• 천문학회보
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• 제44권1호
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• pp.69.3-69.3
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• 2019

The CHIMPS2 survey is to extend the JCMT HARP $^{13}CO/C^{18}O$ J=3-2 Inner Milky-Way Plane Survey (CHIMPS) and the ${12}^CO$ J=3-2 survey (COHRS) into the inner Galactic Plane, the Central Molecular Zone (CMZ), and a section of the Outer Plane. When combined with the complementary $^{12}CO/^{13}CO/C^{18}O$ J=1-0 survey at the Nobeyama 45m (FUGIN) at matching 15" resolution and sensitivity, and other current CO surveys, the results will provide a complete set of transition data with which to calculate accurate column densities, gas temperatures and turbulent Mach numbers. These will be used to: analyze molecular cloud properties across a range of Galactic environments; map the star-formation efficiency (SFE) and dense-gas mass fraction (DGMF) in molecular gas as a function of position in the Galaxy and its relation to the nature of the turbulence within molecular clouds; determine Galactic structure as traced by molecular gas and star formation; constrain cloud-formation models; study the relationship of filaments to star formation; test current models of the gas kinematics and stability in the Galactic center region and the flow of gas from the disc. It will also provide an invaluable legacy data set for JCMT that will not be superseded for several decades. In this poster, we will present the current status of the CHIMPS2.

• 천문학회보
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• 제44권2호
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• pp.52.2-52.2
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• 2019

In the last decades, the use of type Ia supernovae (SN) as standard candles has allowed us to understand the geometry of the Universe as they help to measure the expansion rate of the Universe, especially in combination with other cosmological probes such as the study of cosmic microwave background radiation anisotropies or the study of the imprint of baryonic acoustic oscillations on the galaxy clustering. Cosmological parameter constraints obtained with type Ia SN are mainly affected by intrinsic systematic errors. But there are other systematic effects related with the correlation of the observed brightness of Supernova and the large-scale structure of the Universe such as the effect of peculiar velocities and gravitational lensing. The former is relevant for SN at low redshifts while the latter starts being relevant for SN at higher redshifts. Gravitational lensing depends on how much matter is along the trajectory of each SN light beam. In order to account for this effect, we consider a statistical approach by defining the probability distribution (PDF) that a given supernova brightness is magnified by a given amount, for a particular redshift. We will show that different theoretical approaches to define the matter density along the light trajectory hugely affect the shape and width of the PDF. This may have catastrophic effects on cosmology fits using Supernova lensing as planned for surveys such as the Dark Energy Survey or future surveys such the Large Synoptic Survey Telescope.

• 대한수학회지
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• 제48권4호
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• pp.669-689
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• 2011

The notion of quasi-Einstein manifolds arose during the study of exact solutions of the Einstein field equations as well as during considerations of quasi-umbilical hypersurfaces. For instance, the Robertson-Walker spacetimes are quasi-Einstein manifolds. The object of the present paper is to study Lorentzian quasi-Einstein manifolds. Some basic geometric properties of such a manifold are obtained. The applications of Lorentzian quasi-Einstein manifolds to the general relativity and cosmology are investigated. Theories of gravitational collapse and models of Supernova explosions [5] are based on a relativistic fluid model for the star. In the theories of galaxy formation, relativistic fluid models have been used in order to describe the evolution of perturbations of the baryon and radiation components of the cosmic medium [32]. Theories of the structure and stability of neutron stars assume that the medium can be treated as a relativistic perfectly conducting magneto fluid. Theories of relativistic stars (which would be models for supermassive stars) are also based on relativistic fluid models. The problem of accretion onto a neutron star or a black hole is usually set in the framework of relativistic fluid models. Among others it is shown that a quasi-Einstein spacetime represents perfect fluid spacetime model in cosmology and consequently such a spacetime determines the final phase in the evolution of the universe. Finally the existence of such manifolds is ensured by several examples constructed from various well known geometric structures.

• 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).

