• 한국경제지리학회지
• /
• 제20권2호
• /
• pp.189-213
• /
• 2017

본 연구는 클러스터 진화의 분석에 있어서 클러스터 적응주기 모델의 의의와 한계점을 비판적으로 검토하고, 이를 토대로 향후 클러스터 진화 분석을 위한 연구 과제를 제시하고자 하였다. 1980년대 이전까지 클러스터를 비롯한 산업집적지 연구는 특정 시점에서 경제 공간의 양상에 주목하는 '정태적 관점'을 기초로 이루어졌지만, 최근에는 '복잡적 응계'의 '진화'에 주목하는 '동태적 연구'로 패러다임이 전환되었다. 이에 역동적 지속적으로 진화하는 클러스터에 적절한 분석도구로 적응주기 모델이 주목받게 되었으나, 클러스터 및 그 진화의 속성에 맞게 수정 및 보완되어 클러스터 적응주기 모델이 등장하게 되었다. 클러스터 적응주기 모델은 자원축적, 상호의존성 그리고 회복력의 측면에서 클러스터 진화의 특성을 규명하고, 클러스터 진화 경로를 6가지로 구분하여 살펴 볼 수 있는 포괄적인 분석틀이지만, 모델의 확대 및 심화를 위해서 이론적 경험적 연구 측면에서 더욱 활발한 논의와 보완이 요구된다. 따라서 향후 클러스터 진화 분석에 있어서의 연구 과제로는 클러스터 진화 모델의 구체화 및 정교화, 회복력 개념의 강조 그리고 경험적 연구를 통한 모델의 적용가능성과 유용성의 검증을 제시하고자 한다.

• 천문학회보
• /
• 제41권2호
• /
• pp.60.3-61
• /
• 2016

Galaxy morphology involves complex effects from both secular and non-secular evolution of galaxies. Although it is a final product of galaxy evolution, it gives a clue to the processes that the a galaxy has gone through. Galaxy clusters are the sites where the most massive galaxies are found, and thus the most dramatic merger histories are embedded. Our deep imaging program (${\mu}{\sim}28\;mag\;arcsec^{-2}$), KASI-Yonsei Deep Imaging Survey for Clusters (KYDISC), targets 14 Abell clusters at z = 0.016 - 0.14 using IMACS/Magellan telescope and MegaCam/CFHT to investigate cluster galaxies especially on low surface brightness features related to galaxy interactions. We visually classify galaxy morphology based on criteria related to secular or merger related evolution and find that the morphological mixture of galaxies varies considerably from cluster to cluster. Moreover it depends on the characteristics (e.g. cluster mass) of cluster itself which implies that environmental effects in cluster scale is also an important factor to the evolution of galaxies together with intrinsic (secular) and galaxy merger. Our deep imaging survey for morphological inspection of cluster galaxies with low surface brightness is expected to be a useful basis to understand the nature of cluster galaxies and their internal/external evolutionary path.

• 천문학회보
• /
• 제41권1호
• /
• pp.35.1-35.1
• /
• 2016

Nearby galaxy clusters and their surrounding regions represent the current endpoint of evolution galaxy cluster evolution. We present a new catalog of 1589 galaxies, what we call Extended Virgo Cluster Catalog (EVCC), in wider area of the Virgo cluster based on the Sloan Digital Sky Survey (SDSS) Data Release 7. The EVCC covers an area 5.2 times larger than the footprint of the classical Virgo Cluster Catalog, and reaches out to 3.5 times the virial radius of the Virgo cluster. The EVCC contains fundamental information such as membership, morphology, and photometric parameters of galaxies. The EVCC defines a comprehensive galaxy sample covering a wider range in galaxy density that is significantly different from the inner region of the Virgo cluster. It will be the foundation for forthcoming galaxy evolution studies in the extended Virgo cluster region, complementing ongoing and planned Virgo cluster surveys at various wavelengths. We also present the large scale structures in the field around the Virgo cluster. We identified seven galaxy filaments and one possible sheet in three dimensions of super-galactic coordinates based on the HyperLEDA database. By examining spatial distribution and Hubble diagram of galaxies, we found that six filaments are directly associated with the main body of the Virgo cluster. On the other hand, one filament and one sheet are structures located at background of the main body of Virgo cluster. The EVCC and the filament structures will be the foundation for forthcoming studies of galaxy evolution in various environments as well as buildup of the galaxy cluster at z ~ 0, complementing ongoing and planned Virgo cluster surveys at various wavelengths.

• 천문학회보
• /
• 제42권2호
• /
• pp.46.1-46.1
• /
• 2017

Late-type galaxies falling into a cluster would evolve being influenced by the interactions with both the cluster and the nearby cluster member galaxies. Most numerical studies, however, tend to focus on the effects of the former with little work done on those of the later. We thus perform numerical study on the evolution of a late-type galaxy falling radially toward the cluster center interacting with neighbouring early-type galaxies, using N-body, hydrodynamical simulations. Based on the information about the typical galaxy encounters obtained by using the galaxy catalog of Coma cluster, we run the simulations for the cases where a Milky Way Galaxy-like late-type galaxy, flying either edge-on or face-on, experiences six consecutive collisions with twice more massive early-type galaxies having hot gas in their halos. Our simulations show that the evolution of the late-type galaxy can be significantly affected by the high-speed multiple collisions with the early-type galaxies, such as on the cold gas content and the star formation activity, particularly through the hydrodynamic interactions between the cold disk and the hot gas halos. By comparing our simulation results with those of others, we claim that the role of the galaxy-galaxy interactions on the evolution of late-type galaxies in clusters could be comparable with that of the galaxy-cluster interactions, depending on the dynamical history.

