We trace the dynamical evolution of dark matter (DM) content in NGC 6397, one of the native Galactic globular clusters (GCs). The relatively strong tidal field (Galactocentric radius of ~ 6 kpc) and short relaxation timescale (~ 0.3 Gyr) of the cluster can cause a significant amount of DM particles to evaporate from the cluster in the Hubble time. Thus, the cluster can initially contain a non-negligible amount of DM. Using the most advanced Fokker-Planck (FP) method, we calculate the dynamical evolution of GCs for numerous initial conditions to determine the maximum initial DM content in NGC 6397 that matches the present-day brightness and velocity dispersion profiles of the cluster. We find that the maximum allowed initial DM mass is slightly less than the initial stellar mass in the cluster. Our findings imply that NGC 6397 did not initially contain a significant amount of DM, and is similar to that of NGC 2419, the remotest and the most massive Galactic GC.

본 논문에서는 유전알고리즘을 사용하여 철근콘크리트 구조물의 최적 지진설계를 효율적으로 수행하기 위해 클러스터를 사용하는 경우 확장성을 확인하였다. 클러스터를 구성하는 코어프로세서의 개수를 증가시키면서 유전알고리즘의 각 세대에 소요되는 시간의 감소를 관찰하였다. 단일 퍼스널 컴퓨터의 구성을 분류한 후, wall-clock time과 암달의 법칙으로 예상된 값을 비교하여 예상되었던 병목현상을 확인하였다. 이에 클러스터의 확장성에서 복합적인 요인에 의한 경향을 확인할 수 있었다. 병목현상의 물리적인 요인과 알고리즘 측면에서의 요인을 구분하기 위해 유전알고리즘의 개채수를 나누어 실험을 수행하여 결과를 확인하였다.

본 연구는 방송프로그램 제작산업을 활성화시키기 위한 방안으로 디지털방송콘텐츠 생산 활성화를 위해 필수적인 제작단지를 클 러스터로 구축하기 위한 필요성을 제기하고, 이를 위해 선행되어야 할 조건으로 기존의 제작 시설에 대한 문제점과 개선 방안을 살펴보았으 며, 활용하는 방안을 모색하는데 초점을 두었다. 이를 위해 전문가들의 인식을 중심으로, 기존의 야외세트장과는 달리 방송 제작사들과 관련기 관은 물론 제작시설과 기술 그리고 정보를 일정 지역내에 집중시켜야 함을 강조하고, 이를 위한 선행조건으로 디지털 방송 제작에 필요한 제 작 시설과 제작 지원 시설을 파악했으며, 클러스터 전략을 통해 활용하 는 방안을 도출하고자 했다는 점이다. 이는 디지털 방송콘텐츠를 한곳 에 집적하여 제작과 유통을 가능하게 함으로써, 디지털 방송콘텐츠의 제작 인프라를 구축하고, 미래전략 수립에 실증적인 자료로 활용할 수 있을 것이다.

Star clusters are superb astrophysical laboratories containing cospatial and coeval samples of stars with similar chemical composition. We initiate the Sejong Open cluster Survey (SOS) - a project dedicated to providing homogeneous photometry of a large number of open clusters in the SAAO Johnson-Cousins’ UBV I system. To achieve our main goal, we pay much attention to the observation of standard stars in order to reproduce the SAAO standard system. Many of our targets are relatively small sparse clusters that escaped previous observations. As clusters are considered building blocks of the Galactic disk, their physical properties such as the initial mass function, the pattern of mass segregation, etc. give valuable information on the formation and evolution of the Galactic disk. The spatial distribution of young open clusters will be used to revise the local spiral arm structure of the Galaxy. In addition, the homogeneous data can also be used to test stellar evolutionary theory, especially concerning rare massive stars. In this paper we present the target selection criteria, the observational strategy for accurate photometry, and the adopted calibrations for data analysis such as color-color relations, zero-age main sequence relations, Sp - MV relations, Sp - Teff relations, Sp - color relations, and Teff - BC relations. Finally we provide some data analysis such as the determination of the reddening law, the membership selection criteria, and distance determination.

A cell formation approach based on cluster analysis is developed for the configuration of manufacturing cells. Cell formation, which is to group machines and parts into machine cells and the associated part families, is implemented to add the flexibility and efficiency to manufacturing systems. In order to develop an efficient clustering procedure, this paper proposes a cluster analysis-based approach developed by incorporating and modifying two cluster analysis methods, a hierarchical clustering and a non-hierarchical clustering method. The objective of the proposed approach is to minimize intercellular movements and maximize the machine utilization within clusters. The proposed approach is tested on the cell formation problems and is compared with other well-known methodologies available in the literature. The result shows that the proposed approach is efficient enough to yield a good quality solution no matter what the difficulty of data sets is, ill or well-structured.

As a part of the short-period variability survey (SPVS) at Bohyunsan Optical Astronomy Observatory, we obtained time-series BV CCD images in the region of Cyg OB3 association centered on the open cluster NGC 6871. The observations were performed for 18 nights from September 5, 2008 to September 1, 2009. We found 15 short-period variable stars in the region. They are δ Scuti type stars belonging to the local spiral arm, Orion spur. Among them, only two stars were previously known, and the rest are newly discovered ones. In this paper, we have performed a multiple-frequency analysis to determine frequencies of the 15 δ Scuti type stars, using the discrete Fourier transform and linear least-square fitting methods. One of the newly discovered variable stars is a double-mode δ Scuti type star with the fundamental and the first overtone modes, and two are high amplitude δ Scuti stars.

F-Measure is one of the external measures for evaluating the validity of clustering results. Though it has clear advantages over other widely used external measures such as Purity and Entropy, F-Measure has inherently been less sensitive than other validity measures. This insensitivity owes to the definition of F-Measure that counts only most influential portions. In this research, we present Fn-Measure, an external cluster evaluation measure based on F-Measure. Fn-Measure is so sensitive that it can detect their difference in the cases that F-Measure cannot detect the difference in clustering results. We compare Fn-Measure to F-Measure for a few clustering results and show which measure draws better result based upon homogeneity and completeness

We investigate the role of galaxy environment in the evolution of individual galaxies through the AKARI observations of the merging galaxy cluster A2255. MIR diagnostics using N3-S11 colors are adopted to select star-forming galaxies and galaxies in transition between star-forming galaxies and quiescent galaxies. We do not find particular enhancement of star formation rates as a function of galaxy environment, reflected in cluster-centric distance and local surface density of galaxies. Instead, the locations of intermediate MIR-excess galaxies (-1.2 < N3 - S11 < 0.2) show that star-forming galaxies are transformed into passive galaxies in the substructures of A2255, where the local surface density of galaxies is relatively high.