• 한국전자거래학회지
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• 제22권1호
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• pp.123-146
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• 2017

소비자들이 SNS에 공유하는 정보는 소비자들의 구매나 선택에 대한 결정에 많은 영향을 미친다. 이에 소셜 빅데이터를 활용하여 소비자 가치를 분석한 새로운 연구방법론에 주목할 필요가 있다. 이러한 맥락에서 본 연구의 목적은 소셜 빅데이터 분석을 통해 소비자의 가치 인식을 계량적으로 분석해 보고자한다. 이러한 분석 결과를 토대로 광고전략 개발에 적용할 수 있는지를 규명하고자 하였다. 본 연구에서는 3가지 스마트폰 브랜드에 대해 텍스트 마이닝과 긍 부정 이미지 분석을 활용함으로써 소비자 가치 구조를 파악하였다. 분석결과 브랜드별 소비자의 가치 인식에 대한 감성적인 측면과 이성적인 측면에서 차별적인 내용을 선별할 수 있었다. 갤럭시 S7과 아이폰 6S의 경우 출시일 이전에는 감성적인 측면이 중요한 것으로 나타났지만 출시일 이후에는 이성적인 측면이 중요한 것으로 나타났다. 그러나 LG G5의 경우 출시일 이전이나 이후 모두 감성적인 측면이 중요한 것으로 나타났다. 또한 소비자 가치 인식의 분석 결과를 바탕으로 핵심적인 광고전략 2가지 안을 제안할 수 있다. 갤럭시 S7의 경우 광고전략 개발 시 제품속성에 대한 성능이나 차별화된 기능 등 이성적 측면을 강조해야 할 필요성이 있다. LG G5의 경우 광고전략에서 제품을 사용함으로써 느껴지는 행복감, 설레임, 즐거움, 재미 등의 감성적 측면을 광고전략 개발에 중요하게 고려할 필요가 있다. 결과적으로 본 연구는 소비자 가치 분석을 통해 실제 광고전략에 좋은 기준을 제시할 것으로 판단된다. 광고전략은 주로 직감이나 경험에 의해 이루어진다. 이에 소셜 빅데이터 분석을 통한 소비자의 가치 인식 분석으로 광고전략을 개발하는 것은 중요한 시사점을 안겨 줄 것으로 판단한다.

• 정보처리학회논문지:소프트웨어 및 데이터공학
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• 제10권10호
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• pp.421-428
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• 2021

HEIF(High Efficiency Image File Format)는 MPEG에서 개발된 이미지 포맷으로써, 비디오 코덱인 H.265를 활용하여 정지된 화면을 하나의 이미지 형태로 저장할 수 있도록 개발된 컨테이너이다. 아이폰은 2017년부터 HEIF를 사용하고 있으며, 2019년부터는 갤럭시 S10과 같은 안드로이드 기기도 해당 포맷을 지원하고 있다. 이 포맷은 우수한 압축률을 가지도록 이미지를 제공할 수 있으나, 복잡한 내부 구조를 가지고 있어 기기나 소프트웨어 간 호환성이 현저하게 부족하여 일반적으로 사용되는 JPEG(또는 JPG) 파일을 대체하기에는 아직 대중적이지 못한 상황이다. 하지만 이미 많은 기기에서 HEIF를 사용하고 있음에도 불구하고 디지털 포렌식 연구는 부족한 상황이다. 이는 디지털 포렌식 조사 과정에서 파일 내부에 포함된 정보의 파악이 미흡하여 잠재적인 증거를 놓칠 수 있는 위험에 노출될 수 있다. 따라서 본 논문에서는 아이폰에서 촬영된 HEIF 형식의 사진 파일과 갤럭시에서 촬영된 모션 포토 파일을 분석하여 파일 내부에 포함된 정보와 특징들을 알아본다. 또한 이미지 뷰어 기능을 지원하는 소프트웨어를 대상으로 HEIF에 대한 지원 여부를 조사하고 HEIF를 분석하는 포렌식 도구의 요구사항을 제시한다.

• Journal of Astronomy and Space Sciences
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• 제22권2호
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• pp.125-138
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• 2005

S152 분자운은 S152 분자운 복합체의 중심부에 있으며 페르세우스 나선 팔에 위치하고 있는 작고 밝은 발광 성운이다. 이 분자운까지의 광학적 거리는 3.5kpc이며 지름은 약 1.5pc으로 알려져 있다 . S152 분자운 좌측에는 초신성 잔해로 알려진 SNR G109.1-1.0이 위치하며, S152 분자운 복합체 전체 구조는 전갈 형태를 띠고 있는데, SNR G109.1-1.0과 S152 분자운이 접하는 부분은 특이한 반구 형태를 띠고 있어 많은 연구가 진행되어 왔다. 본 연구에서 FCRAO $^{12}CO(J=\;1{\to}0)$우리 은하 탐사 자료를 이용해 S152 분자운 복합체의 전체 속도 구조를 분석한 결과, 세 개의 다른 속도 성분 값 -54.5, -50.4, -48.8km $s^{-1}$ 에서 구조적인 차이를 보였다. S152 분자운 복합체의 속도 기울기는 0.21km $s^{-1}pc^{-1}$과 0.16km $s^{-1}pc^{-1}$인데 두 개의 속도 기울기 방향이 다르게 분석되었다. 이것은 S152 분자운 주변 영역이 SNR G109.1-1.0 과 상호 작용을 일으킨 후 다른 가스 운들이 병합되면서 서로 다른 진화 과정을 거친 결과로 생각된다.

