• 한국물환경학회지
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• 제27권5호
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• pp.625-633
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• 2011

A long-term water quality monitoring in the Han River Basin reveals a consistent increasing trend for the concentration of refractory organic matter (R-OM) in major monitoring sites of the watershed. Because the determination of R-OM concentrations typically requires a long time of microbial incubation, it is essential to present the estimation indices for R-OM for an efficient watershed management. In this study, a number of surface water samples were classified into three groups, each of which were collected from Lake Paldang, rivers at rain and non-rain events, respectively. The corresponding R-OM concentrations were correlated with biochemical oxygen demand (BOD), chemical oxygen demand (COD), and total organic carbon (TOC) concentrations as well as ultraviolet and fluorescence intensities of the filtered samples. Among the traditional organic matter parameters, TOC exhibited the highest correlation coefficient with the R-OM concentrations regardless of the types of the sample groups. The equations for conversing TOC into R-OM concentrations were finally suggested as $0.43{\times}TOC+1.12$, $0.44{\times}TOC+0.61$, $0.24{\times}TOC+1.28$ for river samples at rain and non-rain events, and lake samples, respectively. TOC-BOD(C), the values of the TOC concentrations subtracted by carbon-converted BOD concentrations, was a good index for estimating the absolute concentrations of R-OM. UV absorbance at 254 nm was well correlated with R-OM concentrations of river samples while fluorescence intensities at 350 nm showed an excellent relationship with R-OM concentration of the lake samples. Our results suggests that simple spectroscopic parameters could be applied for in-situ monitoring tool techniques in watersheds.

• 천문학회보
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• 제40권1호
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• pp.72.3-72.3
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• 2015

We present the mid-infrared (MIR) luminosity function (LF) of local (z < 0.3) star forming (SF) galaxies based on the AKARI's NEP-Wide Survey data. We utilized a combination of the NEP-Wide point source catalogue containing a large number (114,000) of infrared (IR) sources distributed over the wide (5.4 sq. deg) field and spectroscopic redshift (z) data for 1790 selected targets obtained by optical follow-up surveys with MMT/Hectospec and WIYN/Hydra. The AKARI's continuous $2{\sim}24{\mu}m$ wavelength coverage and the spectroscopic redshifts for sample galaxies enable us to derive accurate spectral energy distributions (SEDs) in the mid-infrared. We carried out SED-fit analysis and employed 1/Vmax method to derive the mid-IR (e.g., $8{\mu}m$, $12{\mu}m$, and $15{\mu}m$ rest-frame) luminosity functions. Our results for local galaxies from the NEP region generally consistent with various previous works for other fields over wide luminosity ranges. The comparison with the results of the NEP-Deep data implies the luminosity evolution from higher redshifts towards the present epoch. We attempted to fit our derived LFs to the double power-laws and present the resulting power indices. We also examined the correlation between mid-IR luminosity and total IR luminosity.

• 한국광학회지
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• 제8권4호
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• pp.277-282
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• 1997

광학소자나 전자소자의 코팅에 많이 이용되고 있는 Diamond-like Carbon(DLC) 박막의 복소굴절율을 광학적 방법을 사용하여 구하였다. PECVD(Plasma enhanced CVD)법에 의해 Si(100)기판과 비정질실리카 기판위에 각각 성장시킨 DLC 박막을 분광타원해석기와 분광광도계를 이용하여 타원해석 스펙트럼과 광투과율 스펙트럼을 측정하고, Sellmeier 분산관계식과 양자역학적 진동자 모델을 이용하여 분석하였다. 비정질실리카 위에 증착된 DLC 박막의 광투과영역에서 분광타원해석분석으로 굴절률 및 박막의 유효두께를 구하고 광흡수영역에서 투과스펙트럼을 역방계산하여 소광계수를 구한 뒤, 이 소광계수 스펙트럼에 최적 근사하는 양자역학적 분산식의 계수들을 회귀분석법으로 결정하여 복소굴절율을 구하였다. 그리고 모델링방법을 타워해석 스펙트럼에 적용하여 Si기판과 비정질이산화규소 기판위에 증착된 DLC 박막의 조밀도, 표면거칠기 등 박막상수를 박막의 성장조건에 따라 분석하였다.

