• 한국통신학회논문지
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• 제41권12호
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• pp.1801-1810
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• 2016

본 논문에서는 최근 많은 관심과 집중을 받고 있는 SDN 분야 오픈 소스 프레임워크인 오픈데이라이트 컨트롤러를 중심으로 컨트롤러 클러스터 구조 및 동작방식에 대하여 분석한다. 오픈데이라이트 컨트롤러 클러스터에서는 컨트롤러 간 데이터 스토어의 동기화를 위하여 분산 샤드 구조 및 샤드 리더 선정을 위한 Raft 알고리즘을 적용하고 있다. 성능 분석에서는 컨트롤러 클러스터 크기, 샤드 역할, 샤드 정책에 따른 CRUD, Routed RPC 지연시간 및 리더 재선정 지연시간 등을 분석함으로써, 오픈데이라이트 컨트롤러 클러스터 운영 시의 최적 운영 방안을 논의한다.

• 천문학회지
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• 제31권1호
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• pp.39-50
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• 1998

We present UBV CCD photometry of Be 2, previously unstudied open cluster. Our photometry covers a field of $3'.2\times3'.8$ of the sky centered on the cluster, which is slightly smaller than the cluster diameter estimated to be about 260'. We have determined the reddening, distance, age and metallicity of the cluster by fitting the Pad ova isochrones to the observed stellar distributions in color-magnitude diagram as well as main sequence fitting: $E(B-V)=0.8\pm0.05,\;(m-M)_o=13.6\pm0.1,\;log(t) =8.9\pm0.1$, and Z=0.008. The present photometry shows that Be 2 is a distant open cluster of intermediate age. that it is a distant intermediate-age open duster.

• 천문학논총
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• 제14권2호
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• pp.61-67
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• 1999

We present a new UBVI CCD photometry of the intermediate-age open cluster NGC 2420. Our photometry covers a field of $7'9\times7.'7$ of the sky centered on the cluster. We determined the reddening and distance to the cluster by the main sequence fitting as $E(B - V) = 0.05\pm0.02$ and $(m-M)_o = 11.9\pm0.1$, along with the age of $\~2$ Gyr by fitting the Padova isochrones to the observed color-magnitude diagrams of the cluster. The fraction of binaries is found to be $44\pm5\%$ and they are likely to locate in the central region of the cluster. The spatial distributions of the binaries and the variation of the cluster luminosity functions along the radius suggest mass segregations due to the dynamical evolution of the cluster.

• 천문학회지
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• 제35권2호
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• pp.87-95
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• 2002

We have conducted VI CCD photometry of the open cluster NGC 6819 in order to understand the effects of dynamical evolution in old open clusters. Our photometry covers 18' $\times$ 18' on the sky, centered on the cluster, which seems to cover the whole cluster field. Our photometry reaches down to V $\approx$ 20.5, which allows us to analyze the luminosity function and spatial distribution of stars brighter than Mv $\approx$ 8.5. There is a clear evidence for mass segregation in NGC 6819, i.e., the giants and upper main-sequence stars are concentrated in the inner regions, whereas the lower main-sequence stars distribute almost uniformly throughout the cluster. The luminosity function of the main-sequence stars of NGC 6819 is almost flat. The flat luminosity function indicates that a large number of low mass stars has escaped from the cluster unless its initial mass function is much different from the Salpeter type (${\phi}(m){\propto} m^{-(1+x)},x = 1.35$).

• 천문학회지
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• 제29권2호
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• pp.181-194
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• 1996

We present a study of the metallicity of the old open cluster NGC 1245 , based on the Washington CCD photometry obtained using the 0.6 m telescope at the Sobaeksan Observatory, Korea. NGC 1245 has been known to be a unique cluster among the known open clusters in the sense that the previous metallicity estimates for this cluster are much larger $(by\;\sigma)$ than the value expected from the radial metallicity gradient of the old open clusters in Our galaxy. We have estimated the metallicity of the cluster red giants using the four color-color diagrams, obtaining a value for the mean metallicity of $[Fe/H] = -0.04\pm0.05$ dex. The total error including the error of the metallicity calibration, 0.15 dex, is 0.16 dex. The metallicity estimate of NGC 1245 we have obtained in this study is smaller than previous estimates, and is consistent with the radial metallicity gradient of the old open clusters, showing that the mean metallicity of NGC 1245 is not abnormally high. The reddening, distance, and age of the cluster have also been derived using the isochrones based on the convective overshooting models: the reddening $E(B-V) = 0.28\pm0.03$; the distance $d = 2.5\pm0.2 kpc$ (the corresponding galactocentric distance is RGC = 10.7 kpc, and the distance from the galactic plane is z = -0.4 kpc); and the age $t = 1.1\pm0.1 Gyrs$.

