• 대한전자공학회논문지SP
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• 제42권4호
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• pp.127-132
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• 2005

가상현실을 이용한 사람의 빠른 움직임을 추출하여 파형으로 나타내는 동작곡선이나 자연계에서 실제로 관측되는 대기 전기변동량과 같은 전자계 신호의 시간 변동량은 매우 복잡하다. 이러한 신호의 관측파형에 대하여 변곡점과 같은 신호의 특징을 정확히 결정하는 것이 중요하다. 잡음이 신호에 중첩될 때 종래의 방법으로는 변곡점의 검출이 어렵다. 본 논문에서는 신호에 잡음이 첨가될 때 웨이브릿 임계치 잡음제거와 정규형 자연관측필터를 적용하여 정확한 변곡점 추출이 가능함을 보인다.

• 한국정보통신학회:학술대회논문집
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• 한국해양정보통신학회 2005년도 춘계종합학술대회
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• pp.635-638
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• 2005

전자계 신호의 시간 변동량을 추출하여 파형으로 나타내는 동작곡선 등은 그 형태가 매우 복잡하다. 이러한 신호의 관측파형에 대하여 특징을 나타내는 변곡점과 같은 신호의 특정 시간을 정확히 결정하는 것이 중요하다. 이러한 특징을 검출하는데 흔히 필터를 설계하여 사용하게 된다. 특히 잡음이 신호에 중첩될 때 자연관측필터를 적용하면 변곡점 추출이 가능하다. 본 논문에서는 잡음이 혼재될 경우에 변곡점의 양호한 추출을 위하여 최적의 차수의 자연관측필터 설계방법을 제안 한다.

• 천문학논총
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• 제30권2호
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• pp.223-224
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• 2015

We present the results of visual double stars speckle observations from 2013 using a Zeiss Double Refractor 60 cm with visual focal length f = 1,078 cm, and CCD SBIG ST-402 MEA. A Bessel V filter with ${\lambda}=550nm$ was placed in front of the CCD camera to reduce the chromatic aberration of the objective lens. The objects selected for this observation were calibration candidates and program stars with separations ranging from 0.9-6 arc second, and were located in both the northern and southern hemispheres. Seeing at Bosscha Observatory is generally 1-2 arc second, imposing a limit on visual double star separation below which the system cannot be resolved by long exposure imaging (longer than ~50 ms). Speckle interferometry methods are used to resolve double stars with separations below the typical size of seeing effects. A series of images were captured in fast short-time exposures (~50 ms) using a CCD camera. The result of our experiment shows that our system can be used to measure separations of 0.9 arc second (for systems with small ${\Delta}m$) and ${\Delta}m{\approx}3.7$ (for wide systems).

• Journal of Radiation Protection and Research
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• 제12권1호
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• pp.54-60
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• 1987

The quasi-exposure rate and the quasi-effective energy of the natural radiation in the field at 47 monitoring points around nuclear power plants have been studied with the pair filter thermoluminescence dosimeter system. The results of the six years observation showed that the relationship between the quasi-exposure rate $X_q$, and quasi-effective energy $E_q$ can be represented as a hyperbolic function: $X_q=A+C/(E_q-B)$, where the constants A and B correspond to the quasi-exposure rate of cosmic-rays and the minimum quasi-effective energy of natural radiation, respectively. Furthermore, the constant A is in close agreement with the values obtained by using ionization chambers and scintillation detectors. The constant B is approximately 0.68 MeV, closely corresponding to the mean energy of the photons emitted from natural uranium.

• 대한환경공학회지
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• 제35권10호
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• pp.743-748
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• 2013

본 연구의 목적은 수분이 함유된 한지의 수분을 에탄올, 메탄올, 펜탄 등과 같은 비극성물질로 치환하여 한지 여과지를 만드는데 있다. 실험은 적정 비극성물질의 선택 및 적정 건조방법 그리고 제조된 한지여과지의 물리화학적 특성을 알아보기 위하여 수행되었다. 한지 종이필터를 제조하기 위하여 한지에 함유된 수분을 치환하기 위한 최적 물질은 에탄올이었으며 적정한 건조방법은 냉동 후 진공에 의해 수분을 건조하는 냉동건조방법이었다. 냉동건조에 의해 제조된 필터의 겉보기 밀도는 0.11-0.13 g/mL 으로 자연건조방법의 절반 이었으며 공극율은 약 90%로서 다공성을 나타내었다. 전자현미경 관찰결과 자연건조 및 열건조에 의해 제조된 여과지의 섬유는 섬유끼리 매우 가깝게 밀착되어 있었으나 냉동건조에 의해 제조된 섬유는 섬유간에 간격이 이격되어 있었다. 제조된 여과지의 압력손실은 자연건조 및 열건조 여과지보다 냉동건조에 의해 제조된 한지가 매우 낮았으며 BTEX제거효율은 한지의 수분을 비극성 물질에 의해 치환한 것보다 자연건조시킨 한지가 우수하였다.