• 천문학논총
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• 제30권2호
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• pp.255-259
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• 2015

Recent narrow-band Ca photometry discovered two distinct red giant branch (RGB) populations in some massive globular clusters (GCs) including M22, NGC 1851, and NGC 288. In order to investigate the differences in light/heavy elements abundances between the two subpopulations, we have performed low-resolution spectroscopy for stars on the two RGBs in these GCs. We find a significant difference (more than $4{\sigma}$) in calcium abundance from the spectroscopic HK' index for both M22 and NGC 1851. We also find a more than $8{\sigma}$ difference in CN band strength between the Ca-strong and Ca-weak subpopulations. For NGC 288, however, we detect the presence of a large difference only in the CN strength. The calcium abundances of the two subpopulations in this GC are identical within errors. We also find interesting differences in CN-CH relations among these GCs. While CN and CH indices are correlated in M22, they show an anti-correlation in NGC 288. However, NGC 1851 shows no difference in CH between two groups of stars having different CN strengths. The CN bimodality in these GCs could be explained by pollution from intermediate-mass asymptotic giant branch stars and/or fast-rotating massive stars. For the presence or absence of calcium bimodality and the differences in CN-CH relations, we suggest these would be best explained by how strongly type II supernovae enrichment has contributed to the chemical evolutions of these GCs.

• 천문학회보
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• 제42권1호
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• pp.42.2-42.2
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• 2017

We performed low-resolution spectroscopy for the red giant stars in the Galactic globular cluster (GC) NGC 5286, which is known to show intrinsic heavy element variations. We found that these stars are clearly divided into two subpopulations by CN index. These two subpopulations also show significant differences in the HK'and CH indices, where the CN-strong stars are more enhanced in both indices. From the comparison with high-resolution spectroscopic data of Marino et al. (2015), we found that the CN- and HK'-strong stars are also increased in the abundances of s-process elements and Fe. It appears that, therefore, these stars are later generation stars probably affected by supernova enrichment. In addition, NGC 5286 shows the CN-CH positive correlation among the whole sample, which is only discovered in the GCs with heavy element variations such as M22 and NGC 6273. Therefore, these results strengthen our previous suggestion that the CN-CH positive correlation may be associated with the heavy element variations in the GCs.

• 천문학논총
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• 제30권2호
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• pp.487-488
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• 2015

In type Ia supernovae (SNe Ia) cosmology, a well-established correlation exists between the mass of host galaxies and the Hubble residual (HR) of SNe Ia. In order to investigate the origin of this correlation, we used low-resolution spectroscopic data of early-type host galaxies obtained from our YOnsei Nearby Supernovae Evolution Investigation (YONSEI) project. We measured velocity dispersions and Lick/IDS absorption line indices from these fully calibrated spectra. These indices were used to estimate the luminosity-weighted mean age, metallicity and mass of host galaxies. We found a tight correlation between host mass and population age, which is consistent with the "downsizing" trend in early-type galaxies. This suggests that the well-established correlation between HR and host mass is most likely due to the difference in population age. More observations, which are in progress, are required to understand the impact of luminosity evolution on SNe Ia cosmology.

• 한국표면공학회지
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• 제29권5호
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• pp.532-539
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• 1996

Diamond-like carbon (DLC) films were deposited on silicon substrates by the plasma decomposition of hydrocarbons under various conditions, and studied by the spectroscopic ellipsometry (SE). We used the effective medium approximation with the dispersion model developed by Forouhi and Bloomer to determine simultaneously both the structure and the optical constants of the DLC films from their ellipsometric spectra. Especially, we investigated the variation of the multilayer structure including the interface layer, of the refractive indices, and of the extinction coefficients as the deposition conditions were varied; substrate pretreatment procedure, hydrocarbon precursors, and the substrate bias voltage were varied.

• Journal of Korean Vacuum Science & Technology
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• 제3권2호
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• pp.112-115
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• 1999

The real ($\varepsilon$1) and imaginary ($\varepsilon$2) parts of the dielectric function of ZnS have been measured by spectroscopic ellipsometry (SE) in the 3.7-6.0 eV photon-energy range at room temperature. The obtained dielectric function spectra reveal distinct structures at energies E0/(E0+$\Delta$0) and E1 critical points. The spectrum after chemical treatment to remove surface oxide overlayer showed that these data seem to be the best representation of the dielectric function of ZnS, having the largest $\varepsilon$2 value at E1 peak region reported so far by SE. Dielectric-related optical constants of ZnS, such as the complex refractive indices (n+n=ik), absorption coefficient, and reflectance, are also presented.

