• The Bulletin of The Korean Astronomical Society
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• v.30 no.2
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• pp.52.2-52.2
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• 2005

• The Bulletin of The Korean Astronomical Society
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• v.30 no.2
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• pp.53.1-53.1
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• 2005

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

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

• Publications of The Korean Astronomical Society
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• v.20 no.1 s.24
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• pp.49-53
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• 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
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• v.35 no.1
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• pp.70.1-70.1
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• 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
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• v.35 no.1
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• pp.91.2-91.2
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• 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
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• v.35 no.2
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• pp.69.2-69.2
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• 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
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• v.40 no.9
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• pp.913-919
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• 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
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• 2009.10a
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• pp.33.3-33.3
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• 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.