contrast for the low light level characteristics of the BOES. We also measure the dark count of the CCD by getting five dark images with 3600 seconds exposure time. The mean dark count from median stacked dark images is essentially zero. A table of positions of defected pixels is also presented.

A CCD camera for the BOES (Bohyunsan Observatory Echelle Spectrograph) has been developed. The camera consists of a 2048 × 4096 format CCD, a SDSU Gen-I CCD controller, and a continuous flow cryostat (CFC) designed by the ESO. In order to control the CCD under SDSU Gen-I controller, the voltage level of all the biases and clocks were lowered by -6V. The CFC showed cooling time of about 10 hour, after which the chip temperature settled down with variation less than ±1°C. The final chip temperature is around -105 °C with the setting value for the CFC as -170 °C

We developed a CCD camera that can observe wide fields on the sky. We tested the field of views using various lenses. For cooling the CCD chip, we used a thermoelectric cooling device and tested the cooling efficiency. This camera will continuously observe a part of the sky. The data from the camera will be used to decide the current weather condition by the real-time star counting program (SCount) which will be developed later.

We developed an observation program for a 2K CCD camera, which was newly attached at the SOAO (Sobaeksan Optical Astronomy Observatory) 61cm telescope. The program was designed to control the telescope as well as the CCD camera and to monitor the CCD image quality, with very easy under the window-based graphical user interface (GUI). Furthermore, applying the automated differential photometric algorithm, we can obtain the instrumental magnitudes of several variable and comparison stars in real-time. Simultaneous photometry enables us to get precise differential magnitudes of variable stars even if the weather condition is not photometric. This new observation system has been using for many astronomical observations from September, 2001.

We present the characteristics of the 2K CCD camera at the Bohyunsan Optical Astronomy Observatory of the Korea Astronomy Observatory at the time of its development. The purpose of this paper is to support the observers who may need detailed information on the characteristics of the camera and to provide helpful information on the optimization' of a CCD camera for those who try to develop their own camera. The 2K CCD camera was optimized to have a gain of 1.8e−/ADU and a read out noise of 7e− from an experiment using radioactive 55 Fe X-ray source. The charge transfer efficiency was measured as 0.9999976 for serial and 0.9999942 for parallel direction, which means 0.5% charge loss along the serial direction and 1.2% along the parallel direction across the chip. The quantum efficiency of the camera was measured from an experiment using a homogeneous light source consisting of a halogen lamp and an integrating sphere with a monochromator. The resulting quantum efficiency of the camera peaked at the wavelength range 600-700 nm with the value of ＼-0.89 .

We have developed and tested a CCD camera (100 × 100 pixels) system for observing Ha images of the solar flares with time resolution> 25 msec. The 512 × 512 pixels image of CCD camera at 2 Mpixels/sec can be recorded at the rate of more than 5 frame/sec while 100 × 100 pixels area image can be obtained 40 frames/sec. The 100 × 100 pixels image of CCD camera corresponds to 130 × 130 arc - sec2 of the solar disk.

A new CCD camera equipped with a large format chip is now under construction for the Kiso 105-cm Schmidt telescope. We use SITe TK2048E, of which pixel size is 24 μm and chip size is 48 mm square. TK2048E is thinned back-illuminated so that it has high sensitivity in U-band. The chip is cooled by a refrigerator instead of liquid nitrogen. MESSIA III is used as CCD control system.

The development of universal CCD camera control software for all BOAO CCD camera systems is proposed. The new software, running under Sun SPARCstation and motif based X window system with SunOS 4.1.3 operating system, replaces existing control software based on NeXTstation color and NeXTstep 2.1 operating system which is no more produced now. Several new features of the new software is introduced, some of which are 1) the image contrast is enhanced by color manipulation and display, 2) image zooming and trimming, 3) any size of image can be displayed in the scrolled window, and 4) the offset between telescope pointing position and CCD center is easily calculated by alt-azi map. Along with the above new features, the new software has advantages including ease of maintenance and upgrading and elimination of risk caused by hardware damage. Since September 1, the software beta version is being used by observers and there is not seen severe problem regarding the software itself, but several requests to equip more features to the software will be mirrored to future release.

The characterization of detectors installed in space- and ground-based instruments is important to evaluate the system performance. We report the development of a detector performance test system for astronomical applications using the Andor iKon M CCD camera. The performance test system consists of a light source, monochromator, integrating sphere, and power meters. We adopted the Czerny–Tuner monochromator with three ruled gratings and one mirror, which covers a spectral range of 200–9,000 nm with a spectral resolution of ~1 nm in the visible region. Various detector characteristics, such as the quantum efficiency, sensitivity, and noise, can be measured in wide wavelength ranges from the visible to mid-infrared regions. We evaluated the Korea Astronomy and Space Science Institute (KASI) detector performance test system by using the performance verification of the Andor iKon-M CCD camera. The test procedure includes measurements of the conversion gain (2.86 e−/ADU), full well capacity (130 K e−), nonlinearity, and pixel defects. We also estimated the read noise, dark current, and quantum efficiency as a function of the temperature. The lowest measured read noise is 12 e−. The dark current at 223 K was determined to be 7 e−/s/pix and its doubling temperature is 5.3°C ± 0.2°C at an activation energy of 0.6 eV. The maximum quantum efficiency at 223 K was estimated to be 93 % ± 2 %. We proved that the quantum efficiency is sensitive to the operating temperature. It varies up to 5 % in the visible region, while the variation increases to 30 % in the near-infrared region. Based on the comparison of our results with the test report by the vendor, we conclude that our performance test results are consistent with those from the vendor considering the test environment. We also confirmed that the KASI detector performance test system is reliable and our measurement method and analysis are accurate.