• 한국비블리아학회지
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• 제31권1호
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• pp.237-255
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• 2020

사회 현상 곳곳에서 나타나고 있는 파레토 법칙(Pareto principle)은 상위 20%가 전체 성과의 80%를 차지한다는 법칙이다. 본 연구에서는 대학도서관 학술정보 공유 협력체에서도 파레토 법칙이 발견되고 있는지 확인하였으며, 더불어 지니계수(Gini coefficient)를 통해 대학 간에 나타나는 학술정보 공유 기여 정도에 대한 격차를 수치로 산출하였다. 그 결과 학술정보 공유 협력 사업에서 상위 20%의 대학도서관이 81.2% 이상의 실적을 주도하고 있었으며, 정보 기여에 대한 격차는 평균 0.78로 매우 심각한 상태를 나타냈다. 대학도서관의 규모를 감안하여 재계산한 지니계수도 일부 사업에서만 균등한 쪽으로 조금 조정되는 양상을 나타냈다. 대학의 형태에 따라서는 전문대학도서관 간의 격차가 4년제 대학도서관보다 극심하였으며, 국립대학도서관보다는 사립대학도서관간의 격차가 더욱 심각한 것으로 나타났다. 마지막으로 도서관의 규모와 학술정보 기여 정도에 따라 참여도서관의 분포를 시각화한 결과, 압도적인 기여 수준을 보이는 대규모 도서관이 존재하였으며, 도서관의 규모는 작지만 상대적으로 높은 기여 수준을 보이는 도서관도 분포하였다.

• Communications for Statistical Applications and Methods
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• 제3권3호
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• pp.291-297
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• 1996

In this paper, we propose the jackknife estimator and the bootstrap estimator of Gini index of the two-parameter exponential distribution when the location parameter $\theta$ is unknown and the scale parameter $\sigma$is known. Sinilarly, we propose the bias location parameter $\theta$ and the scale parameter $\sigma$ are unknown. The bootstrap estimator is more efficient than the other estimators when the location parameter $\theta$is unknown and the scale parameter $\sigma$ is known, and the bias corrected estimator is more efficient than the MLE when both the location parameter $\theta$ and the scale parameter $\sigma$are unknown.

• 한국한의학연구원논문집
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• 제17권2호
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• pp.121-127
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• 2011

Objectives : In the clinical field, it is important to understand the factors that have effects on a certain disease or symptom. For this, many researchers apply Data Mining method to the clinical data that they have collected. One of the efficient methods for Data Mining is decision tree induction. Many researchers have studied to find the best split criteria of decision tree; however, various split criteria coexist. Methods : In this paper, we applied several split criteria(Information Gain, Gini Index, Chi-Square) to Sasang constitutional clinical information and compared each decision tree in order to find optimal split criteria. Results & Conclusion : We found BMI and body measurement factors are important factors to Sasang constitution by analyzing produced decision trees with different split measures. And the decision tree using information gain had the highest accuracy. However, the decision tree that produced highest accuracy is changed depending on given data. So, researcher have to try to find proper split criteria for given data by understanding attribute of the given data.

• 천문학회보
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• 제38권1호
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• pp.39-39
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• 2013

We present a study of correlations between the elemental abundances and galaxy morphologies of 91 blue compact galaxies (BCGs) at z=0.20-0.35 with Sloan Digital Sky Survey (SDSS) DR7 data. We classify the morphologies of the galaxies as either 'disturbed' or 'undisturbed', by visual inspection of the SDSS images, and using the Gini coefficient and M20. We derive oxygen and nitrogen abundances using the Te method. We find that a substantial fraction of BCGs with disturbed morphologies, indicative of merger remnants, show relatively high N/O and low O/H abundance ratios. The majority of the disturbed BCGs exhibit higher N/O values at a given O/H value compared to the morphologically undisturbed galaxies, implying more efficient nitrogen enrichment in disturbed BCGs. We detect Wolf-Rayet (WR) features in only a handful of the disturbed BCGs, which appears to contradict the idea that WR stars are responsible for high nitrogen abundance. Combining these results with Galaxy Evolution Explorer (GALEX) GR6 ultraviolet (UV) data, we find that the majority of the disturbed BCGs show systematically lower values of the $H{\alpha}$ to near-UV star formation rate ratio. The equivalent width of the $H{\beta}$ emission line is also systematically lower in the disturbed BCGs. Based on these results, we infer that disturbed BCGs have undergone star formation over relatively longer time scales, resulting in a more continuous enrichment of nitrogen. We suggest that this correlation between morphology and chemical abundances in BCGs is due to a difference in their recent star formation histories.