• 천문학회보
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• 제44권1호
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• pp.67.4-67.4
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• 2019

We present preliminary results of our long-term (2009-2017) observing campaign using the NASA IRTF at Mauna Kea, to obtain $2-5{\mu}m$ spectroscopy of ~200 red point sources in the line of sight to the Galactic center. Point sources in our sample were selected from the mid-infrared images of the Spitzer Space telescope, and include candidate massive young stellar objects, which have previously been identified from our Spitzer/IRS spectroscopy. We show high foreground extinction of these sources from deep $3.1{\mu}m$ H2O ice and aliphatic hydrocarbon absorption features, suggesting that they are likely located in the central 300 pc region of the Galactic center. While many sources reveal photospheric $2.3{\mu}m$ gas CO absorption, few of them clearly indicate $3.54{\mu}m$ CH3OH ice absorption, possibly indicating a large dust column density intrinsic to a massive young stellar object.

• Current Optics and Photonics
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• 제7권6호
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• pp.761-765
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• 2023

We analyzed the absorption spectra of acetone in the 3.37 ㎛ mid-infrared range using the off-axis integrated cavity output spectroscopy technique to develop a real-time, in-line breath analysis device. The linear relationship between acetone concentration and absorption increase was confirmed as 0.32%/ppm, indicating that the developed device allows for a quantitative analysis of acetone concentration in exhaled breath. To further confirm the feasibility of using our device for breath analysis, we measured the acetone concentration of human breath samples at the sub-ppm level.

• 대한전기학회:학술대회논문집
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• 대한전기학회 1989년도 하계종합학술대회 논문집
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• pp.667-671
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• 1989

The CO laser is one of powerful light source for laser magnetic resonance spectroscopy in the mid-infrared region of the spectrum because of its wideband operational characteristics. In this work, a liquid nitrogen cooled cw CO laser is developed to allow broad-band operation from 5 to 8 ${\mu}m$. The design details will be presented.

• 한국광학회:학술대회논문집
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• 한국광학회 2003년도 제14회 정기총회 및 03년 동계학술발표회
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• pp.204-205
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• 2003

미량기체의 흡수스펙트럼을 높은 감도로 측정하는 공동 광자감쇠 분광법(cavity ringdown spectroscopy； CRDS)을 나노초 레이저 펄스의 차주파수 생성(difference-frequency generation； DFG)을 광원으로 이용하여 파장 3 ~ 4 $\mu\textrm{m}$ 영역에서 구현하였다. CRDS는 고반사율 거울로 이루어진 광학적 공동에 단일 파장의 빛을 가두었다가 그 에너지의 시간적 감소율을 측정하여 공동 속 기체의 흡수율을 알아내는 방법이다. (중략)

• 분석과학
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• 제32권1호
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• pp.7-16
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• 2019

본 연구에서는 닥나무 인피섬유와 이를 이용하여 제조한 한지의 FT-NIR및 FT-MIR 스펙트럼 데이터를 각각PLS-DA에 적용하여 닥나무 인피섬유 및 한지의 원산지 판별 모델을 개발하고자 하였다. 본 연구를 위하여 서로 다른 원산지의 국내산 닥나무 인피섬유 10점을 채취하여 한지로 제조하였다. 상기시료의 FT-NIR 및 FT-IR 스펙트럼 데이터는 데이터 전처리 과정을 거쳐 PLS-DA를 수행하였다. 모델링 결과, 닥나무 인피섬유와 한지의 NIR 스펙트럼 데이터가 판별모델의 교차 검증결과 및 성능평가(정확도, 민감도, 특이도)에서 모두 100 %로 MIR 스펙트럼 데이터보다 우수한 판별 성능을 나타냈다. 또한 지역별로 4 개의 그룹을 형성하는 것을 확인 할 수 있었으며, 닥나무 인피섬유와 한지의 원산지 판별 모델 간 score 형태가 유사하게 나타내는 것을 확인하였다.

• 한국임상수의학회지
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• 제15권2호
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• pp.472-475
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• 1998

A female Green iguana (Iguana iguana) was brought to the small animal clinic in Hannover Veterinary school because of anorexia and convulsion. Two months ago, the owner bought two iguanas, one female and one male and had to take a female to the one of local small animal clinic because she, born in 19931 didn't eat well and showed the tremor of the legs. The veterinarian suspected it to have a calcium deficiency and gave an injection of calcium and vitamin D3. But still during the last two months, the female iguana did only eat some lettuce while the other male ate lettuce, fruits and commercial cat-food ($Whiskas^{\circledR}$, Effem, Verden). It was not possible to evaluate the rations of these different "food-components". They are kept in the terrarium with water container. By palpation of the abdomen, hard thing like stone was palpated in the mid-region. The blood test wasn't carried out because of the difficulties of getting blood and because of her bad condition. It was firmly diagnosed as cystic calculus through radiography. Since the animal is in shock state already, the prognosis after surgery was bad. It was assumed to be too late to expect its surviving with the surgery carried out or without it. Cystotomy was performed in the cranial ventral paramedian incision in order to preserve the large ventral abdominal vein in the linen alba region. After two stay sutures ("holding suture" ) with 5-0 polyglactin 910 ($Vicryl^{\circledR}, Ethicon$) on the bladder, cystotomy was carried out and the stone inside was removed. Then, the bladder was closed in one-layer sutures. The abdomen was closed in simple interrupted suture with same material after the instillation of 10 ml saline solution into the abdominal cavity. The cystic calculus was in a size of $5.8{\times} 5.O{\times} 3.5 cm$. The analysis of the stone was carried out in two ways which are the infrared spectroscopy of the stone and quick analysis by $Merckognost^{\circledR}$(Diagnostica Merck, Merck). In the result of the infrared spectroscopy, the stone wee composed of 10% ammonium urate and 90% dihydrated uric acid. This iguana wasn't able to survive.n't able to survive.

