• 한국세라믹학회지
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• 제41권8호
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• pp.618-622
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• 2004

플로라이드, 설파이드 및 셀레나이드 유리에 각각 첨가된 홀뮴 이온의 $^{5}$ I$_{5}$ \$\longrightarrow$$^{5}$ I$_{7}$ 전자천이에 기인하는 1.6$\mu$m 형광의 여기 스펙트럼을 $^{5}$ I$_{5}$ 준위가 위치하는 ∼900nm 대역에서 측정하였다. $^{5}$ $F_{1}$ 준위로의 상향전이가 발생하는 특정 파장대역에서 1.6$\mu$m발광의 여기효율이 감소하는 현상이 플로라이드 및 설파이드 유리에서 관찰되었으나 셀레나이드 유리에서는 $^{5}$ I$_{8}$ \$\longrightarrow$$^{5}$ I$_{5}$ 흡수 스펙트럼과 여기 스펙트럼의 모양이 유사하였으며, 이러한 현상은 각 비정질 유전체 재료의 광학적 비선형성과 단파장쪽 투과단의 차이에 기인한다. 한편, Tb$^{3+}$ , Dy$^{3+}$ , Eu$^{3+}$ 또는 N$d^{3+}$ 이온을 공동 첨가함으로써 $^{5}$ I$_{7}$ 준위의 형광수명을 효과적으로 감소시킬 수 있으나 Eu$^{3+}$ 이온을 제외한 나머지 공동 첨가제는 기저상태 흡수를 통하여 1.6 $\mu$m 대역에서의 흡수 손실을 크게 한다. 따라서 형광수명 감소 효과가 Tb$^{3+}$ 이온보다 크지는 않지만 추가적인 흡수 손실이 없는 Eu$^{3+}$ 이온이 공동 첨가제로 더 적합하다.

• 한국재료학회지
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• 제3권2호
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• pp.121-130
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• 1993

합성용질확산법으로 GaP 단결정을 성장시키고, 몇가지 성질을 조사하였다. 결정성장용 석영관을 전기로내에서 1.75mm/day의 속도로 하강시킴으로써 양질의 GaP 단결정을 성장하였다. 에치피트 밀도는 결정의 성장축 방향으로 3.8 ${\times}{10^4}$c$m^{-2}$부터 2.3 ${\times}{10^5}$c$m^2$이었다. 에너지갭의 온도의존성은 실험적으로 $E_g$(T)=[2.3383-(6.082${\times}{10^{-4}}$)$T^2$(373.096+T)eV로 구하여졌다. 저온에서의 광루미네센스 스펙트럼은 구속된 여기자의 복사재결합과 재결합 과정에 포논의 참여로 인하여 에너지갭 부근의 복잡한 선 스펙트럼이 나타났다. n형의 GaP내에서 Zn의 확산깊이는 확산시간의 제곱근에 비례하였으며, 확산계수의 온도의존성은 D(T)=3.2${\times}{10^3}$ exp(-3.486/KbTc$m^2$/sec이었다. p-nGaP 동종접합다이오드의 전기루미제센스 스펙트럼은 깊은 준위의 도너인 Zn-O 복합중심(complex center)과 Zn가 형성한 역셉터 준위사이의 도너-억셉터 쌍 재결합 천이에 의한 630nm의 발광과 에너지갭 부근의 케리어 재결합 처이에 의한 550nm의 발광으로 구성되었으며, 100mA보다 낮은 전류 영역에서 광자의 방출은 bane-filling 과정으로 이루어 진다.