• 대한환경공학회지
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• 제30권9호
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• pp.893-899
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• 2008

본 연구에서는 낙엽과 토양에서 추출한 용존 자연유기물질(DOM)을 대상으로 생분해 과정 중 변화하는 분광특성과 pyrene 결합 반응성을 조사하였다. 유기물질 특성 변화 분석을 위해 용존 유기탄소(DOC), 용존 자연유기물질 내 방향족 탄소성분을 나타내는 고유흡광도(Specific UV absorbance: SUVA), synchronous 형광 스펙트럼과 유기탄소결합계수(pyrene organic carbon-normalized binding coefficient: K$_{oc}$) 분석을 실시하였다. 3주간의 배양기간 동안 낙엽 추출 DOM과 토양 DOM의 DOC는 각각 61%, 51% 감소하였다. 배양 전과 후의 분광특성을 비교해 보면 단백질/아미노산 계 형광특징(PLF)은 점차 감소된 반면 SUVA, 펄빅산계 형광 특징(FLF)과 휴믹산 계 형광 특징(HLF)은 점차 증가하였다. 이러한 자연유기물질의 분광특성 변화는 생분해 과정을 통해 휴믹화가 진행되며 자연유기물질 내 비방향족 생분해성 탄소성분이 단단한 구조의 방향족 탄소구조로 변화됨을 시사한다. SUVA 값과 유기오염물질과의 결합정도를 나타내는 K$_{oc}$ 값 사이에서는 시료의 종류와 상관없이 1차 상관관계(r = 0.97)를 보여 주어 생분해가 진행되는 동안 방향족 탄소구조 분포가 자연유기물질의 소수성 오염물질과의 결합 정도에 큰 영향을 미침을 보여주었다. 또한 형광특징 중 FLF와 HLF가 K$_{oc}$ 값과 높은 상관관계를 보였으며 자연유기물질의 기원에 따라 다른 상관관계식을 보여주었다. 본 연구를 통해 생분해가 진행되는 동안 자연유기물질 성분변화 및 소수성 유기오염물질의 거동 예측에 자연유기물질의 분광특성이 좋은 모니터링 지표로 사용될 수 있음을 보여 주었다.

• 천문학회보
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• 제37권1호
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• pp.31.2-31.2
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• 2012

We present the Yonsei Evolutionary Population Synthesis (YEPS) models for spectroscopic and photometric evolutions of simple and composite stellar populations. The models are based on the most up-to-date Yonsei-Yale stellar evolutionary tracks and BaSel 3.1 flux libraries, and provide integrated spectroscopic quantities of Lick/IDS system including high-order Balmer absorption-lines. Special care has been taken to incorporate the systematic variation of horizontal branch (HB) morphology as functions of metallicity, age, alpha-element mixture, and helium abundance of simple stellar populations. Our models for normal-helium stellar populations indicate that the realistic modeling of HB and alpha-element brings about 5 Gyr and 0.1 dex differences in age and metallicity estimations, respectively, compared to those without these effects. The HB effect does not depend on the specific choice of stellar libraries and alpha-element enhancements, and this effect is non-negligible even in the metal sensitive absorption indices, such as Mg2 and Mg b. Comparison of the models to observations reveals that the HB and alpha-element effects are critical in understanding otherwise inexplicable phenomena found in globular cluster systems in the Milky Way and nearby galaxies, including the observed bimodality of the line strengths of globular clusters in massive galaxies. In addition, we found that helium-enhanced stellar populations, which are the major sources of extreme HB stars, bring about increased FUV, NUV fluxes, and thus the model colors of those filters become extremely blue. Age dating based on the YEPS model with normal-helium stellar populations reveals that the evidence for 'downsizing' of elliptical galaxies is found not only in the local field but also in Coma cluster, and that the mean age of elliptical galaxies in Coma cluster is about 1.4 Gyr younger than the mean age of those in the local field. We also find that our models with helium-enhanced subpopulations can naturally reproduce the strong UV-upturns observed in giant elliptical galaxies assuming an age similar to that of old GCs in the Milky Way.