• ETRI Journal
• /
• 제18권3호
• /
• pp.147-160
• /
• 1996

We investigate noise-induced phase transitions in globally coupled active rotators with multiplicative and additive noises. In the system there are four phases, stationary one-cluster, stationary two-cluster, moving one-cluster, and moving two-cluster phases. It is shown that multiplicative noise induces a bifurcation from one-cluster phase to two-cluster phase. Pinning force also induces a bifurcation from moving phase to stationary phase suppressing the multiplicative noise effect. Additive noise reduces both effects of multiplicative noise and pinning force urging the system to the stationary one-cluster phase. The frustrated effects of pinning force and additive and multiplicative noises lead to a reentrant transition at intermediate additive noise intensity. Nature of the transition is also discussed.

• 천문학회보
• /
• 제41권1호
• /
• pp.34.3-35
• /
• 2016

A galaxy-cluster phase space diagram is a simple plot of clustocentric velocity versus clustocentric radius for each member of the cluster. Using state-of-the-art, cosmological hydrodynamical simulations, we investigate where simulated galaxies fall in phase space. We find the galaxies with different cluster infall times often separate cleanly in phase space. We also investigate how a galaxy's location in phase space is correlated with its tidal mass loss, and ram pressure stripping. By comparing our simulated cluster galaxies to observed cluster galaxies, we show how phase space diagrams are essential tools for understanding environmental effects acting on cluster galaxies.

• Journal of the Korean Statistical Society
• /
• 제27권3호
• /
• pp.265-278
• /
• 1998

In this paper, we suggest two-phase adaptive cluster sampling schemes. The main feature of the two-phase sampling is that the information collected in the first phase sample is utilized in the selection of the second phase sample. The conventional two-phase sampling is, however, not sufficient to increase efficiency when the population of interest is rare and clustered. In the proposed sampling scheme, the first phase sample is selected with adaptive cluster sampling procedure and the second phase sample is selected by PPSWR and $\pi$PS sampling. We investigate unbiased estimators of population total and their variance for the proposed sampling schemes respectively. Finally we compare these suggested sampling schemes using numerical examples .

• 천문학회보
• /
• 제42권2호
• /
• pp.45.2-45.2
• /
• 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.

• 한국콘텐츠학회논문지
• /
• 제9권1호
• /
• pp.167-176
• /
• 2009

기존의 클러스터 라우팅 방식은 클러스터 헤드를 선출하여 클러스터 내의 멤버 노드들로부터 정보를 수집하고 압축하여 기지국에 전송함으로써 에너지 효율을 높일 수 있는 대표적인 방식이다. 그러나 클러스터 형성 단계 중 매 라운드마다 셋업 단계에서 선출된 클러스터 헤드와 클러스터 내의 멤버 노드들 간의 빈번한 정보 교환으로 인해 발생하는 불필요한 에너지 소모는 클러스터 라우팅 방식이 해결해야 하는 과제이다. 본 논문에서는 셋업 단계에서의 선출된 클러스터 헤드와 기존의 클러스터 헤드 사이에 변경되지 않는 중첩된 영역에 속한 멤버 노드들을 계산함으로써, 중첩된 멤버 노드들의 셋업 단계에서의 불필요한 송수신 횟수를 줄여 정보 교환을 최소화하였다. 따라서 셋업 단계에서의 소모되는 에너지를 절약하여 안정 단계에서 효율적으로 사용함으로써, 에너지의 효율적인 사용과 전체적인 네트워크의 생존시간을 증가시키고자 하며, 전체 네트워크내의 멤버들에게 클러스터 헤드가 될 수 있는 균등한 기회를 주고자 하는클러스터 헤드 선출 프로토콜을 제안한다.

• 천문학회보
• /
• 제44권1호
• /
• pp.40.1-40.1
• /
• 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.

• 한국콘텐츠학회논문지
• /
• 제10권2호
• /
• pp.14-24
• /
• 2010

무선 센서 네트워크에서는 센서 노드의 제한된 자원으로 동작하기 때문에 클러스터 기반의 라우팅 방법을 통해 네트워크의 수명을 향상시키고 있다. 본 논문에서는 클러스터 기반의 라우팅 기법이 가진 에너지 효율을 최대화하기 위해 방향, 거리, 밀도, 그리고 잔여 에너지량을 사용하고자 한다. 상위 클러스터 헤드의 방향 정보를 이용하여 새로운 클러스터 헤드를 자율적으로 선출할 때 고립 노드의 발생 빈도를 최소화하고, 거리 정보를 이용하여 셋업 단계에서 새로운 클러스터와 이전의 클러스터 모두에 포함되어 정보를 갱신할 필요가 없는 센서 노드들을 슬립 모드로 전환하여 에너지 소모를 줄이며, 단지 새로 가입되는 센서노드만 정보 교환함으로써 불필요한 에너지 소비를 줄이고자 한다. 뿐만 아니라, 클러스터 기반의 라우팅 기법에서 내부나 외부의 공격에 강한 키 관리 기법을 통해 안전하고 에너지 효율적인 통신이 가능하도록하여 전체적인 네트워크 효율을 높이고자 한다. 따라서 전체 네트워크내의 멤버들에게 클러스터 헤드가 될 수 있는 안전하고 균등한 기회를 주고자 하는 클러스터 헤드 선출 기법을 제안한다.

• 천문학회보
• /
• 제41권1호
• /
• pp.69.3-70
• /
• 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.

• Journal of Electrical Engineering and Technology
• /
• 제13권2호
• /
• pp.998-1007
• /
• 2018

The advent of Wireless Sensor Networks (WSN) has led to their use in numerous applications. Sensors are autonomous in nature and are constrained by limited resources. Designing an autonomous topology with criteria for economic and energy conservation is considered a major goal in WSN. The proposed honey-hive clustering consumes minimum energy and resources with minimal transmission delay compared to the existing approaches. The honey-hive approach consists of two phases. The first phase is an Intra-Cluster Min-Max Discrepancy (ICMMD) analysis, which is based on the local honey-hive data gathering technique and the second phase is Inter-Cluster Frequency Matching (ICFM), which is based on the global optimal data aggregation. The proposed data aggregation mechanism increases the optimal connectivity range of the sensor node to a considerable degree for inter-cluster and intra-cluster coverage with an improved optimal energy conservation.

• 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.