• 한국수자원학회논문집
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• 제33권2호
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• pp.219-227
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• 2000

전선에 의한 강수는 종종 한반도에서 국지적인 집중호우를 유발한다. 그러나 관측자료의 결핍과 전선의 중규모적 구조에 대한 이해 부족으로 정확하고 신속한 강수량 예측이 어려운 실정이다. 레이더의 공간 해상도는 수 km, 시간 해상도는 수 분으로 중규모 이하의 현상에 대한 관측자료를 제공할 수 있기 때문에 레이더의 효용성은 널리 알려져 있다. 따라서 본 연구에서는 한반도에서 대표적인 전선성 강수 사례를 선택하여 중규모적 특성을 레이더 연직 단면 관측자료에 근거하여 분석하였다. 강수계 내에서 수평규모 약 10 - 20 km의 대류 세포들이 존재하며, 연직 단면도 상에서 나타나는 밝은 띠에 의하면 녹는고도($0^{\circ}C$ 층)는 약 3 - 5 km 사이에 위치하고 있다. 강수 입자에 의하여 추정되는 구름의 높이는 대략 12 km에 달한다. 발달한 층운 지역에서 강수입자의 최대 낙하속도는 밝은 띠가 나타나는 녹는고도 바로 하층에서 나타나고 있다.

• 천문학회보
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• 제39권2호
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• pp.95-95
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• 2014

The mass measurement of neutron stars or black holes is of fundamental importance in our understanding of the evolution of massive stars and core-collapse supernova explosions as well as some exotic physics of the extreme conditions. Despite the importance, however, it's very difficult to measure mass of these objects directly. One way to do this, if they are in binary systems, to measure their binary motions (i.e., Doppler shifts) which can give us direct information on their mass. Recently many new highly-obscured massive X-ray binaries have been discovered by new hard X-ray satellites such as INTEGRAL and NuSTAR. The new highly-obscured massive X-ray binaries are faint in the optical, but bright in the infrared with many emission lines. Based on the near-infrared spectroscopy, one can first understand the nature of stellar companions to the compact objects, determining its spectral types and luminosity classes as well as mass losses and conditions of (potential) circumstellar material. Next, spectroscopic monitoring of these objects can be used to estimate the mass of compact objects via measuring the Doppler shifts of the lines. For the former, broad-band spectroscopy is essential; for the latter, high-resolution spectroscopy is critical. Therefore, IGRINS appears to be an ideal instrument to study them. An IGRINS survey of these new highly-obscured massive X-ray binaries can give us a rare opportunity to carry out population analyses for understanding the evolution of massive binary systems and formation of compact objects and their mass ranges. In this talk, we will present a sample near-infrared high resolution spectra of HMXB, IGR J19140+0951 and discuss about its spectral feature. These spectra are obtained on 13th July, 2014 from IGRINS commissioning run at McDonald 2.7m telescope. And at final, we will introduce the upgrade plan of IGRINS Operation Software (IGOS), to gather the input from IGRINS observer.

• 천문학회보
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• 제41권2호
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• pp.35.1-35.1
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• 2016

To understand the coevolution of Brightest Cluster Galaxies (BCGs) and their host clusters, we conduct a case study on the BCGs in dynamically young and old clusters, Abell 1139 (A1139) and Abell 2589 (A2589). We analyze the pixel color-magnitude diagrams (pCMDs) using deep g- and r-band images, obtained from the CFHT observations. (1) While the overall shapes of the pCMDs are similar to those of typical early-type galaxies, the A2589-BCG tends to have redder mean pixel color and smaller pixel color deviation at given surface brightness than the A1139-BCG. (2) The mean pixel color distribution as a function of pixel surface brightness indicates that the A2589-BCG formed a larger central body by major dry mergers at an early epoch than the A1139-BCG, while they have grown commonly by subsequent minor mergers. (3) The spatial distributions of the pixels with deviated colors reveal that the A1139-BCG experienced considerable tidal events more recently than the A2589-BCG, whereas the A2589-BCG has an asymmetric compact core possibly resulting from major dry merger at an early epoch. (4) The A2589-BCG shows a very large faint-to-bright pixel number ratio compared to early-type non-BCGs, whereas the ratio for the A1139-BCG is not distinctively large. These results imply that the BCG in the dynamically older cluster (A2589) formed earlier and is relaxed better.

