• 천문학회보
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• 제41권1호
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• pp.76.2-76.2
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• 2016

We present near-infrared (0.8 - 1.8 microns) spectra of 63 bright (J_mag < 10) stars observed with Low Resolution Spectrometer (LRS) onboard the rocket-borne Cosmic Infrared Background Experiment (CIBER). Two Micron All Sky Survey (2MASS) photometry information is used to find cross-matched stars after reduction and extraction of the spectra. We identify the spectral types of observed stars by comparing with spectral templates from the Infrared Telescope Facility (IRTF) library. All the observed spectra are consistent with late F to M stellar spectral types, and we identify various infrared absorption lines. As our observations are performed above the Earth's atmosphere, our spectra are free from telluric contamination. Including HST/NICMOS and Cassini/VIMS, the spectral coverage has rarely been achieved in space, and the methods developed here can inform statistical studies with future low-resolution spectral measurements such as GAIA photometric and radial velocity spectrometer.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 2003년도 Proceedings of ACRS 2003 ISRS
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• pp.853-855
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• 2003

Microphytobenthos that supply nutrients to the intertidal ecosystem play an important part as a primary producer. If we estimate distribution and density of microphytobenthos, we can possibly calculate a volume of primary product in the tidal flat and its effect to the intertidal ecosystem. To estimate the portion of microphytobenthos, we used a linear spectral unmixing (LSU) method. LSU is a tool for inference the proportions of the pure components (or end-members) in a mixed pixel. The selection of end-members is critical to LSU. The end-members can be selected either from spectral libraries built from field surveys or from a remotely sensed image. We compared the two approaches of end-member selection, and the preliminary results showed end-members from from spectral library are as effective as those from image itself.

• 천문학논총
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• 제30권2호
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• pp.535-537
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• 2015

Interpreting ultraviolet-to-infrared (UV-to-IR) observations of galaxies in terms of constraints on physical parameters-such as stellar mass ($M_{\ast}$) and star formation rate (SFR)-requires spectral synthesis modelling. We investigate how increasing the level of sophistication of the standard simplifying assumptions of such models can improve estimates of galaxy physical parameters. To achieve this, we compile a sample of 1048 galaxies at redshifts 0.7 < z < 2.8 with accurate photometry at rest-frame UV to near-IR wavelengths from the 3D-HST Survey. We compare the spectral energy distributions of these galaxies with those from different model spectral libraries to derive estimates of the physical parameters. We find that spectral libraries including sophisticated descriptions of galaxy star formation histories (SFHs) and prescriptions for attenuation by dust and nebular emission provide a much better representation of the observations than 'classical' spectral libraries, in which galaxy SFHs are assumed to be exponentially declining functions of time, associated with a simple prescription for dust attenuation free of nebular emission. As a result, for the galaxies in our sample, $M_{\ast}$ derived using classical spectral libraries tends to be systematically overestimated and SFRs systematically underestimated relative to the values derived adopting a more realistic spectral library. We conclude that the sophisticated approach considered here is required to reliably interpret fundamental diagnostics of galaxy evolution.

• 천문학회보
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• 제41권2호
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• pp.43.3-43.3
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• 2016

We present a library of high-resolution (R~45,000) and high signal-to-noise ratio ($S/N{\geq}200$) near-infrared spectra of 147 standard stars. High quality spectra were obtained with Immersion GRating INfrared Spectrograph (IGRINS) covering the full range of H ($1.496-1.795{\mu}m$) and K ($2.080-2.460{\mu}m$) bands. The targets are mainly selected as MK standard stars which have well-defined spectral types and luminosity classes, and cover a wide range of effective temperatures and surface gravities. The spectra were corrected for telluric absorption lines and absolute flux calibrated using Two Micron All Sky Survey (2MASS) photometry. We find new spectral indices in H and K bands and provide their EWs. We describe empirical relations between the measured EWs and stellar atmosphere parameters such as effective temperature and surface gravity.

• Mass Spectrometry Letters
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• 제10권3호
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• pp.93-101
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• 2019

Algorithms and software for predicting tandem mass spectra have been developed in recent years. In this work, we explore how distinct in silico $MS^2$ spectra are predicted for isomers, i.e. compounds having the same formula and similar molecular structures, to differentiate between them. We used the CFM-ID 2.0/3.0 predictor with regard to (a) test compounds, whose experimental mass spectra had been randomly sampled from the MassBank of North America (MoNA) collection, and to (b) the most widespread isomers of test compounds searched in the PubChem database. In the first validation test, in silico mass spectra constitute a reference library, and library searches are performed for test experimental spectra of "unknowns". The searches led to the true positive rate (TPR) of ($46-48{\pm}10$)%. In the second test, in silico and experimental spectra were interchanged and this resulted in a TPR of ($58{\pm}10$)%. There were no significant differences between results obtained with different metrics of spectral similarity and predictor versions. In a comparison of test compounds vs. their isomers, a statistically significant correlation between mass spectral data and structural features was observed. The TPR values obtained should be regarded as reasonable results for predicting tandem mass spectra of related chemical structures.

• Nuclear Engineering and Technology
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• 제55권3호
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• pp.1084-1096
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• 2023

On-the-fly(OTF) generation of Spectral Superhomogenization(SSPH) factors is analyzed in the multigroup(MG) whole core calculation employing pin-wise continuous energy(CE) slowing-down solutions. The motivation for the work is to avoid the huge computing time required for the generation of a parametrized SSPH factor library(PSSL) which is used to resolve the angular dependency of MG resonance cross sections, and also to exploit the advantage of flexible choice of a MG structure by using CE slowing-down solutions. Two pin-wise CE slowing-down methods, the equivalent Dancoff cell method and the shadowing effect correction method, are evaluated with the OTF SSPH method. The effectiveness of the OTF SSPH method is examined for various simplified and realistic core problems with various MG structures. It is demonstrated that the computing time overhead of this method is negligible whereas the solution accuracy is considerably enhanced.

