• 천문학회보
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• 제35권2호
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• pp.40.1-40.1
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• 2010

We present the ultraviolet (UV) properties of early type galaxies (ETGs) in clusters. We obtained a cluster catalogue from Yoon et al.(2008) based on Sloan Digital Sky Survey(SDSS) DR5 in the redshift range of 0.05 < z <0.10. After matching sample galaxies in clusters with Galaxy Evolution Explorer (GALEX) GR5, we have classified the morphologies of ETGs by UV-optical colour distributions and investigated them in terms of the ranks in magnitude in a cluster and in clustocentric distance. It has recently been suggested theoretically that brightest cluster galaxies (BCGs) show a strong UV upturn than non-BCGs, but we find that the difference between them is not significant. Moreover, to our surprise, it appears that density (environment) does not play any significant role to the UV properties. consequent of internal galaxy processes rather than that of environmental processes.

• 천문학회지
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• 제49권2호
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• pp.53-57
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• 2016

We present an optical UBVRI photometric analysis of the poorly studied open star cluster IC 2156 using Sloan Digital Sky Survey data in order to estimate its astrophysical properties. We compare these with results from our previous studies that relied on the 2MASS JHK near-infrared photometry. The stellar density distributions and color-magnitude diagrams of the cluster are used to determine its geometrical structure, real radius, core and tidal radii, and its distance from the Sun, the Galactic plane, and the Galactic center. We also estimate, the age, color excesses, reddening-free distance modulus, membership, total mass, luminosity function, mass function, and relaxation time of the cluster.

• Journal of Astronomy and Space Sciences
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• 제36권1호
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• pp.1-9
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• 2019

In this paper we present analysis of current density when the Cluster spacecraft pass the nightside auroral region at about $4-5R_E$ from the center of Earth. The analysis is made when the inter-spacecraft separation is within 200 km, which allows all four spacecraft to be situated inside the same current sheet. On 22 February 2002, two field-aligned current (FAC) events were observed in both the southern and the northern hemispheres. The FACs were calculated with magnetic field data obtained by the four spacecraft using the Curlometer method. The scales of the FACs along the spacecraft trajectory and the magnitudes were hundreds of kilometers and tens of $nA/m^2$, respectively, and both events were mapped to the auroral region in the ionosphere. We also examined reliability of the results with some parameters, and found that our results are adequately comparable with other studies. Nevertheless, some limitations that decrease the accuracy of current estimation exist.

• 천문학회보
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• 제45권1호
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• pp.62.2-62.2
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• 2020

Globular clusters(GCs) are found not only around galaxies (galaxy GCs), but also between galaxies in galaxy clusters (intracluster GCs; ICGCs). The ICGCs, which are not bound to any of cluster member galaxies, are governed by the galaxy clutster potential. ICGCs have been detected in the wide field of Virgo and Fornax galaxy clusters. However, previous surveys covered only a small fraction of Coma and Perseus. In this study we present a wide field survey of these two galaxy clusters, using Subaru Hyper Suprime-Cam(HSC) archival images, covering a circular field with diameter of ~1.8 deg. We select ICGC candidates, by masking the images of bright galaxies and choosing point sources in the remaining area. We find thousands of ICGCs in each galaxy cluster. These ICGCs show a bimodal color distribution, which is dominated by blue GCs. We investigate spatial distributions and radial number density profiles of the blue and red ICGCs in each galaxy cluster. Implications of the results will be discussed.

• 천문학회보
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• 제46권1호
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• pp.33.2-33.2
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• 2021

To study environmental effects on the circumgalactic medium (CGM), we use the samples of redMaPPer galaxy clusters, background quasars and cluster galaxies from the SDSS. With 82,000 quasar spectra, we detect 197 MgII absorbers in and around the clusters. The detection rate per quasar is 2.70 times higher inside the clusters than outside the clusters, indicating that MgII absorbers are relatively abundant in clusters. However, when considering the galaxy number density, the absorber-to-galaxy ratio is rather low inside the clusters. If we assume that MgII absorbers are mainly contributed by the CGM of massive star-forming galaxies, a typical halo size of cluster galaxies is smaller than that of field galaxies by 30 per cent. This finding supports that galaxy haloes can be truncated by interaction with the host cluster.

