• KASI NEWSLETTER
• /
• s.48
• /
• pp.1-8
• /
• 2005

신년사/ 천문연 영문 명칭 변경/ 한국우주전파관측망(KVN) 기공식/ "04년도 실적평가 및 "05년도 선정평가 공개발표회/ 박상대 이사장 UST, 특별강좌/ 박상대 이사장, 기초연 차세대 연구기반동 기공식 축사/ 조직개편/ 2005 역서, 천문력 발행/ 2004년 동계 교원 천문 연수 실시/ 한-일 VLBI 연구협력을 위한 공동 모임/ 과학기술인공제회 회원 가입신청/ 직원동정/ 학회동정/ 콜로키움/ 일본의 적외선 우주망원경 ASTRO-F/ 2004 천문학.우주과학 및 관련기술에 대한 한일 공동강의/ 레몬산천문대 원격관측 시연회 및 현판식/ 새로 발견된 5개의 소행성에 한국의 과학기술자 이름 헌정/ FIMS이용, 세계최초 돛자리초신성 전체 영상관측/ 크리미아천문대와 공동연구 협정 체결/ 천문 계산용 고성능 PC 클러스터 구축/ 중앙전파관리소와 우주전파기술 교류에 관한 협약 체결/ 세종대학교와 망원경 운영 협정서 체결/ 일본 우주과학연구본부와 상호협약서 체결/ 연구원 창립 30주년 기념식 거행

• Proceedings of the Korean Institute of Electrical and Electronic Material Engineers Conference
• /
• 2004.07b
• /
• pp.748-752
• /
• 2004

The Hydrogenated amorphous carbon (a-C:H) thin films are deposited to fabricate suppored layer on silicon substrate with a closed field unbalanced magnetron(CFUBM) sputtering system. This study focuses on the characteristic of Diamond like carbon (DLC) films and Pb(Zr,Ti)$O_3$ (PZT) films for membrane structure. The deposition rate and the surface roughness of DLC fims decrease with DC bias voltage. hardness is 26 GPa at -200 V. Interface of DLC/Si and Pt/DLC layers was excellent.

• KASI NEWSLETTER
• /
• s.42
• /
• pp.1-8
• /
• 2004

신년사/ 03/04년도 기관고유사업(및 일반사업) 연차실적 및 계획 평가 공개발표회 개최/ 제 4 차 동북아 서브 밀리미터파 수신기 기술 워크샵 개최/ 역서, 천문력 발간 및 배포/ 2004 동계 교원연수/ 신규직원 지역천문대 방문/ 학회동정/ 인사발령/ 정부포상/ 직원동정/ 콜로키움/ 태양활동 및 우주환경 연구/ 연구원 홈페이지 개편/ 김종수 박사, 이달의 과학기술자상 수상/ KAO Vision21 공청회 실시/ 2003 간섭계전파천문 여름학교 개최/ 원자외선 분광기(FIMS) 발사 성공/ 서귀포 별의 축제와 서울 화성축제 개최/ 2003년도 한국천문학회 추계 학술발표대회 개최/ 천문 계산용 리눅스 클러스터 구축 기념식 개최/ 현행역법의 제문제 워크샵 개최/ 대형망원경을 이용한 천체관측연구 워크샵 개최/ 2003 KVN 과학 워크샵 개최

• The Bulletin of The Korean Astronomical Society
• /
• v.34 no.2
• /
• pp.78.1-78.1
• /
• 2009

• Publications of The Korean Astronomical Society
• /
• v.20 no.1 s.24
• /
• pp.49-53
• /
• 2005

We are often faced with the task of having to estimate the amplitude of a source signal in the presence of a background. In the simplest case, the background can be taken as being flat, and of unknown magnitude B, and the source signal of interest assumed to be the amplitude A of a peak of known shape and position. We present a robust method to find the most probable values of A and B by applying the one-dimensional Newton-Raphson method. In the derivation of the formula, we adopted the Bayesian statistics and assmumed Poisson distribution so that the results could be applied to the analysis of very weak signals, as observed in FIMS (Far-ultraviolet IMaging Spectrogaph).

