• 천문학논총
• /
• 제18권1호
• /
• pp.75-79
• /
• 2003

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.

• 천문학논총
• /
• 제23권1호
• /
• pp.1-12
• /
• 2008

Understanding of the basic characteristics of an astronomical instrument is a prerequisite to obtaining reliable data from the instrument. We have analyzed more than 1,000 calibration images from the Fairchild 486 CCD (hereafter the Maidanak 4k CCD system) attached to the AZT-22 1.5m telescope at Maidanak Astronomical Observatory in Uzbekistan. The Maidanak 4k CCD system supports three readout modes through 1, 2, or 4 amplifiers. In most cases observers use 4-amplifier readout mode to save time. We have tested the stability and seasonal variation of zero levels and confirm that two quadrants of the images (Amp 1 & 2) show no appreciable seasonal variation. but the other two quadrants (Amp 3 & Amp 4) show an evident seasonal variation in the bias level. The Cryo Tiger, the cooling system used at the Maidanak 4k CCD system, maintains the CCD temperature at -108'E, and effectively suppresses the dark electrons. The mean value versus the variance plot of the flat images does not show the expected relation for an ideal Poisson noise distribution and this is attributed to the large variation in quantum efficiency between different pixels. In addition, we confirm that there is no appreciable difference in gain between readout amplifiers, but there is a large variation in quantum efficiency across CCD chip especially in U. Due to the finite length of shutter opening and closing time, the effective exposure time varies across the science images. We introduce two parameters to quantify the effect of this uneven illumination and present a method to remove these effects. We also present a method to remove the interference patterns appearing in the images obtained with longer wavelength filters and investigate the spatial variation of the point spread function.

• 한국광학회지
• /
• 제7권1호
• /
• pp.1-8
• /
• 1996

렌즈의 실시간 성능축정을 위하여 MTF측정장치에 CCD를 많이 사용하고 있다. 본 연구에서는 2차원 CCD를 복사기 렌즈의 실시간 MFT측정장치에 사용했을 때 CCD에 의한 각종 MTF특성을 분석하였다. CCD로 측정한 복사기 렌즈의 MTF는 2차원 CCD의 shift register가 배열된 방향과 셔터 속도, 광신호 증폭회로의 증폭률에 따라 다른 특성을 나타내었다. 광원의 밝기에 의한 MTF 값의 변화를 줄이기 위하여 축상면 및 비축상면에서 복사조도가 균일한 광원장치를 제작하였으며 MTF 값이 측정된 표준렌즈를 사용하여 복사기 렌즈용 실시간 MTF측정장치를 교정하였다.

• 천문학논총
• /
• 제10권1호
• /
• pp.67-78
• /
• 1995

An introduction to the first CCD camera system in Bohyunsan Optica1 Astronomy Observatory(CCD#l) is presented. The CCD camera adopts modular dewar design of IfA(Institute for Astronomy at Hawaii University) and SDSU(San Diego State University) general purpose CCD controller. The user interface is based on IfA design of easy-to-use QUI program running on the NeXT workstation. The characteristics of the CCD#l including Gain, Charge Transfer Efficiency, rms Read-Out Noise, Linearity and Dynamic range is tested and discussed. The CCD#l shows 6.4 electrons RON and gain of 3.49 electrons per ADU, and the optimization resulted in about 27 seconds readout time guaranteeing charge transfer efficiency of 0.99999 for both direction. Linearity test shows that non-linear coefficient is $6{\times}10^{-7}$ in the range of 0 to 30,000 ADU.

• 천문학논총
• /
• 제16권1호
• /
• pp.31-36
• /
• 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 $\~0.89$.

• 천문학회보
• /
• 제37권2호
• /
• pp.222.2-222.2
• /
• 2012

Camera for QUasars in EArly uNiverse (CQUEAN) is an optical CCD camera attached to the 2.1m Otto Struve telescope at the McDonald Observatory, USA. CCD output signal contains the electrons generated by photoionization of incident light and thermal ionization. Therefore reliable photometric result can be obtained only under the stable condition of CCD thermal properties. We investigated the temperature dependency of the various characteristics of CQUEAN CCD chip, including bias level, dark level, gain, and quantum efficiency (QE), with the CQUEAN observation and calibration data obtained during 2012 May run. We discuss the environmental effects, i.e., ambient temperature, as well as CCD temperature on the stability of its characteristics.

• Nuclear Engineering and Technology
• /
• 제33권5호
• /
• pp.514-525
• /
• 2001

Optimum characteristics of digital X-ray sensor components were analyzed to develop intra- oral dental digital X-ray image sensor using indirect method. Parametric analysis was carried out to optimize the phosphor thickness and the fiber optic plate (FOP) coupling to charge coupled device (CCD). X-ray absorption and light diffusion in the phosphor layer were analyzed by the Monte Carlo method. Real time X-ray image was obtained with prototype X- ray image sensor using general CCD camera with 1∼10 Ip/mm resolution. It has been previously shown that large resolution degradation in X-ray images was caused by miss alignment of FOP to CCD and optical adhesive selection. In this study, we reported that X-ray image quality was greatly improved by using optimized characteristics of alignment device and phosphor thickness.

• 천문학회지
• /
• 제37권4호
• /
• pp.185-191
• /
• 2004

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.

• 한국산업정보학회논문지
• /
• 제8권2호
• /
• pp.30-37
• /
• 2003

최근 들어 인터넷 및 TV 홈쇼핑 등을 통한 전자상거래의 활성화로 인하여 소포 및 택배 등의 물류량이 급속도로 늘어나고 있으며, 이의 효율적인 운송을 위하여 우편 물류 시스템의 고도화 기술이 개발되고 있다. 소포 및 택배의 빠른 처리를 위하여 CCD스캐너 시스템이 필요로 하게 된다. 대량의 우편 물량을 효과적으로 처리하기 위하여 CCD 스캐너 영상으로부터 택배 라벨의 주소 영역을 검출하기 위한 자동 시스템이 필요하다. 본 논문에서는 우체국 표준 라벨의 주소 영역을 효과적으로 검출할 수 있는 알고리즘을 제안하였다. 이는 주소 영역의 기하학적인 특징을 이용하였으며, 주소 영역의 고속 검출을 위한 판단 기준을 정의하여, 실시간으로 택배 라벨의 주소 영역을 효과적으로 검출하였다.

• 한국통신학회논문지
• /
• 제12권1호
• /
• pp.9-18
• /
• 1987

DPCM의 선형예측기를 비감광성 원소(dummy pixel)를 가지고 있는 선형 감광성 전하결합소자(CCD)를 광전자 시스템으로 구현하는 방법을 제시하였다. 종래의 시스템과 마찬가지로 이 시스템은 입력광원, 공간여파기(마스크), 선형감광성 CCD의 3부분으로 구성되었다. 비감광성 원소에 의한 시간지연을 고려하여 종래의 마스크를 변형하여 각 예측계수를 하나 이상의 마스크 원소에 분산시킨, 새로운 방식의 분산형 마스크를 제시하고 이 마스크를 사용할 때의 특성을 이론적으로 분석하였으며 실험으로 확인하였다.