• 한국경제지리학회지
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• 제16권3호
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• pp.492-511
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• 2013

국제회계기준위원회(IASB)에서 규정한 R&D 산업은 다양한 분야에서 '연구'와 '개발'을 동시에 진행하는 3차 산업에 해당한다. R&D 산업과 관련한 기존 정성적 연구들은 공간군집 사례들을 기반으로 분류한 클러스터 유형 중 하나인 하이테크 혁신 클러스터로 취급하여 분석한다(Coe et al., 2007). 그러나 이는 다양한 R&D 산업의 공간군집 사례들을 일반화하는데 그쳤으며, 특히 클러스터 형성 과정에서 시간의 흐름을 고려하지 않은 R&D 클러스터가 시공간적으로 유의미한 것인지 알 수 없다. 이에 본 연구는 기존 공간적인 혹은 시간적인 측면만을 강조하는 클러스터 분석의 한계를 인식하고, 섬유 및 의복 제조업의 비교를 통해 R&D 시공간 클러스터를 탐색해본다. 연구방법으로는 시공간 클러스터의 발견 및 위치탐색을 위해 시공간 K-함수와 시공간 스캔통계를 이용하였다. 그 결과, R&D는 공간적 측면만 고려한 분석에서는 유의미한 클러스터가 발견되었지만, 공간적 분포와 시간적 흐름을 동시에 고려한 시공간 클러스터는 발견되지 않았다. 즉, 시간에 따른 R&D의 신설 과정은 이미 존재하는 R&D의 공간적 위치와 독립적인 것으로 나타났다. 반면 섬유 및 의복 제조업은 공간과 시공간 클러스터 모두 유의미한 클러스터를 발견했다.

• 천문학회보
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• 제42권2호
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• pp.45.2-45.2
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• 2017

Using the latest cosmological hydrodynamic N-body simulations of groups and clusters, we study how location in phase-space coordinates at z = 0 can provide information on environmental effects acting in clusters. We confirm the results of previous authors showing that galaxies tend to follow a typical path in phase-space as they settle into the cluster potential. As such, different regions of phase-space can be associated with different times since first infalling into the cluster. However, in addition, we see a clear trend between total mass loss due to cluster tides and time since infall. Thus, we find location in phase-space provides information on both infall time and tidal mass loss. We find the predictive power of phase-space diagrams remains even when projected quantities are used (i.e.,line of sight velocities, and projected distances from the cluster). We provide figures that can be directly compared with observed samples of cluster galaxies and we also provide the data used to make them as supplementary data to encourage the use of phase-space diagrams as a tool to understand cluster environmental effects. We find that our results depend very weakly on galaxy mass or host mass, so the predictions in our phase-space diagrams can be applied to groups or clusters alike, or to galaxy populations from dwarfs up to giants.

• 천문학회보
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• 제41권1호
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• pp.69.3-70
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• 2016

We study the orbital histories of Virgo galaxies undergoing different HI gas stripping stages using phase-space diagrams. Based on the HI properties of galaxies, we find that location of galaxies is in good agreement with ram-pressure stripping predicted by numerical simulations with different infall time. For example, galaxies experiencing active gas stripping are mostly found in the first infall region showing high velocity with respect to the cluster center. Meanwhile, most galaxies that are likely to have lost gas a while ago are found in the cluster outskirts with low orbital velocities. We also discuss the cases where observational properties of galaxies and their locations in the phase-space do not well agree. In addition, we probe the phase-space of filaments and subgroups around or within Virgo. Our results strongly suggest that substructures can play important roles in galaxy evolution while galaxies are falling to the cluster.

• 천문학회보
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• 제44권1호
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• pp.40.1-40.1
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• 2019

We utilize times since infall of cluster galaxies obtained from Yonsei Zoom-in Cluster Simulation (YZiCS), the cosmological hydrodynamic N-body simulations, and star formation rates from the SDSS data release 10 to study how quickly late-type galaxies are quenched in the cluster environments. In particular, we confirm that the distributions of both simulated and observed galaxies in phase-space diagrams are comparable and that each location of phase-space can provide the information of times since infall and star formation rates of cluster galaxies. Then, by limiting the location of phase-space of simulated and observed galaxies, we associate their star formation rates at z ~ 0.08 with times since infall using an abundance matching technique that employs the 10 quantiles of each probability distribution. Using a flexible quenching model covering different quenching scenarios, we find the star formation history of satellite galaxies that best reproduces the obtained relationship between time since infall and star formation rate at z ~ 0.08. Based on the derived star formation history, we constrain the quenching timescale (2 - 7 Gyr) with a clear stellar mass trend and confirm that the refined model is consistent with the "delayed-then-rapid" quenching scenario: the constant delayed phase as ~ 2.3 Gyr and the quenching efficiencies (i.e., e-folding timescale) outside and inside clusters as ~ 2 - 4 Gyr (${\propto}M_*^{-1}$) and 0.5 - 1.5 Gyr (${\propto}M_*^{-2}$), Finally, we suggest: (i) ram-pressure is the main driver of quenching of satellite galaxies for the local Universe, (ii) the quenching trend on stellar mass at z > 0.5 indicates other quenching mechanisms as the main driver.

• 천문학논총
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• 제19권1호
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• pp.77-81
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• 2004

A high performance computing cluster for astronomical computations has been built at Korea Astronomy Observatory. The 64 node cluster interconnected with Gigabit Ethernet is composed of 128 Intel Xeon processors, 160 GB memory, 6 TB global storage space, and an LTO (Linear Tape-Open) tape library. The cluster was installed and has been managed with the Open Source Cluster Application Resource (OSCAR) framework. Its performance for parallel computations was measured with a three-dimensional hydrodynamic code and showed quite a good scalability as the number of computational cells increases. The cluster has already been utilized for several computational research projects, some of which resulted in a few publications, even though its full operation time is less than one year. As a major resource of the $K^*Grid$ testbed, the cluster has been used for Grid computations, too.

