• Journal of Conservation Science
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• v.37 no.2
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• pp.154-166
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• 2021

The royal seal, in either gold or jade, is used to symbolize Joseon's royal family, and it is made up of a Bonu (a handle), Bosin (a body), Bomun (a letter inscribed on the seal), and Bosu (a string attached to the seal). The Bosu was designed to enhance the seal's dignity and facilitate convenient handling. Bosu consists of Kkeun-mog and Bangwool-sul (decorated with gilt paper), which are made of Bangwool, Bangwool-mog, and Sul. In this study, the form survey, color, material, and composition of 318 Bosu pieces from the Joseon Dynasty and Korean Empire produced from 1441 to 1928 were analyzed. As time passed, the strings on the seals became longer and thinner. Bangwool-mog disappeared from the mid-1800s, and a ring appeared at the end of the Sul. Most of the colors used were scarlet, but orange and purple were also identified. Although most of the Bosu are silk, five Bosu from the 1900s and one Bosu from the 1740s (likely replaced in the 1900s) are estimated to be rayon. The gilt paper's main chemical components used to decorate the Bangwool-sul vary according to age. Until the mid-1800s, gold (Au) was used for the Sul and Bangwool, but since the mid-1800s, gold (Au) and brass (Cu-Zn) were used for Sul and Bangwool, respectively, and then brass (Cu-Zn) was used for Sul and Bangwool. While the Bosu was a seal accessory, it can be used to identify changes in the manufacturing techniques and materials of the period.

• Proceedings of the Korean Vacuum Society Conference
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• 2016.02a
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• pp.282.2-282.2
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• 2016

중적외선 물질에는 Ge, ZnS, ZnSe, Si 등이 있으나 고굴절율이므로 반사가 매우 크게 발생을 한다. 이를 줄이기 위해 다층 박막 무반사 코팅을 일반적으로 사용하지만 열에 취약함, 적합한 물질을 찾는 것이 매우 어려움, 다층 박막으로 제작 시 두께가 매우 두꺼워짐의 단점이 있다. 또한 Ge, ZnS, ZnSe 의 소재는 가격이 Silicon에 비해 매우 비싸다. 그러므로 RCWA(Rigorous Coupled Wavelength Analysis) 시뮬레이션을 이용하여 상대적으로 저렴한 소재임에도 고투과성을 지닌 중적외선용 무반사 실리콘 서브파장구조(Subwavelength Structures, SWSs)를 제안한다. 본 연구에서는 원기둥, 원뿔, 파라볼라, 잘린 원뿔(truncated cone) 등의 형태에 따른 투과율 특성을 파악하여 최적구조가 파라볼라 형태임을 증명하였다. 또한 서브파장구조의 주기, 높이의 특성을 조절하여 공정 시의 종횡비(Aspect ratio)를 고려한 최적형태를 제안하였다. 중적외선 영역($3{\mu}m{\sim}5{\mu}m$)에서 일반 Silicon의 적외선 영역에서 평균 55%의 낮은 투과율을 보이나, 양면에 무반사 구조를 설계 하였을 때 평균 94%의 높은 투과율을 확인할 수 있다. 다양한 형태를 가진 무반사 실리콘 서브파장 구조물을 RCWA 방식으로 계산함으로서 특성을 파악하며 최적구조를 설계 할 수 있다. 또한 단면에 비하여 양면으로 SWSs 구조를 제작할 시 매우 두드러지는 투과특성을 확인할 수 있다. 고굴절율이지만 뛰어난 투과특성을 이용하여 초소형 적외선 카메라 렌즈 뿐만 아니라 적외선 광검출기, 광학 필터 등에 이용 가능할 것으로 예상된다.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.2
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• pp.72.2-72.2
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• 2013

We present a UBVI and $H{\alpha}$ photometric study of the young open cluster NGC 1893 in the outer Galaxy as part of "Sejong Open cluster Survey (SOS)" project. Using the properties of early-type stars in the photometric diagrams 65 early-type members were selected. More than 120 $H{\alpha}$ emission stars and candidates were found by $H{\alpha}$ photometry. Together with the published young stellar object catalogue and X-ray source list for this cluster, a total of 837 pre-main sequence (PMS) stars were identified in our photometric data. We obtained the mean reddening of < E(B-V) > = $0.56{\pm}0.08$ mag from the (U-B, B-V) diagram and confirmed the normal reddening law ($R_V=3.1$) toward NGC 1893 based on color excess ratios from optical to mid-infrared wavelengths. The zero-age main sequence fitting to the reddening-corrected color-magnitude diagrams gives a distance modulus of $V_0-M_V=12.8{\pm}0.1$. The age of the cluster inferred from stellar evolution models is about 1-2 Myr. We also found the Salpeter/Kroupa type initial mass function for this cluster. Finally, the mass accretion rate of 80 PMS stars with UV excess emission was estimated for the stars with masses from $0.6M_{\odot}$ to $5M_{\odot}$.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.2
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• pp.34.2-34.2
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• 2013