• 마이크로전자및패키징학회지
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• 제6권1호
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• pp.1-10
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• 1999

본 논문에서는 평탄형 GaAs 기판과 $2^{\circ}$, $6^{\circ}$, $10^{\circ}$경사형 GaAs 기판 등 네 종류의 기판에 유기금속 기강성장장치를 이용하여 InGaP 에피막을 성장시켰고, 기판-에피막간의 격자부정합, 탄성변형, 격자굴곡, 부정합응력 등을 측정하여 기판 경사도, 즉 misorientation이 InGaP 에피막의 탄성특성에 미치는 영향에 대해 최초로 연구하였다. 또한 에피막의 x-선 반치폭과 PL강도 및 PL 반치폭, 발진파장 등을 측정하여 기판의 경사도가 에피막의 결정질에 미치는 영향에 대하여도 연구하였다. 시료 분석은 TXRD(tripple-axis x-ray diffractometer)와 저온 (11K) PL(photoluminescence)를 이용하여 수행했다. 기판 경사도 증가에 따라 Ga 원자의 흡착율이 평탄기판의 경우에 비해 상대적으로 증가하였으며, x-선 반치폭이 감소하였다. 또한 선형 탄성이론에 입각하면 격자 misfit 감소에 따라 부정합응력도 감소해야 하나, 반대로 미세하게 증가하는 현상이 관측되었으며 이는 경사기판을 사용할 때 접계면의 에피막 원자의 탄성효율이 향상되는 것에 기인함을 밝혔다. 그리고 기판의 경사도가 증가함에 따라 PL발진파장이 감소하였고, PL 강도는 증가하였으며, PL 반치폭은 감소하였다. 따라서 본 연구에서는 경사기판을 사용할 때 접계면의 탄성효율이 향상되고, InGaP 에피막의 결정질이 향상됨을 밝혔다.

• 한국입자에어로졸학회지
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• 제6권2호
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• pp.51-59
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• 2010

ZnO quantum dots embedded in a silica matrix without agglomeration were synthesized from $TEOS:Zn(NO_3)_2$ solutions in one-step process by aerosol-gel method. It was successfully demonstrated that the size of ZnO Q-dots could be controlled from 2 to 7 mm verified by a high resolution transmission electron microscope observation. The line scanning energy dispersive X-ray spectroscopy(EDS) revealed that the Q-dots existed preferentially inside SiO2 sphere when Zn/Si < 0.5. However, the Q-dots distributed homogeneously all over the sphere when Zn/Si > 1.0. Blue-shifted UV/Vis absorption peak observation confirmed the quantum size effect on the optical properties. The photoluminescence(PL) emission peaks of the powders at room temperature were consistent with previous reports in the following aspects: 1) PL characteristics are dominated by two peaks of deep-level defect-related emissions at 2.4 - 2.8 eV, 2) the first defect-related peak at 2.4 eV was blue shifted due to the quantum size effect with decreasing the concentration of $Zn(NO_3)_2$(decreasing the size of ZnO q dots). More interestingly, the existence of surface-exposed ZnO q dots affects greatly the second defect PL peak at 2.8 eV.

• 천문학회보
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• 제39권2호
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• pp.57.2-57.2
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• 2014

Red active galactic nuclei (AGNs) are supposed to be transitional objects becoming normal AGNs in the galaxy evolution scenario. So far, ~200 red AGNs have been found by very red color in optical through NIR wavelength (e.g., r'-K >5 and J-K>1.3; Urrutia et al. 2009). Here, we compare nuclear activities of the red AGNs to those of normal AGNs to verify the evolutionary phase of the red AGNs. In order to study the nuclear activities of the red AGNs, we use broad emission lines of $P{\beta}$ ($1.28{\mu}m$) of which flux is less suppressed by a factor of 100 than the $H{\beta}$ line in the case of the red AGNs with a color excess of E(B-V)=2 mag. We use 16 red AGNs discovered in previous red AGN surveys by using SDSS, 2MASS, and FIRST (Glikman et al. 2007; Urrutia et al. 2009) at z ~0.7 for which $P{\beta}$ lines are redshifted to the sky window at ${\sim}2.2{\mu}m$. The mean Eddington ratio of the 16 red AGNs is 0.562, and that of the normal AGNs is 0.320, which indicates the red AGNs include more active black hole (BH) than the normal AGNs. To test how significantly the nuclear activities of the red AGNs and the normal AGNs are different, we perform a two-dimensional Kolmogorov-Smirnov test (K-S test) on their Eddington ratio distributions. The K-S test shows the maximum deviation between the cumulative distributions, D, is 0.48, and the probability of null hypothesis, p, is even less than 0.001. This result is consistent with a picture of that the red AGNs are in intermediate phase between the stage of merger-driven starburst galaxy and the normal AGN.