• Journal of Animal Science and Technology
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• 제64권3호
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• pp.531-538
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• 2022

In Italy, buffalo mozzarella is a largely sold and consumed dairy product. The fraudulent adulteration of buffalo milk with cheaper and more available milk of other species is very frequent. In the present study, Fourier transform infrared spectroscopy (FTIR), in combination with multivariate analysis by partial least square (PLS) regression, was applied to quantitatively detect the adulteration of buffalo milk with cow milk by using a fully automatic equipment dedicated to the routine analysis of the milk composition. To enhance the heterogeneity, cow and buffalo bulk milk was collected for a period of over three years from different dairy farms. A total of 119 samples were used for the analysis to generate 17 different concentrations of buffalo-cow milk mixtures. This procedure was used to enhance variability and to properly randomize the trials. The obtained calibration model showed an R² ≥ 0.99 (R² cal. = 0.99861; root mean square error of cross-validation [RMSEC] = 2.04; R² val. = 0.99803; root mean square error of prediction [RMSEP] = 2.84; root mean square error of cross-validation [RMSECV] = 2.44) suggesting that this method could be successfully applied in the routine analysis of buffalo milk composition, providing rapid screening for possible adulteration with cow's milk at no additional cost.

• 천문학회보
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• 제38권1호
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• pp.49.1-49.1
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• 2013

We have been carrying out near-infrared (NIR) spectroscopy as well as [Fe II] narrow band imaging observations of Cassiopeia A supernova remnant (SNR). In this presentation, we describe the spectral classification of the iron knots around the SNR. From eight long-slit spectroscopic observations for the iron-bright shell, we identified a total of 61 iron knots making use of a clump-finding algorithm, and performed principal component analysis in an attempt to spectrally classify the iron knots. Three major components have emerged from the analysis; (1) Iron-rich, (2) Helium-rich, and (3) Sulfur-rich groups. The Helium-rich knots have low radial velocities (${\mid}v_r{\mid}$ < 100 km/s) and radiate strong He I and [Fe II] lines, that match well with Quasi-Stationary Flocculi (QSFs) of circumstellar medium, while the Sulfur-rich knots show strong lines of oxygen burning materials with large radial velocity up to +2000 km/s, which imply that they are supernova ejecta (i.e. Fast-Moving Knots). The Iron-rich knots have intermediate characteristics; large velocity with QSF-like spectra. We suggest that the Iron-rich knots are missing "pure" iron materials ejected from the inner most region of the progenitor and now encountering the reverse shock.

• 천문학회보
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• 제41권2호
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• pp.63.3-63.3
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• 2016

We present the two-dimensional distribution of stellar populations in five E+A galaxies from GMOS-N/IFU spectroscopy (GN-2015B-Q-15). Numerical simulations demonstrated that E+A galaxies formed by major mergers contain young stellar populations (e.g. A-type stars) that are centrally-concentrated within scales of 1 kpc. However, several IFU studies reported that A-type stars are widely distributed on ${\gg}$ 1kpc scales. In contrast, Pracy et al. (2013) found a central concentration of A-stars and strong negative Balmer absorption line gradients within 1 kpc scales for local (z < 0.03) E+A galaxies. They claimed that previous studies failed to detect the central concentration because the E+A galaxy samples in previous studies are too far (z ~ 0.1) to resolve the central kpc scales. To verify Pracy et al.'s argument and the expectation from simulations, we selected five E+A galaxies at 0.03 < z < 0.05. Furthermore, we selected the targets in the mid-infrared green valley (Lee et al. 2015). Thanks to good seeing (${\sim}0.4^{{\prime}{\prime}}{\simeq}0.33kpc$) of our observation, we are able to resolve the central 1 kpc region of our targets. We found that all five galaxies have negative Balmer line gradients, but that three galaxies have flatter gradients than those reported in Pracy et al. We discuss the results in relation with galaxy merger history.

• 한국근적외분광분석학회:학술대회논문집
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• 한국근적외분광분석학회 2001년도 NIR-2001
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• pp.1041-1041
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• 2001

Removal of variability in spectra data before the application of chemometric modeling will generally result in simpler (and presumably more robust) models. Particularly for sparsely sampled data, such as typically encountered in diode array instruments, the use of Savitzky-Golay (S-G) derivatives offers an effective method to remove effects of shifting baselines and sloping or curving apparent baselines often observed with scattering samples. The application of these convolution functions is equivalent to fitting a selected polynomial to a number of points in the spectrum, usually 5 to 25 points. The value of the polynomial evaluated at its mid-point, or its derivative, is taken as the (smoothed) spectrum or its derivative at the mid-point of the wavelength window. The process is continued for successive windows along the spectrum. The original paper, published in 1964 [1] presented these convolution functions as integers to be used as multipliers for the spectral values at equal intervals in the window, with a normalization integer to divide the sum of the products, to determine the result for each point. Steinier et al. [2] published corrections to errors in the original presentation [1], and a vector formulation for obtaining the coefficients. The actual selection of the degree of polynomial and number of points in the window determines whether closely situated bands and shoulders are resolved in the derivatives. Furthermore, the actual noise reduction in the derivatives may be estimated from the square root of the sums of the coefficients, divided by the NORM value. A simple technique to evaluate the actual convolution factors employed in the calculation by the software will be presented. It has been found that some software packages do not properly account for the sampling interval of the spectral data (Equation Ⅶ in [1]). While this is not a problem in the construction and implementation of chemometric models, it may be noticed in comparing models at differing spectral resolutions. Also, the effects on parameters of PLS models of choosing various polynomials and numbers of points in the window will be presented.