• Journal of Astronomy and Space Sciences
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• v.25 no.2
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• pp.101-112
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• 2008

Systematic CCD observations of times of minimum lights for eclipsing binaries has been carried out from 2002 to 2007 at Campus Station of Chungbuk National University Observatory which is located in Cheongju city, Korea. As a by-product of our observations, photometric data for stars in CCD images taken from 2005 to 2007 were used to determine 1st order atmospheric extinction coefficient (hereafter AEC) and seasonal and yearly variations of the AECs were studied. Total nights used for determination of AECs were 57 days in 2005, 51 days in 2006, and 63 days in 2007. As a result the annual mean value of the AECs per air mass is calculated as $0.^m34{\pm}0.^m18$ for 2005, $0.^m38{\pm}0.^m19$ for 2006, and $0.^m45{\pm}0.^m20$ for 2007. These values show that the AECs and their standard deviations are two and four times, respectively, larger than those of normal observatories which are not located near large cities. Annual comparison between concentration of atmospheric fine dust and coefficient of atmospheric extinction show strong correlation between two quantities of which time variations show similar patterns. The AECs for the east sky show larger than those for the west sky. It can be easily understood by the reasonable possibility that air pollutants remain more in the east sky than in the west because the east area of Cheongju city has been more developed than the west one. In conclusion the atmospheric extinction of the night sky of Cheongju city has an annual trend of increase of $0.^m06\;airrnass^{-1}\; year^{-1}$ implying that it may take only about 13 years for Cheongju city to have 2 times brighter night sky than the present one. Our study highlights that variations of AEC can be used as an important indicator of air pollution to monitor night skies.

• Bulletin of the Korean Space Science Society
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• 1992.10a
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• pp.22-22
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• 1992

식쌍성 Algo1과 44i Boo에 대해 각각 두 개의 비교성을 이용하여 광전관측을 수행하여 광도곡선을 얻었다. 색효과는 목적성과 비교성의 색의 차이에 기인한 효과로서 광도곡선상에 체계적인 오차로 남게 된다. 따라서, 자료보정 과정에서 전체 소과계수인 k만으로 보정하게 디면 색효과에 의한 체계적인 오차는 광도곡선상에 그대로 남게 된다. 즉, 쌍성관측에서는 비교성을 목적성과 거의 같은 위치의 것을 택하여 관측하기 때문에 투과 대기량의 차이와 곱해져 등급에 영향을 주는 1차 소광계수에 의한 효과보다는 색의 차에 기인한 2차 소광계수에 의한 효과가 더 크다는 의미이다. 물론 투과 대기량의 크기가 큰 곳에서는 1차 소광계수에 의한 효과도 커지게 된다. Algo1의 경우, 비교성과 점검성을 이용하여 얻은 광도걱선들은 평탄영역에서 이들의 색의 차이 때문에 다르게 나타났으며, 색항을 보정한 결과 두 광도곡선이 거의 유사하게 나타났다. 44i Boo의 경우는 평탄 영역이 거의 보이지 않고, 색에 의한 효과는 광도곡선의 전 영역에 걸쳐 나타났으며, 비교성이 점검성에 비하여 목적성으로부터 더 멀리 떨어진 관계로 k1,k2항이 모두 중요하게 나타났다. 한편, 1,2차 소광 보정 이후에도 날짜에 따라 다른 그림을 보여 준 것은 기기 효과에 기인한 것으로 보여졌으며, 자료에 가장 큰 오차로 기여하는 것은 시간에 따른 대기 상태의 변화이기 때무에 보다 정확한 자료보정을 하기 위해서는 동-서쪽으로 나누어 소광보정을 하는 것이 바람직 할것으로 보여졌다.

• The Bulletin of The Korean Astronomical Society
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• v.33 no.2
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• pp.40.2-40.2
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• 2008

• Publications of The Korean Astronomical Society
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• v.4 no.1
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• pp.53-62
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• 1989

낱별의 광전측광 관측을 위하여 두 가지 컴퓨터 프로그램을 개발하였다. 하나는 자료수집 (data aquisition), 자료의 표시, 통계처리, 오차추정, 대기상태의 모니터링 등을 다루는 실시간(實時間, real time) 측광제어 프로그램이고, 다른 하나는 하룻밤 관측의 도중 또는 관측 종료 직후에 수집된 자료 전체를 입력 파일로 만들어 주면 대기소광계수 결정과 표준계 변환 및 오차 추정을 해 주는 자료분석(資料分析, data reduction) 프로그램이다. 두 프로그램은 모두 임의의 다색측광계(多色測光系)에 대해서 입력 과일에 필터의 갯수, 색지 수의 정의 등 필요한 자료만 써주면 수행 가능하도록 일반화되어 있다.

• Bulletin of the Korean Space Science Society
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• 2008.04a
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• pp.17.4-17.4
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• 2008

• Proceedings of the KSRS Conference
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• 2001.03a
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• pp.85-90
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• 2001

대기복사모델인 MODRAN를 이용해 다목적실용위성 2호 탑재체인 Multispectral Camera (MSC)의 총복사량에 대한 계산을 수행하고 그 결과를 분석해 보았다. 모델계산은 4계절 조건을 모의실험하기 위해 1월 15일, 4월 15일, 7월 15일과 10월 15일에 대해 중위고 동절기 및 하절기, 그리고 US 표준대기를 사용했다. 다목적실용위성 2호 궤도 조건과 각 계절에 대한 대표적인 태양천정각 (solar zenith angle)을 이용하였다. 사정거리는 대류권 에어로솔 소광계수 (tropospheric aerosol extinction)에 해당하는 50 km를 사용하고 지표의 알비도는 맑은 날 지구 연평균 값에 해당하는 0.135가 사용되었다. 위 4개월 평균치로써 연평균 총복사량은 MSC 계약서에 명시된 값들과 상당한 차이를 보였고 심지어 파장에 따른 경향조차도 서로 다름을 알 수 있었다. 가시광선 대역에서 근적외선 대역으로 파장이 증가함에 따라 두 값의 차이가 커짐을 보였다.