• 대한원격탐사학회지
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• 제32권5호
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• pp.423-434
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• 2016

적외선을 이용한 지표 온도 추정 및 변화 탐지를 위해서는 해당 파장대역의 각 센서에 따른 지표 복사율 추정 및 배경값에 대한 확보가 필요하다. 이 연구는 위성 영상으로부터 한반도에서의 중파장적외선 복사율 산출방법에 대한 제안 및 토지피복 종류별 대표 복사율을 산출하여 한반도 배경값을 제시할 수 있다. 중파장적외선 복사율을 추정하기 위해 Visible Infrared Imaging Radiometer Suite(VIIRS)의 $3.74{\mu}m$ 파장 대역 밴드4 영상에 Temperature Independent Spectral Indices(TISI) 방법을 적용하여 복사율을 계산하였으며, 또한 이와 비교하기 위해 Advanced Spaceborne Thermal Emission Reflection Radiometer(ASTER) spectral library로부터 토지피복에 따른 복사율도 계산하였다. 그 결과 활엽수립(0.958) 및 혼합림(0.955) 지역의 연평균 복사율이 가장 높았으며 농지(0.925) 및 자연식생(0.935) 지역보다는 약 2-3% 높게 나타났다. 도심지역의 경우 0.914로 가장 낮으며 연간 변화율이 1%인 다른 지역과는 달리 약 2%로 그 편차가 크다. ASTER spectral library와 비교한 결과 위성영상에서 추정한 중파장적외선 복사율은 동일한 토지 피복에 비해 약 2-3% 낮게 나타나는데, 이는 실제 지표면이 불균질한 점 외 기타 다양한 원인에 의한 것으로 추정된다. 이러한 연구 결과는 중파장적외선 영상을 이용하여 지표온도 추정 및 토지피복도의 계절 및 외부환경 변화에 의한 한반도 중파장적외선 복사율의 변화 특성을 이해하는데 기초 자료로 활용될 것이다.

• 대한전기학회논문지
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• 제34권3호
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• pp.107-114
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• 1985

This paper presents the iterative algorithm for obtaining the ME PSE(Maximum Entropy Power Spectral Estimation) of 2-dimensional signals. This problem involves a correction matching power spectral estimate that can be represented as the reciprocal of the spectral of 2-dimensional signals. This requires two matrix inversion every iterations. Thus, we compensate the matrix to be constantly positive definite with relaxational parameters. Using Row/Column decomposition Discrete Fourier Transform, we can decrease a calculation quantity. Using Lincoln data and white noise, this paper examines ME PSE algorithms. Finally, the results output at the graphic display device. The 2-dimensional data have the 3-dimensional axis components, and, this paper develops 3-dimensional graphic output algorithms using 2-dimensional DGL(Device Independent Graphic Library) which is prepared for HP-1000 F-series computer.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 2003년도 Proceedings of ACRS 2003 ISRS
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• pp.732-734
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• 2003

In the middle -resolution remote sensing, the Ground Sampled Distance(GSD) sensed and sampled by the detector is generally larger than the size of objects(or materials) of interest, in which case several objects are embedded in a single pixel and cannot be detected spatially. This study is intended to solve this problem of a hyperspectral data with high spectral resolution. We examined the detection algorithm, Linear Spectral Mixing Model, and also made a test on the Hyperion data. To find class Endmembers, we applied two methods, Spectral Library and Geometric Model, and compared them with each other.

• 대한원격탐사학회지
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• 제33권5_1호
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• pp.599-605
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• 2017

위성 영상의 정확한 구름 판별 여부는 이를 활용하여 생산되는 다른 산출물들의 정확도에 민감한 영향을 미치므로 매우 중요하다. 특히 해양에서 구름에 오염된 화소는 해수면 온도(Sea Surface Temperature: SST), 해색(ocean color), 클로로필-a(chlorophyll-a) 등 다양한 해양 기반산출물의 주된 오차 요인으로써 해양에서의 정확한 구름 탐지는 필수적이며 이는 해양 순환을 이해하는데 기여한다. 그러나 현재 Moderate Resolution Imaging Spectroradiometer (MODIS), Advanced Himawari Imager (AHI) 등 대부분 실시간 운영을 위한 알고리즘에서 사용되고 있는 고정 경계값 검사 방법은 태양-해양-센서의 상대적인 위치에 따라 변화하는 해양의 분광 특성을 고려하지 못하는 단점을 가지고 있다. 따라서 본 연구에서는 NOAA의 Himawari-8 구름 산출물을 이용하여 Himawari-8/AHI 반사도 채널에서의 태양 천정각(Solar Zenith Angle: SZA), 위성 천정각(Viewing Zenith Angle: VZA) 변화에 따른 청천 해양 표면 화소의 반사도를 수집하여 분광 라이브러리를 구축하였고 이를 이용하여 동적 경계값 방법인 Dynamic Time Warping (DTW)기법에 적용하여 구름탐지를 수행하였다. 본 연구의 구름탐지 결과를 Japan Meteorological Agency (JMA)의 구름 산출물과 정성적 비교한 결과 JMA 구름 산출물은 청천 화소를 불확실(unknown)으로 오탐지 및 과대탐지 하는 경향을 보였다. 이에 반해 본 연구에서는 태양 천정각이 고각인 지역에서 과대 탐지 및 오탐지되는 문제점을 개선하였다.