• 천문학회보
• /
• 제43권2호
• /
• pp.33.2-33.2
• /
• 2018

Fossil galaxy cluster has a dominant central elliptical galaxy (${\Delta}M12$ >2 in 0.5Rvir) embedded in highly relaxed X-ray halo, which indicates dynamically stable and passively evolved system. These features are expected as a final stage of the cluster evolution in the hierarchical structure formation paradigm. It is known that Abell 2261(A2261 hereafter) is classified as a fossil cluster, but has unusual features such as a high central X-ray entropy (i.e., non-cool core system), which is not expected in normal fossil clusters. We perform a kinematic study with a spectroscopic data of 589 galaxies in the A2261 field. We define cluster member galaxies using the caustic method and discover a new second bright galaxy at ~1.5 Rvir (nearly the splash-back region). It implies the current fossil state of the cluster can break in the near future. In addition, with three independent substructure finding methods, we find that A2261 has many substructures within 3 Mpc from the center of the cluster. These findings support that A2261 is not in a dynamically stable state. We argue that A2261 is in a transitional phase of dynamical evolution of the galaxy cluster and maybe previously defined fossil cluster does not mean the final stage of the evolution of galaxy clusters.

• 산업클러스터
• /
• 제2권1호
• /
• pp.1-13
• /
• 2008

지역경제의 성공에 있어 산업클러스터의 중요성에 대한 증대된 인식에도 불구하고, 구산업지구에 대한 클러스터 정책의 효과성에 대해서는 그다지 많은 관심이 모이지 못했다. 이들 지역 중 상당수에서는 아직 산업클러스터가 작동하고 있거나 재도약을 위한 새로운 전략이 모색되고 있다. 본 연구는 구산업지구에서 대한 산업클러스터 정책의 효과성을 산업클러스터의 진화적 성격에 대한 이해로부터 찾으려 한다. 이를 위하여 유럽 구산업지구의 변환에 대한 선행연구들을 고찰하고, 어떻게 클러스터 정책이 주요한 정책수단으로 등장하게 되었는지 살펴본다. 본 연구는 또한 영국의 북동지 역에서 어떻게 철강산업의 공급체인이 형성되었는지 사례 연구를 통해 살펴본다. 마지막으로 본 연구의 결론은 클러스터 형성 과정에서의 정책적 개입의 타이밍을 어떻게 잡을 것인지를 보여주는 자료에 초점을 맞추고 있다.

• 천문학회보
• /
• 제35권1호
• /
• pp.56.2-56.2
• /
• 2010

M87, a cD galaxy in the Virgo cluster, has 3-10 times larger enclosed mass than the Milky Way at any given galactocentric radius. Thus the globular cluster (GC) system in M87 is expected to have undergone a more significant dynamical evolution than that of the Milky Way if it had started from the same initial mass function (MF) and radial distribution (RD) as the Milky Way. The evolution of MF and RD of the M87 GC system has been calculated using an advanced, realistic Fokker-Planck (FP) model that considers dynamical friction, disk/bulge shocks, and eccentric cluster orbits. We perform hundreds of FP calculations with different initial cluster conditions, and then search a wide parameter space for the best-fit initial GC MF and RD that evolves into the observed present-day GC MF and RD. We also find best-fit initial MFs and RDs for blue and red GC groups, separately.

• 천문학회보
• /
• 제41권2호
• /
• pp.64.1-64.1
• /
• 2016

We study the evolution of a late-type galaxy (LTG) in a rich cluster environment by using N-body/SPH simulations. To do that we perform a set of simulations of a LTG falling in a Coma-like cluster and also the LTG colliding with early-type galaxies (ETGs) multiple times in the cluster environment. We use a catalog of the Coma cluster in order to estimate the typical number of collisions and the closest approach distances that a LTG would experience in the cluster. We investigate the cold gas depletion and star formation quenching of our LTG model influenced by the hot cluster gas as well as the hot halo gas of the colliding ETGs.

• 천문학회지
• /
• 제46권4호
• /
• pp.173-181
• /
• 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
• /
• 제39권1호
• /
• pp.46.2-46.2
• /
• 2014

Galaxy morphology is involved complex effects of both secular and non-secular evolution of galaxies. Although it is a final product of a galaxy evolution, it may give a clue for the process that the galaxy suffer. Galaxy clusters are the sites where the most massive galaxies are found, and the most dramatic merger histories are embedded. Morphology study in nearby universe, e.g. Virgo cluster, is well established, but for clusters at z ~ 0.1 it is only focused on bright galaxies due to observational limits. Our optical deep imaging of 14 Abell clusters at z = 0.014 - 0.16 using IMACS f/2 on a Magellan Badde 6.5-m telescope and MegaCam on a 3.8-m CFHT enable to classify detailed morphology. For the galaxies in our data, we investigated their morphology with several criteria related to secular or merger related evolution. Our research on detailed morphology of thousands of galaxies through deep imaging would give a general census of cluster galaxies and help to estimate the evolution of cluster galaxies.