• Structural Engineering and Mechanics
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• 제36권2호
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• pp.129-147
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• 2010

This study deals with the viability of using a designed geometrical model consists of plane, polar coordinates (PC) and span length in the determination of bridges deformation. The data of a Tianjin Yonghe bridge located in the southern part of China as collected by RTK-DGPS technique and Accelerometer were used in the analysis. Kalman filter and fast Fourier transformation (FFT) analyses were used to determine the frequency. The results indicate that the designed plane and PC geometrical model are easy to calculate the long-time structural deformation monitoring. In addition, the observed frequency using GPS with the rate of 20 Hz doesn't give correction natural frequency of the observation structures.

• Applied Microscopy
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• 제28권4호
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• pp.435-446
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• 1998

It is suggested that Urechis unicinctus is a filler feeder as like many tide and watery invertebrates which filtrate food materials by ciliary movement. However, the structure of the filter is not yet known in U. unicinctus, nor the filtering mechanism is not well understood. This study reveals ciliated epithelial cells in the foregut and the features of the cilia are good accord with that of known filtrating apparatus of other tide animals. This may implies that the foregut is in function of filtration and the food materials are filtrated by the ciliary movement. With the observation of the filtrating apparatus in the foregut, the intestine of U. unicinctus can be functionally compartmented into 3 parts. These are already known midgut and hindgut in function of digestion and respiration respectively, and the foregut in function of filtrating apparatus for foods. The filtrating apparatus of U. unicinctus is composed of the pseudostratified columnar epithelial cells with numerous cilia. The cilia are well differentiated kinocilia with the typical microtubule pattern, kinetosome and cilia roots. There are two kinds of striated cilia roots, the main root and the accessory root. The main root is extended perpendicularly from the cell surface to basement membrane and the short accessory root is branched with an acute angle of about $80^{\circ}$ from the main root at level of basal plate of the kinetosome. The spacial approaches of the main root with the large fused form of mitochondria is one of the characteristic features which might be in structural consideration an intimate association between energy source and energy mass consuming cell organelles.

• 천문학회지
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• 제48권3호
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• pp.177-185
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• 2015

We develop a new auto-guiding system for the Camera for QUasars in the EArly uNiverse (CQUEAN). CQUEAN is an optical CCD camera system attached to the 2.1-m Otto-Struve Telescope (OST) at McDonald Observatory, USA. The new auto-guiding system differs from the original one in the following: instead of the cassegrain focus of the OST, it is attached to the finder scope; it has its own filter system for observation of bright targets; and it is controlled with the CQUEAN Auto-guiding Package, a newly developed auto-guiding program. Finder scope commands a very wide field of view at the expense of poorer light gathering power than that of the OST. Based on the star count data and the limiting magnitude of the system, we estimate there are more than 5.9 observable stars with a single FOV using the new auto-guiding CCD camera. An adapter is made to attach the system to the finder scope. The new auto-guiding system successfully guided the OST to obtain science data with CQUEAN during the test run in 2014 February. The FWHM and ellipticity distributions of stellar profiles on CQUEAN, images guided with the new auto-guiding system, indicate similar guiding capabilities with the original auto-guiding system but with slightly poorer guiding performance at longer exposures, as indicated by the position angle distribution. We conclude that the new auto-guiding system has overall similar guiding performance to the original system. The new auto-guiding system will be used for the second generation CQUEAN, but it can be used for other cassegrain instruments of the OST.

• 천문학회지
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• 제49권1호
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• pp.25-35
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• 2016

Multiple color selection techniques are successful in identifying quasars from wide-field broadband imaging survey data. Among the quasars that have been discovered so far, however, there is a redshift gap at 5 ≲ z ≲ 5.7 due to the limitations of filter sets in previous studies. In this work, we present a new selection technique of high redshift quasars using a sequence of medium-band filters: nine filters with central wavelengths from 625 to 1025 nm and bandwidths of 50 nm. Photometry with these medium-bands traces the spectral energy distribution (SED) of a source, similar to spectroscopy with resolution R ~ 15. By conducting medium-band observations of high redshift quasars at 4.7 ≤ z ≤ 6.0 and brown dwarfs (the main contaminants in high redshift quasar selection) using the SED camera for QUasars in EArly uNiverse (SQUEAN) on the 2.1-m telescope at the McDonald Observatory, we show that these medium-band filters are superior to multi-color broad-band color section in separating high redshift quasars from brown dwarfs. In addition, we show that redshifts of high redshift quasars can be determined to an accuracy of Δz/(1 + z) = 0.002 - 0.026. The selection technique can be extended to z ~ 7, suggesting that the medium-band observation can be powerful in identifying quasars even at the re-ionization epoch.