• 천문학논총
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• 제32권1호
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• pp.287-291
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• 2017

We present the results of our mid-infrared (MIR) observations of distant clusters of galaxies with AKARI. The wide-field of view of IRC/AKARI ($10^{\prime}{\times}10^{\prime}$) is ideally suited for studying dust-obscured star-formation (SF) activity of galaxies along the cosmic web in the distant universe. We performed a deep and wide-field $15{\mu}m$ (rest-frame ${\approx}8{\mu}m$) imaging observation of the RXJ1716+6708 cluster (z = 0.81) with IRC. We find that $15{\mu}m$-detected cluster member galaxies (with total infrared luminosities of $L_{IR}{\geq}10^{11}L_{\odot}$) are most preferentially located in the cluster outskirt regions, whilst such IR-luminous galaxies avoid the cluster centre. Our $H{\alpha}$ follow-up study of this field confirmed that a significant fraction of $15{\mu}m$-detected cluster galaxies are heavily obscured by dust (with $AH{\alpha}$>3 mag in extreme cases). The environment of such dusty star-burst galaxies coincides with the place where we see a sharp "break" of the colour-density relation, suggesting an important link between dust-obscured SF activity and environmental quenching. We also report the discovery of a new cluster candidate around a radio galaxy at z = 1.52 (4C 65.22), where we obtained one of the deepest IRC imaging datasets with all the nine filters at $2-24{\mu}m$. This field will provide us with the final, excellent laboratory for studying the dust-enshrouded SF activity in galaxies along the cosmic web at the critical epoch of cluster galaxy evolution with AKARI.

• 천문학회보
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• 제37권1호
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• pp.41.1-41.1
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• 2012

Interactions between the galactic interstellar medium (ISM) and the intra cluster medium (ICM) are believed to be one of the main processes affecting galaxy evolution in cluster environments. The aim of our research is to study the molecular gas properties of a galaxy under the ICM pressure in the cluster environment. It has been well known that cluster galaxies are deficient in atomic hydrogen gas (HI gas) compared to their field counterparts and now there is much evidence that low density ISM is being removed by ram pressure due to ICM wind. Meanwhile, no significant molecular gas deficiency of the cluster galaxy population has been found yet they show overall lower star formation rate than galaxies in the field, and it is still puzzling how the star formation could decrease without stripping of dense molecular gas. To address this issue, we probe the detailed molecular gas properties of NGC 4402, located near the cluster center, as part of a study of four spiral galaxies in the Virgo Cluster. NGC 4402 is well known undergoing ram pressure stripping with a truncated HI disk($D_{HI}/D_{opt}$ - 0.75 and only 36% of HI gas compare to field galaxies of a similar size) and a disturbed gas morphology. Comparing the high resolution 12CO and 13CO data of NGC 4402 from the Sub Millimeter Array (SMA) with existing other wavelength data, we probe the spatial distribution and a physical condition of molecular gas under strong ICM pressure. We discuss the star formation activity might have been altered and hence how the global color of NGC4402 would change in the future.

• 천문학회지
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• 제33권2호
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• pp.111-121
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• 2000