• The Bulletin of The Korean Astronomical Society
• /
• v.35 no.1
• /
• pp.70.1-70.1
• /
• 2010

We present the far-ultraviolet (FUV) emission line morphologies in the whole region of the supernova remnant G65.3+5.7 using the FIMS/SPEAR data. The morphologies of the C IV ${\lambda}{\lambda}1548$, 1551, $H2{\lambda}1608 $, He II ${\lambda}1640$, and O III] ${\lambda}{\lambda}1661$, 1666 lines appear to correlate clearly with the optical emission line images or the ROSAT X-ray (0.11-0.284 keV) image obtained in some of the previous studies. We found that a foreground dust cloud, resonant scattering, and incompleteness of radiative shocks have made the definite differences between the morphologies of the above FUV emission lines. We also present the FUV spectra and line intensities from a few sub-regions.

• The Bulletin of The Korean Astronomical Society
• /
• v.35 no.1
• /
• pp.91.2-91.2
• /
• 2010

We present far-ultraviolet (FUV) observations of comet C/2001 Q4 (NEAT) obtained with Far-ultraviolet Imaging Spectrograph (FIMS, also called SPEAR) around perihelion between 8 and 15 May 2004. Several important emission lines, including S I (1425, 1474 ${\AA}$), C I (1561, 1657 ${\AA}$), CO (1087.9, 1340-1680 ${\AA}$) were detected. Especially, the spectral features of CO are its electronic transitions belongings to the A-X, C-X systems. We also obtained radial profile of S I, C I, H I $Ly{\beta}$ with line fitting from central coma. The production rate of several spectral lines calculated from observed FUV photon flux. FUV spectral images of S I, C I, H I $Ly{\beta}$ emission lines were obtained.

• The Bulletin of The Korean Astronomical Society
• /
• v.35 no.2
• /
• pp.69.2-69.2
• /
• 2010

We investigate the southeastern region of the Vela supernova remnant (SNR) in the multi-wavelength domains. This region is quite interesting because it includes the bullet feature D/D´ and another SNR (the Vela Jr.). The C IV $\lambda\lambda1548$, 1551 emission-line morphologies obtained from the FIMS/SPEAR data show that there are several local peaks of C IV on the bullet D/D´ and the Vela Jr. SNR. This may provide clues to direct interaction between both SNRs. Also, we found that the southeastern side of the Vela is in direct contact with an H-alpha ring feature whose central source seems to be a B-type star, HD 76161. The C IV emission peaks along this contact boundary. We investigate this interacting region in detail.

• The Transactions of the Korean Institute of Electrical Engineers
• /
• v.40 no.9
• /
• pp.913-919
• /
• 1991

For an elementary study of the molecular electronic devices, in this study, N-alkylpyridinium(TCNQ) (1:1) and (1:2) complexed were synthesized. These complexes were verified by the UV, IR and the elemental analysis. Deposition of the LB films were verified by the reciprocal capacitance, UV absorbance and decresement area of Langmuir fims as functions of number of layers. The internal voltage of LB membrane devices fabricated with Y-type resides in 100-300mV. Finally, it seemed that self-polarization of LB membrance generates internal voltage.

• Bulletin of the Korean Space Science Society
• /
• 2009.10a
• /
• pp.33.3-33.3
• /
• 2009

We report the detection of the C IV $\lambda\lambda1548$, 1551 emission line in the region of the RCW 114 nebula using the FIMS/SPEAR data. The observed C IV line intensity indicates that RCW 114 is much closer to us than HD 156385, a Wolf-Rayet star that was thought to be associated with RCW 114 in some of the previous studies. We also found the existence of a small H I bubble centered on HD 156385, with a different LSR velocity range from that of the large H I bubble which was identified previously as related to RCW 114. These findings imply that the RCW 114 nebula is an old supernova remnant which is not associated with the Wolf-Rayet star, HD 156385. Additionally, the global morphology of the C IV and $H{\alpha}$ emissions shows that RCW 114 has evolved in a non-uniform interstellar medium.