• 천문학회보
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• 제41권2호
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• pp.54.1-54.1
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• 2016

Stellar wind and radiation pressure from massive stars can trigger the formation of new generation of stars. The sequential age distribution of stars, the morphology of cometary globules, and bright-rimmed clouds have been accepted as evidence of triggered star formation. However, these characteristics do not necessarily suggest that new generation of stars are formed by the feedback of massive stars. In order to search for any physical connection between star forming events, we have initiated a study of gas and stellar kinematics in NGC 1893, where two prominent cometary nebulae are facing toward O-type stars. The spectra of gas and stars in optical and near-infrared (NIR) wavelength are obtained with Hectochelle on the 6.5m MMT and Immersion GRating INfrared Spectrograph on the 2.7m Harlan J. Smith Telescope at McDonald observatory. In this study, the radial velocity field of gas across the cluster is investigated using $H{\alpha}$ and [N II] ${\lambda}$ 6584 emission lines, and that of the cometary nebula Sim 130 is also probed using 1-0 S(1) transition line of $H_2$. We report a distinctive velocity field of the cometary nebulae and many ro-vibrational transitions of $H_2$ even at high energy levels in the NIR spectra. These properties indicate the interaction between the cometary nebulae and O-type stars, and this fact can be a clue to triggered star formation in NGC 1893.

• 천문학회보
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• 제37권1호
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• pp.48.1-48.1
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• 2012

We present the ultraviolet (UV) color-color relation of early-type galaxies (ETGs) in the nearby universe (0.05 < z < 0.12) to investigate the properties of hot stellar populations responsible for the UV excess (UVX). The initial sample of ETGs is selected by the spectroscopic redshift and the morphology parameter from the SDSS DR 7, and then cross-matched with the GALEX far-UV (FUV) and near-UV (NUV) GR6 data. The cross-matched ETG sample is further classified by their emission line characteristics in the optical spectra into quiescent, star-forming, and active galactic nucleus categories. Contaminations from early-type spiral galaxies, mergers, and morphologically disturbed galaxies are removed by visual inspection. By drawing the FUV-NUV (as a measure of UV spectral shape) versus FUV-r (as a measure of UVX strength) diagram for the final sample of -3700 quiescent ETGs, we find that the "old and dead" ETGs consist of a well-defined sequence in UV colors, the "UV red sequence," so that the stronger UVX galaxies should have a harder UV spectral shape systematically. However, the observed UV spectral slope is too steep to be reproduced by the canonical stellar population models in which the UV flux is mainly controlled by age or metallicity parameters. Moreover, 2 mag of color spreads both in FUV-NUV and FUV-r appear to be ubiquitous among any subsets in distance or luminosity. This implies that the UVX in ETGs could be driven by yet another parameter which might be even more influential than age or metallicity.

• 천문학회보
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• 제37권1호
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• pp.89.1-89.1
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• 2012

We have investigated a coronal jet observed near the limb on 2010 June 27 by the Hinode/X-Ray Telescope (XRT), EUV Imaging Spectrograph (EIS), and Solar Optical Telescope (SOT), and the SDO/Atmospheric Imaging Assembly (AIA), Helioseismic and Magnetic Imager (HMI), and on the disk by STEREO-A/EUVI. From EUV (AIA and EIS) and soft X-ray (XRT) images we have identified both cool and hot jets. There was a small loop eruption in Ca II images of the SOT before the jet eruption. Using high temporal and multi wavelength AIA images, we found that the hot jet preceded its associated cool jet by about 2 minutes. The cool jet showed helical-like structures during the rising period. According to the spectroscopic analysis, the jet's emission changed from blue to red shift with time, implying helical motions in the jet. The STEREO observation, which enabled us to observe the jet projected against the disk, showed that there was a dim loop associated with the jet. We have measured a propagation speed of ~800 km/s for the dimming front. This is comparable to the Alfven speed in the loop computed from a magnetic field extrapolation of the HMI photospheric field measured 5 days earlier and the loop densities obtained from EIS Fe XIV line ratios. We interpret the dimming as indicating the presence of Alfvenic waves initiated by reconnection in the upper chromosphere.

