• Journal of Photoscience
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• 제4권3호
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• pp.121-125
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• 1997

The 77 K emission and excitation, and room-temperature visible spectra of cis[Cr(cyclam)Br$_2$]Br (cyclam=1,4,8,11-tetraazacyclotetradecane) are reported. The mid- and far-infrared spectra at room-temperature are also measured. The vibrational intervals of the electronic ground state are extracted from the far-infrared and emission spectra. The ten electronic bands due to spin-allowed and spin-forbidden transitions are assigned. It is found that nitrogen atoms of the cyclam ligand have strong $\sigma$-donor characters, but bromide ligand has weak $\sigma$- and $\pi$-donor properties toward chromium(III) ion. The zerophonon line in the excitation spectrum splits into two components by 172 cm$^{2-}$, and the large $^2E_g$ splitting can be reproduced by the ligand field theory.

• 천문학논총
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• 제30권2호
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• pp.159-161
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• 2015

We have carried out optical spectroscopic measurements of emission lines for a sample of Galactic planetary nebulae with Wolf-Rayet (WR) stars and weak emission-line stars (wels). The plasma diagnostics and elemental abundance analysis have been done using both collisionally excited lines (CELs) and optical recombination lines (ORLs). It was found that the abundance discrepancy factors ($ADF{\equiv}ORL/CEL$) are closely correlated with the difference between temperatures derived from forbidden lines and those from $He\;{\small{I}}$ recombination lines, implying the existence of H-deficient materials embedded in the nebula. The $H{\beta}$ surface brightness correlations suggest that they might be also related to the nebular evolution.

• 천문학논총
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• 제30권2호
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• pp.145-148
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• 2015

Young Galactic supernova remnants (SNRs) are where we can observe closely supernova (SN) ejecta and their interaction with the circumstellar/interstellar medium. They also provide an opportunity to explore the explosion and the final stage of the evolution of massive stars. Near-infrared (NIR) emission lines in SNRs mostly originate from shocked dense material. In shocked SN ejecta, forbidden lines from heavy ions are prominent, while in shocked circumstellar/interstellar medium, [Fe II] and $H_2$ lines are prominent. [Fe II] lines are strong in both media, and therefore [Fe II] line images provide a good starting point for the NIR study of SNRs. There are about twenty SNRs detected in [Fe II] lines, some of which have been studied in NIR spectroscopy. We will review the NIR [Fe II] observations of SNRs and introduce our recent NIR spectroscopic study of the young core-collapse SNR Cas A where we detected strong [P II] lines.

• Bulletin of the Korean Chemical Society
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• 제14권1호
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• pp.118-122
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• 1993

The 77 K luminescence and excitation spectra, room-temperature FT-infrared and visible absorption spectra of a newly prepared complex cis-[Cr(cyclam)(pn)]$(ClO_4)_3$, where cyclam and pn represent 1,4,8,11-tetraazacyclotetradecane and 1,2-propanediamine respectively, have been measured. Absorption maximum of the first spin-allowed transition in the electronic absorption spectra of cis-[Cr(cyclam)(pn)]$^{3+}$ and cis-[Cr(cyclam)(en)]$^{3+}$ appears at nearly the same position. The two spin-allowed and six spin-forbidden electronic transitions are assigned from the visible absorption and excitation spectra. It is also shown that the zero phonon line in the excitation spectrum splits into two components by 50 cm$^{-1}$.

• Bulletin of the Korean Chemical Society
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• 제20권1호
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• pp.81-84
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• 1999

The emission and excitation spectra of [Cr(NH3)5(imH)](ClO4)3·H2O (imH=imidazole) taken at 77 K are reported. The 298 K visible and far-infrared spectra are also measured. The vibrational intervals of the electronic ground state are extracted from the far-infrared and emission spectra. The ten electronic bands due to spin-allowed and spin-forbidden transitions are assigned. Using the observed transitions, a ligand field analysis has been performed to determine the bonding properties of coordinated imidazole in the title chromium(Ⅲ) complex. It is confirmed that nitrogen atom of the imidazole ligand has a medium it-acceptor property toward chromium(Ⅲ) ion. The zero-phonon line in the excitation spectrum splits into two components by 181 cm-1, and the large 2Eg splitting can be reproduced by the ligand field theory.

• 한국콘텐츠학회논문지
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• 제9권12호
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• pp.113-120
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• 2009

온라인 게임에서의 언어폭력 문제는 매우 심각하지만 그에 대한 효과적인 정책이나 기술적인 방법은 부족한 상황이다. 온라인 게임 서비스 업체에서는 금칙어 리스트를 작성하여 Swear Filter를 이용한 고정된 형식의 문자열 검색 방식을 통해 문제를 해결하려고 하고 있으나 사용자들은 다양한 방법으로 욕설을 조합 또는 변형시켜 기존의 필터링을 회피하고 있다. 특히 한글은 욕설의 변형이 매우 쉬운 특성을 가지고 있다. 본 논문에는 한글에 기초한 변형 욕설을 효율적으로 탐색하여 걸러내는 알고리즘을 제시한다. 이 알고리즘의 주된 특징은 변형 욕설의 표준형 변환과 자소단위의 반 전체 정렬(semi-global alignment), 이다. 실험 결과 저자들이 다양한 인터넷 게임 환경에서 직접 수집한 다종의 욕설 단어들에 대하여 약 90%의 우수한 필터링 성능을 보였다.