• Publications of The Korean Astronomical Society
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• v.12 no.1
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• pp.167-172
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• 1997

Detailed low spectral resolution observations of the spectrum have been made for three early spectral type standard stars, HR718, HR1544, HR3454, respectively, for the wavelength region 4,300 A to 7,500 A, using the Bohyunsan Optical Astronomy Observatory (BOAO) Middle- Dispersion Spectrograph. These standard stars were chosen from well-known bright northern standard stars. All of the observed long slit spectral data has been reduced and analyzed using the IRAF reduction procedure. The derived extinction coefficients are compared with the other observatory result. The derived value can be used in the determination of flux calibration of BOAO spectroscopic observation. However, until the high quality data are secured from a new series of observation in the blue region and are re-analyzed together, the extinction coefficients below the 4,000 A wavelength remains unknown.

• Journal of Korean Society for Atmospheric Environment
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• v.3 no.1
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• pp.27-33
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• 1987

The environment and biological studies of tritium have been carried out in the advanced countries since the mid 1950's. In the case of a potential tritium exposure, the usual procedure is trifium bioassay (as HTO) in human urine in order to determine the amount of tritium deposited in the body called tritium body burden. The maximum permissible body burden(MPBB) of tritium in total body is about $30{\mu}Ci/{\ell}$ for body tissue. In the bioassay, the most common investigation level for detection of tritium in urine is 1/10th of MPBB. For this bioassay project, the first priority is given to obtaining a quench correction curve. This consideration is necessary because of the variability in color of human urine specimens. Quenching effect in this case mainly is caused by the absorption of scintillation light flashes by the urine sample. By the least squares method on the statistical basis, an estimated formula for quench correction curve was determined to be Y = 0.771 + 1.836 ${\tmes}10^{-4}$X, where the efficiency(Y) was ranged from about 12% to 31% in the liquid scientillation counting. In this paper, a brief theory concerning the biological half-life of tritium and the retention formula to apply to systematically distributed tritium are described.

• Journal of the Korean earth science society
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• v.36 no.7
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• pp.661-673
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• 2015

UBVI CCD photometry of the intermediate age open cluster NGC 7790 has been obtained using AZT-22 1.5 m telescope (f/7.74) at the Maidanak Astronomical Observatory in Uzbekistan. NGC 7790 contains three ${\delta}$ Cep variable stars including CEa Cas, CEb Cas, and CF Cas. PSF photometry was carried out using IRAF/DAOPHOT for all observations. The total number of stars observed both in V and I filter was 1008 and the limiting magnitude was $V{\approx}22$. To determine atmospheric extinction coefficients and photometric zero points, many blue and red standard stars as well as the standard stars in the celestial equator under various airmass were observed. Photometric data were transformed into the standard Johnson-Cousins' UBVI standard system. From the analysis of UBVI color-magnitude diagram and color-color diagram, the color excess in V and I filter [$E(B-V)=0.58{\pm}0.02$], the selective extinction ratio in V and I filter [$R_V{\equiv}A_V/E(B-V)=3.02{\pm}0.09$] and distance modulus ($V_0-M_V=12.65{\pm}0.10$) of the cluster were determined. The age of the cluster was estimated to be log $age=8.05{\pm}0.05$ [yr] based on the position of these three Cepheid variables in the color-magnitude diagram, the isochrone of the Geneva group ($Ekstr{\ddot{o}}m$ et al., 2012-Z=0.019), and the isochrone of the Padova group (Bressan et al., 2012-Z=0.014) were used to compare each other. Of them, the Geneva models that considered stellar rotation well described the position of ${\delta}$ Cepheid variables in the blue loop. Although they were well consistent with standard period-luminosity relation of ${\delta}$ Cepheid variables, three Cepheid variables in NGC 7790 were, on average, brighter by about 0.5 mag than the absolute magnitude estimated from the mean period-luminosity relation at a given period.

• Korean Journal of Remote Sensing
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• v.17 no.3
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• pp.211-218
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• 2001

We have performed the calculation of total radiances for the KOMPSAT-2 Multispectral Camera (MSC) using a radiative transfer model of MODTRAN and examined its results. To simulate four seasonal conditions in the model calculation, we used model atmospheres of mid-latitude winter and summer for calculations of January 15 and July 15, and US standard for April 15 and October 15, respectively. Orbital parameters of KOMPSAT-2 and the seasonal solar zenith angles were taken into account. We assumed that the meteorological range is the tropospheric aerosol extinction of 50 km and surface albedo is the global average of clear-sky albedo of 0.135. MSC contract values are found to be considerably greater in the MSC spectral range than the total radiances calculated with the above general conditions. It is also shown that the spectral behavior of model results with the constant surface albedo differs from the pattern of MSC contract values. From these results, it can be inferred that the forthcoming MSC images would be somewhat dark.