• 천문학회보
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• 제42권2호
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• pp.39.1-39.1
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• 2017

The standard hierarchical galaxy formation scenario in the popular LCDM cosmogony has been very successful in explaining the large-scale distribution of galaxies. However, one of the failures of the theory is that it predicts too many satellite galaxies associated with massive galaxies compared to observations, which is called the missing satellite galaxy problem. Isolated groups of galaxies hosted by passively evolving massive early-type galaxies are ideal laboratories for finding the missing physics in the current theory. We discover through a deep spectroscopic survey of galactic satellite systems that bright isolated early-type galaxies have almost no satellite galaxies fainter than the r-band absolute magnitude of about Mr=-14. The cutoff is at somewhat brighter magnitude of about Mr=-15 when only early-type satellites are used. Such a cutoff is not observed in the luminosity function of galaxies in the field. Physical properties of the observed satellites depend sensitively on the host-centric distance. All these are strong evidence that galactic satellites can become invisible due to astrophysics of satellite-host galaxy interaction. A recent state-of-the-art hydrodynamic simulation of galaxy formation does not reproduce such a cutoff in the satellite galaxy luminosity function. But the past history of the simulated satellites shows that many satellite galaxies near or somewhat fainter than the cutoff magnitude have recently become extinct through fatal encounters with the host or other satellite galaxies. Our observation indicates that the missing satellite galaxy problem could be mitigated if the astrophysics of galaxy interaction is more elaborated in the theory.

• Bulletin of the Korean Chemical Society
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• 제35권12호
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• pp.3590-3594
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• 2014

Blue phosphorescent $(dfpypy)_2Ir(mppy)$, where dfpypy = 2',6'-difluoro-2,3'-bipyridine and mppy = 5-methyl-2-phenylpyridine, has been synthesized by newly developed effective method and its solid state structure and photoluminescent properties are investigated. The glass-transition and decomposition temperature of the compound appear at $160^{\circ}C$ and $360^{\circ}C$, respectively. In a crystal packing structure, there are two kinds of intermolecular interactions such as hydrogen bonding ($C-H{\cdots}F$) and edge-to-face $C-H{\cdots}{\pi}(py)$ interaction. This compound emits bright blue phosphorescence with ${\lambda}_{max}=472nm$ and quantum efficiencies of 0.23 and 0.32 in fluid and the solid state. The emission band of the compound is red-shifted by 40 nm relative to homoleptic congener, $Ir(dfpypy)_3$. The ancillary ligand in $(dfpypy)_2Ir(mppy)$ has been found to significantly destabilize HOMO energy, compared to $Ir(dfpypy)_3$, $(dfpypy)_2Ir(acac)$ and $(dfpypy)_2Ir(dpm)$, without significantly changing LUMO energy.

• 천문학논총
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• 제20권1호
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• pp.151-161
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• 2005

The reimaging optics of the KASINICS (KASI Near Infrared Camera System) includes many transparent components like an entrance window, band-pass filters, and blocking filters. As observational targets or in-field background objects, bright stars may cause optical ghosts that can significantly degrade the system performance of the KASINICS. We estimated analytically the relative brightness of ghost components with respect to a point source and examined the effects of tilting optical components as a method of suppressing ghosts. We also performed numerical ray tracings including all the optical components and found the results are consistent with those of the analytic estimations. We conclude that the KASINICS will not suffer from significant ghost effects with appropriate anti-reflection coatings and fittings for the optical components.

• 천문학회지
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• 제41권5호
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• pp.121-137
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• 2008

We present optical and near-infrared imaging and long-slit spectroscopy for the blue compact dwarf galaxy (BCD) Mrk 49 in the Virgo Cluster. The surface brightness distribution analysis shows that Mrk 49 consists of an off-centered blue bright compact core of r = 10" and a red faint outer exponential envelope. The $H_{\alpha}$ image and color difference suggest that these two components have different stellar populations: a high surface brightness population of massive young stars and an underlying low surface brightness population of older stars. The redder near-infrared colors of the inner most region suggest that the near-infrared flux of Mrk 49 originates from evolved massive stars associated with the current star-forming activity. The total apparent magnitude is $B_T\;=\;14.32$ mag and the mean effective surface brightness is ${\mu}_{eff}(B)\;=\;21.56$ mag $arcsec^{-2}$. Long-slit spectroscopy shows that Mrk 49 rotates apparently as a solid body within r = 10" in a plane at position angle 55 degrees with an amplitude of about $20\;km\;sec^{-1}$. The measured radial velocity of Mrk 49 was derived as $1,535\;km\;sec^{-1}$; and the total mass of stars and gases is in the range of 3 to $6\;{\times}\;10^9\;M_{\odot}$. The mass-to-light ratios for the central region of Mrk 49 in I and B band are estimated 1.0 and 0.5, respectively. The upper limit of the dark matter to visible matter ratio seems to be < 5. The oxygen abundance is $12\;+\;\log(O/H)\;=\;8.21\;{\pm}\; 0.1$ which is about one quarter of the solar value while the relative helium abundance appears to be similar to that of the sun.