• 한국항공우주학회지
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• 제47권10호
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• pp.728-737
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• 2019

본 연구에서는 초소형 위성을 이용한 위성 편대 및 군집 운용 시 실시간으로 위성 간의 상대 위치 정보를 제공할 수 있는 통합 항법용 모듈형 온보드 컴퓨터(On-board Computer, OBC)를 개발하였다. 모듈은 구조적으로는 큐브위성의 기준 규격에 맞게 설계하되 사용자가 원하는 무선 통신모듈 및 항법용 Global Positioning System(GPS) 장비를 적용할 수 있도록 확장성을 고려하였다. 개발된 OBC는 제품 개발 및 제작 이후 야외 테스트를 통해 저전력 Micro Controller Unit(MCU)로 군집 운용을 수행하는 초소형 위성들의 통합 항법 및 실시간 데이터 동기화 요구 처리속도를 만족함을 확인하였다. 또한, 열진공, 방사능 시험을 거쳐 우주급 환경에서 정상 작동함을 확인하였으며, 진동시험의 경우 underfill 공정을 추가하면 정상적으로 요구조건을 만족할 수 있음을 확인하였다. 이를 통해 향후 수요가 늘어날 군집 운용을 위한 위성군 개발의 핵심 부품인 OBC의 대량생산 체계를 구축하였다.

• 천문학회지
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• 제46권4호
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• pp.173-181
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• 2013

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.

• 천문학회보
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• 제36권2호
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• pp.121-121
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• 2011

Thanks to KMTNet's wide field of view, it is time to implement imaging survey of extensive area of clusters of galaxies in the southern sky with modern instrument. As part of potential long-term survey of nearby (D < 50 Mpc) well-known clusters of galaxies, we propose a wide-field and deep survey of Fornax cluster as a first step of the project. By imaging the 400 square deg region (100 fields) enclosed within the five times virial radius of the Fornax cluster, in three SDSSfilters(g', r', i'), we can provide an unprecedented view of structure of Fornax cluster using sample from giant to dwarf galaxies. We will secure galaxies with brightness comparable to the limiting magnitude (r'=23.1 AB mag) of SDSS. Furthermore, we also request extremely deep (limiting surface brightness of ~ 28 mag $arcsec^{-2}$forr'band) survey for the central region (16 square degree, i.e., four fields) of Fornax cluster. This will allow us to detect the diffuse intracluster light (ICL) that permeates clusters as a valuable tool for studying the hierarchical nature of cluster assembly. In order to complete whole survey, about 285 hr observing time (without overhead) is required. By combining data available at other wavelengths, it will offer unique constraints on the formation of large-scale structure and also provide important clues for theories of galaxy formation and evolution. Our proposed survey will be implemented in the close collaboration with researchers in various countries (Germany, Australia, UK, USA) and ongoing project (e.g., SkyMapper).

• 천문학회보
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• 제43권2호
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• pp.38.2-38.2
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• 2018

To understand the assembly of the galaxy population in clusters today, it is important to first understand preprocessing, the impact of environments prior to cluster infall. We use 15 cluster samples from YZiCS, a hydrodynamic cluster zoom-in simulation to determine the significance of preprocessing, and focus on the tidal mass loss of dark matter halos. We find ~48% of the cluster member halos were once satellites of another host. The preprocessed fraction depends on each cluster's recent mass growth history. Also, we find that the total mass loss is a clear function of the time spent in a host. However, two factors can increase the mass loss rate considerably. First, if the satellite mass is approaching the mass of its host. Second, when the halo suffers tidal mass loss at a higher redshift. Being in hosts before cluster infall enables halos to experience tidal mass loss for an extended period of time.

• 한국콘텐츠학회논문지
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• 제8권2호
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• pp.18-26
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• 2008

본 논문은 사용자로 하여금 표정공간으로부터 일련의 표정들을 선택하게 함으로써 3차원 아바타의 표정을 제어할 수 있는 표정공간의 단계적 가시화 기법을 기술한다. 본 기법에 의한 시스템은 무표정 상태를 포함하여 11개의 서로 다른 모션들로 구성된 2400여개의 표정 프레임으로 2차원 표정공간을 구성하였으며, 3차원 아바타의 표정 제어는 사용자가 표정공간을 항해함으로서 수행되어진다. 그러나 표정공간에서는 과격한 표정 변화에서부터 세밀한 표정 변화까지 다양한 표정 제어를 수행할 수 있어야하기 때문에 단계적 가시화 기법이 필요하다. 표정공간을 단계적으로 가시화하기 위해서는 퍼지 클러스터링을 이용한다. 초기 단계에서는 11개의 클러스터 센터를 가지도록 클러스터링하고, 단계가 증가될 때 마다 클러스터 센터의 수를 두 배씩 증가시켜 표정들을 클러스터링한다. 이때 클러스터 센터와 표정공간에 분포된 표정들의 위치는 서로 다른 경우가 많기 때문에, 클러스터 센터에서 가장 가까운 표정상태를 찾아 클러스터 센터로 간주한다. 본 논문은 본 시스템이 어떤 효과가 있는지를 알기 위해 사용자들로 하여금 본 시스템을 사용하여 3차원 아바타의 단계적 표정 제어를 수행하게 하였으며, 그 결과를 평가한다.