• 디지털융복합연구
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• 제14권2호
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• pp.345-350
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• 2016

현대의 디자인은 자연과 생물 형태를 지닌 것에서 주로 시작되면서 점차 디자인 대상은 한계에 부딪혀 디자인은 형태에서 감성을 담는 것으로 변화하였다. 하지만, 개인적인 감성은 대중의 공감을 얻기는 어렵다. 따라서 연구자는 이미 대중적으로 사랑받고 있는 대상을 선정하여 금속조형으로 시각화 하고자 했다. 연구자가 선정한 시각화 대상은 한국인이 가장 사랑하는 시인인 윤동주의 '별 헤는 밤' 으로 시각화하기 위한 미적요소는 선행 연구된 문헌들을 통해 미적요소를 선정하고 이를 금속과 원석, 착색기법, 세공 등을 응용하여 제작하였다. 그 결과 윤동주 '별헤는 밤'의 시어 속에 내재된 감성을 객관적으로 이해하고 미적요소를 선정할 수 있어 감성적으로 객관성을 잃지 않았으며, 완성된 금속조형물 속에서 윤동주의 '별 헤는 밤'의 깊은 감성과 금속조형물의 아름다움을 함께 느낄 수 있었다. 이를 통해 무형의 대상을 형태화할 수 있는 가능성을 제시하는 계기가 되었다.

• 인문언어
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• 제1권1호
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• pp.185-194
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• 2001

In this paper, I propose that the figurative structure of Tongjoo Yoon′s "One Night, Counting the Stars" reflects the poet′s anguish over the colonial reality of Korea in the later stages of the Japanese occupation, especially regarding the forced adoption of Japanese names in 1939. The poet Yoon himself registered at Yonhi College with an adopted Japanese name. In the second half of the poem, the speaker alludes to this historical fact when he confesses that "On a hill lit by myriads of stars / I spelled my name / And covered it over with dirt," and that he "laments (his) shameful name." In the simile of the last stanza, the speaker continues to allude to the "buried" name: "But past winter, come spring to my star, / As green grass sprouts on a grave mound, / So will it spread with pride / On the hill where my name is buried." The longing and the yearning, expressed so simply and in child-like manner in the first half of the poem, become in the second half an urgent need for something that should have been but cannot be, and yet will be in the future-for a world that should be, now lost but to be regained. The poem contains the poet′s earnest belief that the inherited Korean names that were then so shamefully taken away will one day be recovered. It is almost impossible to find any other work written in Korean (despite the most suppressive measures against the use of the Korean language) that also alludes to the adoption of Japanese names. In this respect, "One Night, Counting the Stars" has a unique value in the history of modem Korean literature.

• 천문학회지
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• 제46권6호
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• pp.203-224
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• 2013

Wide-field $JHK_s$ images obtained with the SIRIUS near-infrared camera of the IRSF 1.4m telescope are used to examine the tidal structures of the spatial stellar configuration around six metal-poor ([Fe/H]< -1.0) globular clusters located within 3 kpc from the Galactic center. The radial surface density profiles are obtained from the surface photometry of the cluster images and the star counting for the photometric data. For the star counting, candidates of cluster member stars are selected with an filtering algorithm in color-magnitude diagrams. We find that the six target clusters show tidal overdensity features in the radial surface density profiles. There is a break inside the tidal radius for each cluster, and the profile in the outer overdensity region is characterized by a power law. Two-dimensional density maps of all the clusters show distorted asymmetric stellar configurations in the outer region. In five out of the six target clusters, the overdensity features are likely to be associated with the effects of the Galaxy dynamical interaction and the cluster space motions. The observed tidal configurations of stars suggest that several metal-poor clusters in the Galactic bulge are possibly surviving remnants of mergers to build the old stellar system of the Galactic bulge.

• 천문학회지
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• 제41권4호
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• pp.99-107
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• 2008

When a new counting experiment is proposed, it is crucial to predict whether the desired source signal will be detected, or how much observation time is required in order to detect the signal at a certain significance level. The concept of the a priori prediction of the detection limit in a newly proposed experiment should be distinguished from the a posteriori claim or decision whether a source signal was detected in an experiment already performed, and the calculation of statistical significance of a measured source signal. We formulate precise definitions of these concepts based on the statistical theory of hypothesis testing, and derive an approximate formula to estimate quickly the a priori detection limit of expected Poissonian source signals. A more accurate algorithm for calculating the detection limits in a counting experiment is also proposed. The formula and the proposed algorithm may be used for the estimation of required integration or observation time in proposals of new experiments. Applications include the calculation of integration time required for the detection of faint emission lines in a newly proposed spectroscopic observation, and the detection of faint sources in a new imaging observation. We apply the results to the calculation of observation time required to claim the detection of the surface thermal emission from neutron stars with two virtual instruments.

• 천문학회지
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• 제21권2호
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• pp.155-171
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• 1988

We have examined how sensitively the extinction value determined by the method of star-count depends on such factors as the plate limit, the size of counting reseau, the non-linearity in the number distribution of stars with magnitude, and the angular resolution demanded by the given problem. We let the Poisson distribution portray the statistical nature of the countings, and chose the region containing the globule Barnard 361 as an example field. Uncertainties due to various combinations of the factors are presented in graphic forms: (1) Dynamic range in the extinction measurements is evaluated as a function of reseau size for varying plate limits. (2) Statistical errors involved in the star-count are analized in terms of the signal-to-noise ratio, the plate limit and the reseau size. (3) Systematic error due to the non-linearity in the number distribution are thoroughly analized. (4) Finally, a methodology is presented for correcting the systematic error in the observed radial density gradient. These graphs are meant to be used in selecting proper size of the reseau and in estimating errors inherent to the star-count analysis.

• 한국위성정보통신학회논문지
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• 제8권3호
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• pp.32-40
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• 2013

Boltwood 구름센서는 구름으로부터 복사되는 적외선을 감지하여 구름의 유무와 많고 적음을 판별할 수 있는 기상센서의 한 종류이다. 이 구름센서는 한국천문연구원이 진행하고 있는 국가현안과제의 일환인 우주물체 전자광학 감시체계 시스템(OWL, Optical Wide-field patroL)에 사용될 계획이다. 실제 시스템 적용에 앞서, Boltwood 구름센서를 충북대학교 천문대에 설치, 약 2주간 구름센서의 구름감지 성능 시험을 위한 관측을 진행하였다. 구름센서의 성능과 비교할 대상으로 충북대학교 천문대에 현재 설치, 운영 중인 구름량 측정을 위한 CCD 관측시스템을 이용하였다. 성능 테스트 결과, 하늘과 지상의 온도차이와 측광 자료의 별 개수간 명확한 상관관계가 도출되지 못했다. 그 원인으로는 시험 환경상의 문제와 Boltwood 구름센서의 내부 알고리즘 및 하드웨어에 대한 정보공개가 제한 때문인 것으로 판단된다. 이 논문에서는 Boltwood 구름센서와 CCD 관측시스템의 구름지수를 비교, 분석한 과정과 그 상세 결과를 제시하고자 한다.