• 천문학회지
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• 제25권2호
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• pp.91-104
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• 1992

New photoelectric UBV Photometry of 112 stars in open cluster M35 field was obtained. The distance modulus and age of the cluster are $9.^m3$(725pc) and $8.5{\times}10^7yrs$, respectively. The internal differential reddening within the cluster is apparent.

• 천문학회보
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• 제41권2호
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• pp.59.1-59.1
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• 2016

Blue Straggler Stars(BSS) affect their host star cluster in various parameters like color, dynamics, etc. For this reason, it is important to know how to relate BSS frequency and evolution of their host stellar system. To statistical study about global properties of open clusters as the environments of BSS formation, we use three catalogues - (1) two galactic open clusters catalogues including BSS candidate, (2) Milky Way Star Cluster (MWSC) survey data. Then, we compare with the data of two BSS catalogues for test of the result of Marchi et al. 2006. We also investigate the radial mass distribution in open cluster, because it is possible that changing the gradient of radial mass distribution cause increasing the BSS frequency. When we group the open cluster into having BSS or not and other criteria, the groups show slight discrepancies, but we show some important results.

• 한국측량학회지
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• 제37권6호
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• pp.445-452
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• 2019

본 연구에서는 대용량 위성영상의 무감독분류를 위해 k-means clustering 알고리즘의 병렬처리 코드를 개발하여 PC-cluster에서 구현하였다. 이를 위해 OpenMP (Open Multi-Processing)를 기반으로 CPU (Central Processing Unit)의 다중코어를 이용하는 intra-node 코드와 message passing interface를 기반으로 PC-cluster를 이용하는 inter-nodes 코드, 그리고 이 둘을 병용하는 hybrid 코드를 구현하였다. 본 연구에 사용한 PC-cluster는 한 대의 마스터 노드와 여덟 대의 슬래이브 노드로 구성되어 있고 각 노드에는 여덟 개의 다중코어가 장착되어 있다. PC-cluster에는 Microsoft Windows와 Canonical Ubuntu의 두 가지 운영체제를 설치하여 병렬처리 성능을 비교하였다. 실험에 사용한 자료는 두 가지 다중분광 위성영상으로서 중용량인 LANDSAT 8 OLI (Operational Land Imager) 영상과 대용량인 Sentinel 2A 영상이다. 병렬처리의 성능을 평가하기 위하여 speedup과 efficiency를 측정한 결과 전반적으로 speedup은 N/2 이상, efficiency는 0.5 이상으로 나타났다. Microsoft Windows와 Canonical Ubuntu를 비교한 결과 Ubuntu가 2-3배의 빠른 결과를 나타내었다. 순차처리와 병렬처리 결과가 일치하는지 확인하기 위해 각 클래스의 밴드별 중심값과 분류된 화소의 수를 비교하고 결과 영상간 화소대 화소 비교도 수행하였다. Intra-node 코드를 구현할 때에는 OpenMP에 의한 false sharing이 발생하지 않도록 주의해야 하고, PC-cluster에서 대용량 위성영상을 처리하기 위해서는 파일 I/O에 의한 성능저하를 줄일 수 있도록 코드 및 하드웨어를 설계해야 함을 알 수 있었다. 또한 PC-cluster에 설치된 운영체제에 따라서도 성능 차이가 발생함을 알 수 있었다.

• 천문학회지
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• 제29권2호
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• pp.269-278
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• 1996

We present the color-magnitude diagrams (CMD) of more than 24,000 stars in the field of an intermediate age open cluster M11, based on wide field CCD imaging. The morphology of the CMDs varies strikingly as the distance from the center of the cluster increases. From the surface number density analysis, we confirm the mass segregation effect in this cluster: the bright, massive stars are centrally more concetrated than the faint, low mass stars. The slope of the field-corrected surface density with respect to magnitude progressively increases as the radius increases, up to r = 5'. Most of the field stars in or near the cluster main sequence band and in the bright part of the red stars in the CMDs appear to be nearly at the same distance as M11, and they are considered to be the major component of disk stars in the Sagittarius-Carina arm.

• 천문학회지
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• 제29권2호
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• pp.137-156
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• 1996

NGC 6716 is an intermediate-age open cluster in Sagittarius. In this paper, we present the new UBV CCD photometry of the stars in the cluster, which is deeper than previous ones. From the color-color diagram and the color-magnitude diagram, we derived a reddening $E_{B- V} = 0.17\pm0.03$ and a distance modulus of the cluster, $(V - Mv)_o = 9.2\pm0.1$. An age of the cluster is estimated as $8\pm10^7 yrs$ from the latest isochrone. Luminosity function and mass function of the cluster are derived. The gradient of the mass function of bright stars is a bit steep, $\Gamma = -1.85\pm0.05$, and there is no distinct bump and dip in the mass function.