• 약학회지
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• 제38권4호
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• pp.366-371
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• 1994

To improve the identification power of TLC/HPTLC the in situ reflectance spectra obtained directly from plates with commercial scanner are used. The spectrum normalization should be carried out prior to comparing and searching the spectra from library for the identification of compounds. Because the reflectance does not obey the Lambert-Beer's law, there arise some problems in normalization. These problems could be solved to some extent by normalizing the spectra with regression methods. The spectra are manipulated with the regression function of a curve obtained from the correlation plot. When the parabola was used as the manipulating function, the spectra were identified with the accuracy of 97% and this result was better than that of conventionally used the point and area normalization method.

• 전기전자학회논문지
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• 제22권4호
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• pp.999-1005
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• 2018

본 논문에서는 전력계통에서 정밀하고 변화에 수렴성이 빠른 탐색을 기반으로 하는 주파수 추정 기법을 제안하였다. 제안된 주파수 추정 알고리즘은 고분해능 스펙트럼의 기울기를 추정하여 스펙트럼의 peak 점을 탐색하는 구조를 적용하였다. 과도적으로 주파수 변화가 큰 경우에 기존 방법들의 단점인 수렴속도가 늦는 점을 보완 또는 개선하기 위한 방법으로 Context analysis를 통하여 Full-search 기법과 주파수 추정변수들을 적응적으로 적용하여 주파수 추정의 정밀도와 수렴속도를 향상시키고 대표적인 주파수 추정기법인 DFT(discrete Fourier transform) 방법, ECKF(extended complex Kalman filter), MV(minimum variable)방법들과 비교하여 수렴성과 정밀도가 우수함을 보였다.

• 천문학회지
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• 제48권5호
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• pp.313-323
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• 2015

Active galactic nuclei (AGN) are known for irregular variability on all time scales, down to intra-day variability with relative variations of a few percent within minutes to hours. On such short timescales, unexplored territory, such as the possible existence of a shortest characteristic time scale of activity and the shape of the high frequency end of AGN power spectra, still exists. We present the results of AGN single-dish fast photometry performed with the Korean VLBI Network (KVN). Observations were done in a “anti-correlated” mode using two antennas, with always at least one antenna pointing at the target. This results in an effective time resolution of less than three minutes. We used all four KVN frequencies, 22, 43, 86, and 129 GHz, in order to trace spectral variability, if any. We were able to derive high-quality light curves for 3C 111, 3C 454.3, and BL Lacertae at 22 and 43 GHz, and for 3C 279 at 86 GHz, between May 2012 and April 2013. We performed a detailed statistical analysis in order to assess the levels of variability and the corresponding upper limits. We found upper limits on flux variability ranging from ~1.6% to ~7.6%. The upper limits on the derived brightness temperatures exceed the inverse Compton limit by three to six orders of magnitude. From our results, plus comparison with data obtained by the University of Michigan Radio Astronomy Observatory, we conclude that we have not detected source-intrinsic variability which would have to occur at sub-per cent levels.