• 천문학회보
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• 제36권2호
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• pp.73.2-73.2
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• 2011

We present a new database of absorption and emission-line measurements based on the entire spectral atlas from the Sloan Digital Sky Survey (SDSS) 7th data release of galaxies within a redshift of 0.2. Our work makes use of the publicly available penalized pixel-fitting(pPXF) and gas and absorption line fitting (gandalf) IDL codes, aiming to improve the existing measurements for stellar kinematics, the strength of various absorption-line features, and the flux and width of the emissions from different species of ionized gas. Our fit to the stellar continuum uses both standard stellar population models and empirical templates obtained by combining a large number of stellar spectra in order to fit a subsample of high-quality SDSS spectra for quiescent galaxies. Furthermore, our fit to the nebular spectrum includes an exhaustive list of both recombination and forbidden lines. Foreground Galactic extinction is implicitly treated in our models, whereas reddening in the SDSS galaxies is included in the form of a simple dust screen component affecting the entire spectrum that is accompanied by a second reddening component affecting only the ionised gas emission. Most notable of our work is that, we provide quality of the fit to assess reliability of the measurements. The quality assessment can be highly effective for finding new classes of objects. For example, based on the quality assessment around the Ha and [NII] nebular lines, we found approximately 1% of the SDSS spectra which classified as "galaxies" by the SDSS pipeline are in fact type I Seyfert AGN.

• 한국지구과학회지
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• 제43권3호
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• pp.351-366
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• 2022

우리는 CFHT에 부착된 OASIS 분광기, MR 1 그리즘으로 관측한 방출선 중, H𝛽와 [O III] 5007 방출선을 분석하여, 제 2형 세이퍼트 은하 Mrk 1의 운동학적 특성을 파악하였다. [O III] 금지선의 가우시안 선 윤곽 분석을 통해 초과하는 청색 이동 성분의 방출 영역이 비대칭적으로 보이는데, (1) 은하 중심부 약 960 pc거리에서 플럭스는 최대를 보이고, (2) 은하 중심부에서 NS 방향으로 ~900 km s^-1인 큰 선폭 지역이 있음을 확인하였다. 두 원소의 분광 영상에서 보이는 시선 속도의 특징은 NE 방향에서 접근하는 가스의 흐름이, SW 방향으로 적색 이동, 즉 멀어지는 가스의 흐름이 나타나 반시계 방향 은하의 회전 경향성을 보여준다. 시선 속도 자료로부터 은하 중심은 우리를 향해 접근하는 먼지 가스가 가리고 있음을 파악하였다.

• 대한화학회지
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• 제39권7호
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• pp.501-507
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• 1995

cis-$[Cr(cyclam)Cl_2]Cl$의 전자 구조를 77K의 방출 및 들뜬 상태 분광법을 비롯하여, 실온의 적외선과 가시선 분광법을 이용하여 연구하였다. 스핀-허용 및 스핀-금지에 해당하는 10개의 순수 전자전이의 성분을 배정하였다. 들뜬 상태 스펙트럼에서 0-0 띠는 $139\;cm^{-1}$로 분리되었으며, 이러한 갈라짐을 현대 리간드장 이론으로 재현할 수 있었다. 리간드장 해석의 결과에 의하면 cyclam의 N 원자는 Cr(III) 이온에 강한 ${\sigma}$-주개로 작용하는 반면에 Cl 리간드는 약한 ${\sigma}-$ 및 ${\pi}-$주개의 성질이 있음을 확인할 수 있었다.

• 천문학논총
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• 제27권4호
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• pp.261-262
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• 2012

The aim of this research is to reveal the spatial distribution of the star formation activity of nearby galaxies by comparing CO molecular emission lines with the large area observation in far-infrared (FIR) lines. We report the imaging observations of NGC 253 by FIR forbidden lines via FIS-FTS and CO molecular lines from low to high excitation levels with ASTE, which are good tracers of star forming regions or photo-dissociation regions, especially spiral galaxies, in order to derive the information of the physical conditions of the ambient interstellar radiation fields. The combination of spatially resolved FIR and sub-mm data leads to the star formation efficiency within galaxy. The ratio between the FIR luminosity and molecular gas mass, $L_{FIR}/M_{H_2}$, is expected to be proportional to the number of stars formed in the galaxy per unit molecular gas mass and time. Moreover the FIR line ux shows current star formation activity directly. Furthermore these can be systematic and statistical data for star formation history and evolution of spiral galaxies.