Star formation beyond the galaxy discs and the principles governing it have attracted a lot of recent attention and the advent of ultraviolet (UV) and mid-infrared (MIR) telescopes like the GALEX and Spitzer have enabled major advances in such studies. In order to study the HI gas properties such as the morphology, kinematics and column density distributions, and their correlation with the star forming zones, especially in the tidal bridges, tails and debris, we carried out an HI survey of a set of Spitzer-observed interacting systems using the Giant Metrewave Radio Telescope (GMRT). Here we present results from three of these systems, Arp86, Arp181 and Arp202. In Arp86, we detect excellent star-gas correlation in the star forming tidal bridges and tails. In Arp181, we find the two interacting galaxies to be highly gas depleted and the entire gas of the system is found in the form of a massive tidal debris about 70 kpc from the main galaxies. In all three cases, Arp86, Arp181 and Arp202, the tidal debris seem to host ongoing star formation. We also detect three new candidate tidal dwarf galaxies (TDG) in these systems with large quantities of gas associated with them.

• Journal of The Korean Astronomical Society
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• v.45 no.5
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• pp.117-125
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• 2012

We present $^{12}CO$ J = 2-1 line observations of G54.1+0.3, a composite supernova remnant with a mid-infrared (MIR) loop surrounding the central pulsar wind nebula (PWN). We map an area of $12^{\prime}{\times}9^{\prime}$ around the PWN and its associated MIR loop. We confirm two velocity components that have been proposed to be possibly interacting with the PWN/MIR-loop; the +53 km $s^{-1}$ cloud, which appears in contact with the eastern boundary of the PWN and the +23 km $s^{-1}$ cloud, which has CO emission coincident with the MIR loop. However, we have not found a direct evidence for the interaction in either of these clouds. Instead, we detected an 5'-long arc-like cloud at +15-+23 km $s^{-1}$ with a systematic velocity gradient of ~3 km $s^{-1}$ $arcmin^{-1}$ and broad-line emitting CO gas with widths (FWHM) of ${\leq}7km\;s^{-1}$ in the western interior of the supernova remnant. We discuss their association with the supernova remnant.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.1
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• pp.56.2-56.2
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• 2012

We present a study of the asymptotic giant branch (AGB) contribution to the total Ks band luminosity of star clusters in the Large Magellanic Cloud (LMC) as a function of age. AGB stars, a representative intermediate-age population, are a strong source of NIR to MIR emission so that they are a critical component for understanding the near-to-mid infrared observation of galaxies. Current calibration of IR emission in evolutionary population synthesis (EPS) models for galaxies is mainly based on a small number of LMC star clusters. However, each LMC star cluster with intermediate age contains only a few AGB stars so that it suffers from a stochastic effect. Therefore a large number of them are needed for solid calibration of the EPS models. We study physical properties of a large number of LMC star clusters to estimate the Ks band luminosity fraction of AGB stars in star clusters as a function of age. We discuss the stochastic effect in calibrating models, and the importance of this calibration for studying the evolution of not only nearby galaxies but also of high-z galaxies.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.72.1-72.1
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• 2010

Gas materials in the inner Galactic disk continuously migrate toward the Galactic center (GC) due to interactions with the bar potential, magnetic fields, stars, and other gaseous materials. In case of the Milky Way, those in forms of molecules appear to accumulate around 200 pc from the center (the central molecular zone, CMZ) to form stars there and further inside. The bar potential in the GC is thought to be responsible for such acculmulation of molecules and subsequent star formation, which is believed to have been continous throughout the lifetime of the Galaxy. We present 3-D hydrodynamic simulations of the CMZ that consider self-gravity, radiative cooling, and supernova feedback, and discuss the efficiency and role of the star formation in that region. We find that the gas accumulated in the CMZ by a bar potential of the inner bulge effectively turns into stars, supporting the idea that the stellar cusp inside the central 200 pc is a result of the sustained star formation in the CMZ. The obtained star formation rate in the CMZ, 0.03-0.1 Msun, is consistent with the recent estimate based on the mid-infrared observations by Yusef-Zadeh et al. We discuss the secular evolution of nuclear bulges in general, based on our results.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.40.2-40.2
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• 2010