• 천문학논총
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• 제27권4호
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• pp.219-220
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• 2012

We present the results of far-infrared spectroscopic observations of the Large Magellanic Cloud (LMC) with FIS-FTS. We covered a large area across the LMC, including 30 Doradus (30 Dor) and N44 star-forming regions, by 191 pointings in total. As a result, we detect the [OIII] and [CII] line emission as well as far-infrared dust continuum emission throughout the LMC. We find that the [OIII] emission is widely distributed around 30 Dor. The observed size of the distribution is too large to be explained by massive stars in 30 Dor, which are assumed to be enshrouded by clouds with the constant gas density estimated from the [OIII] line intensities. Therefore the surrounding structure is likely to be highly clumpy. We also find a global correlation between the [OIII] and the far-infrared continuum emission, suggesting that the gas and dust are well mixed in the highly-ionized region where the dust survives in clumpy dense clouds shielded from energetic photons. Furthermore we find that the ratios of [CII]/CO are as high as 110,000 in 30 Dor, and 45,000 even on average, while they are typically 6,000 for star-forming regions in our Galaxy. The unusually high [CII]/CO is also consistent with the picture of clumpy small dense clouds.

• 천문학논총
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• 제27권4호
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• pp.335-338
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• 2012

We present the $18{\mu}m$ luminosity function (LF) of galaxies at 0.006 < z < 0.8 (the average redshift is ~ 0.04) using the AKARI mid-infrared All-Sky Survey catalogue. We have selected 243 galaxies at $18{\mu}m$ from the Sloan Digital Sky Survey (SDSS) spectroscopic region. These galaxies then have been classified into five types; Seyfert 1 galaxies (Sy1, including quasars), Seyfert 2 galaxies (Sy2), low ionization narrow emission line galaxies (LINER), galaxies that are likely to contain both star formation and Active Galactic Nuclei (AGN) activities (composites), and star forming galaxies (SF) using optical emission lines such as the line width of $H{\alpha}$ or the emission line ratios of [OIII]/$H{\beta}$ and [NII]/$H{\alpha}$. As a result of constructing the LF of Sy1 and Sy2, we found the following results; (i) the number density ratio of Sy2 to Sy1 is $1.64{\pm}0.37$, larger than the results obtained from optical LF and (ii) the fraction of Sy2 in the entire AGN population may decrease with $18{\mu}m$ luminosity. These results suggest that most of the AGNs in the local universe are obscured by dust and the torus structure probably depends on the mid-infrared luminosity.

• 천문학회지
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• 제48권4호
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• pp.213-228
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• 2015

The Horizon Run 4 is a cosmological N-body simulation designed for the study of coupled evolution between galaxies and large-scale structures of the Universe, and for the test of galaxy formation models. Using 6300³ gravitating particles in a cubic box of L_box = 3150 h⁻¹Mpc, we build a dense forest of halo merger trees to trace the halo merger history with a halo mass resolution scale down to M_s = 2.7 × 10¹¹h⁻¹M_⊙. We build a set of particle and halo data, which can serve as testbeds for comparison of cosmological models and gravitational theories with observations. We find that the FoF halo mass function shows a substantial deviation from the universal form with tangible redshift evolution of amplitude and shape. At higher redshifts, the amplitude of the mass function is lower, and the functional form is shifted toward larger values of ln(1/σ). We also find that the baryonic acoustic oscillation feature in the two-point correlation function of mock galaxies becomes broader with a peak position moving to smaller scales and the peak amplitude decreasing for increasing directional cosine μ compared to the linear predictions. From the halo merger trees built from halo data at 75 redshifts, we measure the half-mass epoch of halos and find that less massive halos tend to reach half of their current mass at higher redshifts. Simulation outputs including snapshot data, past lightcone space data, and halo merger data are available at http://sdss.kias.re.kr/astro/Horizon-Run4.