• 천문학회보
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• 제35권1호
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• pp.79-79
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• 2010

To investigate whether the present-day active galaxies follow the same black hole mass vs. stellar velocity dispersion (MBH-$\sigma*$) relation as quiescent galaxies, we measured the velocity dispersions of a sample of local Seyfert 1 galaxies, for which black hole masses were measured via reverberation mapping. We measured stellar velocity dispersions from high S/N optical spectra centered on the Ca II triplet region (${\sim}8500^{\circ}A$), obtained at the Keck, Palomar, and Lick Observatories. For two objects, in which the Ca II triplet region was contaminated by nuclear emission, we used high-quality H-band spectra obtained with the OH-Suppressing Infrared Imaging Spectrograph and laser-guide star adaptive optics at the Keck-II Telescope. Combining our new measurements with data from the literature, we assemble a sample of 24 active galaxies with stellar velocity dispersions and reverberation MBH in the range of black hole mass 106< MBH /$M{\odot}$ < 109,toobtainthefirstreverberationmappingconstraintsontheslopeandintrinsicscatteroftheMBH- $\sigma*$ relation of active galaxies. Assuming a constant virial coefficient f for the reverberation MBH, we find a slope ${\beta}=3.55{\pm}0.60$ and the intrinsic scatter ${\sigma}int=0.43{\pm}0.08$ dex in the relation log (MBH/M${\odot}$)=$\alpha+\beta$ log(${\sigma}*$/200 km s-1), which are consistent with those found for quiescent galaxies. We derive an updated value of the virial coefficient f by finding the value which places the reverberation masses in best agreement with the MBH - $\sigma*$ relation of quiescent galaxies; using the quiescent MBH - $\sigma*$ relation determined by Gultekin et al. we find log f=0.72+0.09 (or $0.71{\pm}0.10$) with an intrinsic scatter of $0.44{\pm}0.07$ (or 0.46+0.07) dex. No correlations between f and parameters connected to the physics of accretion (such as the Eddington ratio or line-shape measurements) are found. The uncertainty of the virial coefficient remains one of the main sources of the uncertainty in black hole mass determination using reverberation mapping, and therefore also in single-epoch spectroscopic estimates of black hole masses in active galaxies.

• 한국진공학회:학술대회논문집
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• 한국진공학회 2011년도 제40회 동계학술대회 초록집
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• pp.16-16
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• 2011

Plasmas in saline solutions receive considerable attention in recent years. How the operating parameters influence the plasma characteristics and how the electrode erosion occurs have been topics that require further study. In the first part of this talk, the effect of the frequency on the plasmas characteristics in saline solution driven by 50~1000 Hz AC power will be presented. Two distinct modes, namely bubble and jetting modes, are identified. The bubble mode occurs under low frequencies. In this mode, one mm-sized bubble is tightly attached to the electrode tip and oscillates with the applied voltage. With an increase in the frequency, it shows the jetting mode, in which many smaller bubbles are continuous formed and jetted away from the electrode surface. Multiple mechanisms that are potentially responsible to such a change in bubble dynamics have been proposed and the dominant mechanism is identified. From the Stark broadening of the hydrogen optical emission line, electron densities in both modes are estimated. It shows clearly that the driving frequency greatly influences the bubble dynamics, which in turn alters the plasma behavior. In the second part, the study of the erosion of a tungsten electrode immersed in saline solution under conditions suitable for bio-medical applications is presented. The electrode is immersed in 0.1 M saline solution and is positively or negatively biased using a DC power source up to 600 V. It is identified that when the electrode is positively biased, erosion by the surface electrolytic oxidation is the dominant mechanism with an applied voltage below 150 V. An increase in the applied voltage leads to the formation of the plasma and the damage by the plasma and the thermal effect becomes more prominent. The formation of the gas film at the electrode surface leads to the formation of the plasma and hinders the electrolytic erosion. In the negatively-biased electrode, no electrolytic oxidation is seen and the damage is mostly likely due to the plasma erosion and the thermal effect.