• 천문학회보
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• 제42권1호
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• pp.50.1-50.1
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• 2017

We present our study of the correlation between star formation rate(SFR) and merging activities of nearby galaxies(d<150Mpc). Our study uses 265 UV-selected galaxies which are not classified as AGN. The UV selection is made using the GALEX Atlas of Galaxies (Gil de Paz+07) and the updated UV catalog of nearby galaxies (Bai+15). We use deep R band optical images reaching to $1{\sigma}$ surface brightness detection limit ${\sim}27mag/arcsec^2$ to classify merger features by visual inspection. We also estimated unobscured SFR($SFR_{NUV}$) and obscured SFR($SFR_{W4}$) using Near-UV continuum and 22 micron Mid-IR luminosity respectively as a indicator of star forming activity. The fraction of galaxies with merger features in each SFR bin is obtained to see if how the fraction of galaxies with merging features($F_m$) changes as a function of SFR. As a result, for 203 late type galaxies(LTGs), we found that merger fraction increases from ~8% up to 50% with $SFR_{W4}$, while for 229 LTGs $SFR_{NUV}$ shows relatively consistent fraction(~18%) of merger fraction. For early type galaxies(ETGs), we could also find no significant correlation between $F_m$ and SFR(both $SFR_{NUV}$ and $SFR_{W4}$). This result suggests that a main driver of star forming activity of UV bright galaxies, especially for obscured late types, is mergers.

• 대한전자공학회논문지SP
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• 제44권1호
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• pp.70-75
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• 2007

44.1kHz 샘플링 레이트의 표준 CD 음질의 오디오 신호를 인터넷 상에서 전송 및 분배하기 위해서는 네트워크 대역폭과 저장 공간의 제한 점을 고려해야 한다. 이러한 제한은 MP3, AAC, OGG 등과 같은 오디오 신호 압축 코덱을 이용하여 해결할 수 있지만, 이러한 코덱들은 공통적으로 고 주파수(High frequency) 대역의 정보가 손실 된다는 문제가 발생한다. 이러한 고주파수 손실은 결국 표준 CD음질을 가지는 오디오 신호보다 제한된 저 주파수 대역만을 재생 할 수 있게 된다. 일반적으로 오디오 신호의 고 주파수 성분은 위치정보 와 명료도, 재생 환경 등에 대한 음의 풍부한 정보를 제공한다. 본 연구에서는 MP3 오디오 코덱으로 디코드(decode) 된 오디오 신호에서 손실된 고 주파수 대역의 정보를 효과적으로 추정 및 복원하는 ARM 플랫폼 기반의 MP3 오디오 음질향상 시스템을 구축하였다. 제안된 시스템과 기존의 대표적인 알고리즘인 Liu의 HFR 과의 비교실험을 통해 제안된 알고리즘이 신호 스펙트럼상에서 고주파 신호 추정 및 복원 능력이 우수함을 볼 수 있고, 알고리즘 연산량도 약 2배 정도 절약할 수 있었다.

• KSBB Journal
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• 제17권2호
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• pp.158-161
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• 2002

본 연구에서는 화학무기, 농약 등에 사용되는 신경독성물질인 유기인화합물의 측정을 위하여 유기인화합물의 효소반응 저해작용을 이용한 광바이오센서장치의 시제품을 제작하였다. 효소반응을 위하여 효소로는 신경세포의 필수효소인 acetylcholinesterase, acetylthiocholine iodide을 사용하였으며 효소반응의 저해제인 유기인화합물로는 paraoxon을 사용하였다. 센서의 폭정원리는 유기인화합물에 의해 저해된 효소반응정도를 효소반응의 생성물인 아세트산의 정량적 측정으로 분석하였으며, pH에 의하여 최대 흡광파장의 변화가 일어나는 litmus를 사용하여 흡광도 측정으로 아세트산의 정량분석을 수행하였다. 광바이오센서 시제품의 제작은 광원으로 고취도 LED와 광세기 측정을 위한 photodiode로 구성하였으며, 제작된 센서를 이용한 실험결과로부터 0 ppm에서 2 ppm의 paraoxon 농도에서 구성된 센서시스템의 선형적 신호 변화를 관찰하였다. 이상의 실헐결과로부터 광바이오센서 시제품은 2분의 반응시간으로 신속하고 정확한 유기인화합물의 정량분석이 가능함을 확인하였다.