Many models of globular cluster formation assume the presence of cold dense clouds in early universe. Here we re-examine the Fall & Rees (1985) model for formation of proto-globular cluster clouds (PGCCs) via thermal instabilities in a protogalactic halo. We first argue, based on the previous study of two-dimensional numerical simulations of thermally unstable clouds in a stratified halo of galaxy clusters by Real et al. (1991), that under the protogalactic environments only nonlinear (${\delta}{\ge}1$) density inhomogeneities can condense into PGCCs without being disrupted by the buoyancy-driven dynamical instabilities. We then carry out numerical simulations of the collapse of overdense douds in one-dimensional spherical geometry, including self-gravity and radiative cooling down to T = $10^4$ K. Since imprinting of Jeans mass at $10^4$ K is essential to this model, here we focus on the cases where external UV background radiation prevents the formation of $H_2$ molecules and so prevent the cloud from cooling below $10^4$ K. The quantitative results from these simulations can be summarized as follows: 1) Perturbations smaller than $M_{min}\~(10^{5.6}\;M{\bigodot})(nh/0.05cm^{-3})^{-2}$ cool isobarically, where nh is the unperturbed halo density, while perturbations larger than $M_{min}\~(10^8\;M{\bigodot})(nh/0.05cm^{-3})^{-2}$ cool isochorically and thermal instabilities do not operate. On the other hand, intermediate size perturbations ($M_{min} < M_{pgcc} < M_{max}$) are compressed supersonically, accompanied by strong accretion shocks. 2) For supersonically collapsing clouds, the density compression factor after they cool to $T_c = 10^4$ K range $10^{2.5} - 10^6$, while the isobaric compression factor is only $10^{2.5}$. 3) Isobarically collapsed clouds ($M < M_{min}$) are too small to be gravitationally bound. For supersonically collapsing clouds, however, the Jeans mass can be reduced to as small as $10^{5.5}\;M_{\bigodot}(nh/0.05cm^{-3})^{-1/2}$ at the maximum compression owing to the increased density compression. 4) The density profile of simulated PGCCs can be approximated by a constant core with a halo of $p{\infty} r^{-2}$ rather than a singular isothermal sphere.

• 인터넷정보학회논문지
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• 제9권4호
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• pp.43-50
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• 2008

에너지 교체가 어려운 무선 센서네트워크(Wireless Sensor Network)에서 에너지 소모량을 줄이기 위하여 효율적 라우팅에 관한 연구가 다양하게 진행되고 있다. 그 중 라우팅 분야는 현재 클러스터링 방식이 가장 효율적인 방식으로 연구되고 있다. 클러스터링 방식은 클러스터를 구성하는 부분과 데이터를 전송하는 부분으로 구성된다. 클러스터를 구성하는 부분은 클러스터 내에 센서 노드들 간에 에너지 소모를 동등하게 하기 위하여 주기적으로 반복된다. 클러스터 구성 부분은 클러스터 헤드 노드를 선정하고 클러스터 헤드 노드에 최적화된 클러스터 멤버 노드를 구성하는 부분으로 알고리즘이 복잡하고 에너지 소모가 크다. 또한 데이터를 전송하는 부분은 크로스오버 영역을 중심으로 에너지 소모량이 $d^2$ 과 $d^4$ 으로 비례된다. 본 논문은 클러스터 방식에서 주기적으로 일어나는 클러스터 구성 부분을 효율화하여 에너지 소모량을 줄이는 방법을 제안하였다. 이 방식은 클러스터의 구성에 있어서 밀도를 고려한 노드가 배치될 영역을 균등 분할하여 클러스터 내의 센서 노드수를 거의 일정하게 하고, 클러스터의 중앙 근처에 헤드 노드의 선정함으로 에너지 소모를 줄이는 방식이다. 이 제안의 타당성을 모의실험을 통하여 보면, LEACH 방식에서의 에너지 소모량보다 적은 것이 확인하였다.

• 한국정보통신학회:학술대회논문집
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• 한국정보통신학회 2015년도 춘계학술대회
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• pp.105-107
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• 2015

본 논문에서는 네트워크의 유동확률밀도를 이용하여 분산적인 라우팅 경로를 분석하는 LTD(Load Tolerance Density-distribution) 알고리즘을 제안한다. 모바일 애드 혹 네트워크(Mobile Ad-hoc Networks)는 유동성을 가진 노드들로 구성된 네트워크로서, 토폴로지의 변화가 빈번하다. 토폴로지의 변화를 줄이기 위해 계층적 네트워크가 연구되었으나, 특정 클러스터 헤드노드에게 부하가 집중되어 통신이 단절된다. 본 논문에서 제안하는 알고리즘은 포아송 분포를 이용한 노드의 유동확률밀도를 계산하여, 분산적인 라우팅 경로를 제공하는 알고리즘이다. 모의실험에서, 본 논문에서 제안한 알고리즘의 패킷 전송률은 비교 알고리즘에 비해 향상된 결과를 보여주었다.