Polycyclic aromatic hydrocarbon (PAH) features have emerged as one of the most important infrared (IR) features since these PAH features dominate mid-IR spectra of galaxies and are ubiquitous within galactic and extragalactic objects. These PAH features have the potentials to become reliable star formation rate (SFR) proxies and diagnostics of physical conditions of interstellar medium, such as ionization states of dust grains and grain sizes. While constructing an unbiased library of 44 sample galaxies selected from 5MUSES sample, AKARI mJY Unbiased Survey of Extragalactic Sources in 5MUSES (AMUSES) intends to measure and to calibrate the PAH 3.3 mm emission feature which has not been studied extensively due to its weak strength and dearth of capable instruments. Out of 20 target galaxies, we detected the 3.3mm feature from eight galaxies and measured their line strengths, line widths and line ratios with other PAH emission features. Sample galaxies whose spectral energy distributions (SEDs) are classified as starburst-type have clearly stronger 3.3mm emission features than ones with AGN-type SEDs. We also found that there is a correlation between the PAH 3.3mm luminosity and total IR luminosity within our sample galaxies, albeit a large scatter. We further discuss implications of our results.

• Journal of the Korean Society for Aeronautical & Space Sciences
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• v.40 no.8
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• pp.688-694
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• 2012

A study on the effect of engine nozzle configuration on the engine plume Infra-red (IR) signature characteristics is performed. Configuration design of an engine nozzle with high aspect ratio to reduce IR signature level and a cylindrical nozzle which is typically used for conventional aircraft which does not require IR signature reduction is performed. And CFD analysis for the two nozzles is performed to compare the flowfields characteristics of the two nozzles. Finally IR signature analysis for the two nozzles is accomplished to calculate the total intensity level at mid-wave infra-red and investigate the differences of IR signature characteristics between the two nozzles.

• Proceedings of the KSRS Conference
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• 2008.03a
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• pp.125-130
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• 2008

Mid-Infrared (MIR) 영상은 화산 활동 및 산불로 인한 재난관측, 지표물질 관측, 해수 온도 측정과 같은 분야들에서 사용되고 있다. 그러나 MIR영역은 지표의 복사율과 대기의 영향으로 인한 변화가 매우 심하고, 낮 영상의 경우 태양 복사량에 의한 영향도 고려해야 하는 어려움이 있다. 따라서 단일밴드인 MIR영상을 이용하여 표면온도를 얻기 위해서는 영상이 취득된 시간과 장소에서 관측된 태양 복사량 및 여러 가지 대기 변수가 필요하다. 본 연구의 목적은 기존의 MIR 영상 연구가 다중밴드를 기반으로 한 것과 달리 단일 밴드의 영상을 이용하여 표면온도를 측정하는데 있다. 이를 위하여 MODIS MIR 영상을 대상으로 MODTRAN을 사용하여 MIR 영역의 대기보정 기법을 적용 한 뒤 복사전달 모델을 이용하여 지표의 복사량을 측정하였다. 획득된 지표온도 영상의 정밀도를 측정하기 위해서 기존의 온도 알고리즘인 split-window algorithm에 의해 얻어진 해수온도 영상과의 비교를 통하여 오차 원인에 대해 분석을 실시하였다. 그 결과 낮 영상의 경우 -4.19${\pm}$1.19$^{\circ}C$ 정도의 온도 차가 났으며, 밤 영상의 경우 0.5$^{\pm}C$0.39$^{\circ}C$ 정도로 비교적 좋은 결과를 보였다. 이는 낮 영상의 경우 지표의 복사율에 대한 온도의 민감도가 매우 높기 때문에 높은 오차가 발생하지만, 밤 영상의 경우 태양빛에 의한 영향이 없으므로 좋은 결과를 나타내기 때문이다. 따라서 단일밴드 MIR영상을 이용한 지표온도 추정 시 대기에 의한 영향보다 지표 복사율에 의한 영향이 높다고 추정할 수 있다.