• 천문학회보
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• 제43권1호
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• pp.43.2-44
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• 2018

One of the keys to interpreting the characteristics and evolution of interstellar medium in the Milky Way is to understand the distribution of hot gas ($10^5-10^6K$). Gases in this phase are difficult to observe because they are in low density and lack of easily observable tracers. Hot gases are observed mainly in the emission of the FUV ($912-1800{\AA}$), EUV ($80-912{\AA}$), and X-rays (T> $10^6K$) of which attenuation is very high. Of these, FUV emission lines originated from high-stage ions such as O VI and C IV can be the most effective tracers of hot gases. To determine the spatial distribution of O VI and C IV emissions, we have analyzed the spectra obtained from FIMS (Far-ultraviolet IMaging Spectrograph), which covers about 80 percent of the sky. The hot gas volume filling factor, which varies widely from 0.1 to 0.9 depending on the supernova explosion frequency and the evolution model, has been calculated from the O VI and C IV maps. The hot gas generation models has been verified from the global distribution of O VI and C IV emissions, and a new complementary model has been proposed in this study.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2011년도 한국우주과학회보 제20권1호
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• pp.20.1-20.1
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• 2011

We present the results of far-ultraviolet (FUV) observations of comet C/2001 Q4 (NEAT) obtained with Far-ultraviolet Imaging Spectrograph (FIMS) on board the Korean microsatellite STSAT-1, which operated at an altitude of 700 km in a sun-synchronous orbit. FIMS is a dual-channel imaging spectrograph (S channel 900-1150 ${\AA}$, L channel 1350-1750 ${\AA}$, ${\lambda}/{\Box}{\lambda}$ ~ 550) with large image fields of view (S: $4^{\circ}.0{\times}4'.6$, L: $7^{\circ}.5{\times}4'.3$, angular resolution 5'-10') optimized for the observation of diffuse emission of astrophysical radiation. Comet C/2001 Q4 (NEAT) was observed with a scanning survey mode when it was located around the perihelion between 8 and 15 May 2004. Several important emission lines were detected including S I (1425, 1474 ${\AA}$), C I (1561, 1657 ${\AA}$) and several emission lines of CO $A1{\cap}-X1{\sum}+$ system in the L channel. We estimated QCO = ($2.58\;{\pm}\;0.64)\;{\times}\;1028$ s-1 from the production rate of CO 1510 ${\AA}$. We obtained L-channel image which have map size of $5^{\circ}{\times}5^{\circ}$. The image was constructed for the wavelength band of L-channel (1350-1750 ${\AA}$).We also obtained radial profile of S I, C I, CO with line fitting from central coma.

• Applied Biological Chemistry
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• 제51권4호
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• pp.276-280
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• 2008

식품 allergen 저감화 수단으로 자외선 조사의 타당성을 검토하고 자외선조사가 식품 단백질의 분자적 성질에 미치는 영향을 조사하고자 ovalbumin 용액에 자외선을 조사한 후 단백질의 분자량 분포와 2차구조 및 3차구조의 변화를 조사하였다. SDS-PAGE와 Gel permeation chromatography 결과 ovalbumin은 자외선 조사에 의하여 단백질이 분해되고 조사시간이 증가할수록 펩티드가 중합하는 형태를 나타냈다. Circular dichroism 연구는 자외선 조사에 의하여 ${\alpha}$-helix 구조가 감소하고 조사시간이 증가할 경우 compact denatured ovalbumin의 구조를 나타내는 2차구조의 변화를 나타냈다. 자외선 조사된 ovalbumin의 형광스펙트럼은 조사시간이 증가할수록 단백질의 maximum emission intensity가 감소하는 3차구조의 변화를 나타냈다. 결과적으로 자외선 조사는 ovalbumin의 분자적 성질을 변화시키며 allergen의 항원성을 변화시키는 수단으로 이용가능성을 시사한다.

• Current Optics and Photonics
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• 제5권1호
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• pp.1-7
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• 2021

For higher sensitivity in ultraviolet (UV) and even vacuum ultraviolet (VUV) detection of silicon-based sensors, a sandwich-structured film sensor based on Ag Localized Surface Plasmon Resonance (LSPR) was designed and fabricated. This film sensor was composed of a Ag nanoparticles (NPs) layer, SiO2 buffer and fluorescence layer by physical vapour deposition and thermal annealing. By tuning the annealing temperature and adding the SiO2 layer, the resonance absorption wavelength of Ag NPs matched with the emission wavelength of the fluorescence layer. Due to the strong plasmon resonance coupling and electromagnetic field formed on the surface of Ag NPs, the radiative recombination rate of the luminescent materials and the number of fluorescent molecules in the excited state increased. Therefore, the fluorescent emission intensity of the sandwich-structured film sensor was 1.10-1.58 times at 120-200 nm and 2.17-2.93 times at 240-360 nm that of the single-layer film sensor. A feasible method is provided for improving the detection performance of UV and VUV detectors.

• 한국염색가공학회지
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• 제23권3호
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• pp.187-194
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• 2011

This study used Jeju scoria to dye cotton fabric and measured its dyeability, colorfastness, antibacterial activity, deodorization efficiency, ultraviolet protection, and far-infrared emission. The cotton fabric was colored to yellowish red and optimal dyeing can be achieved at a temperature of $80^{\circ}C$ for a dyeing time of 120 minutes with a colorant concentration of 25%(o.w.b). The colorfastness to light, rubbing, perspiration, and washing was 8, 5, 5, and 4~5 ratings respectively, where the wash colorfastness remained after 15 wash cycles. The cotton fabric dyed with Jeju scoria demonstrated excellent antimicrobial activity to Staphylococcus aureus and high deodorization efficiency. Ultraviolet protection factor was as high as 50+. The Jeju scoria can be used as a new colorant for the natural dyeing of silk.

• 천문학회보
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• 제36권2호
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• pp.110.2-110.2
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• 2011

Nishikida et al. (2006) presented the first far-ultraviolet (FUV) em${\lambda}$ission-line images of the Vela supernova remnant (SNR) obtained with FIMS/SPEAR instrument. Those include C III ${\lambda}$977, O VI ${\lambda}{\lambda}$1032, 1038, Si IV+O IV] ${\lambda}{\lambda}$1393, 1403 (un-resolved), C IV ${\lambda}{\lambda}$1548, 1551 emission-line images. As a following work, we re-constructed these emission-line images using the new-version processed FIMS/SPEAR data. Additionally, we made N IV] ${\lambda}$1486, He II ${\lambda}$1640.5, O III] ${\lambda}{\lambda}$1661, 1666 emission-line images. The new-version images cover the whole region of the Vela SNR and show more resolved features than the old-version. We compare these FUV emission-line images with other wavelength (X-ray, optical, etc.) images obtained in previous studies.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2004년도 한국우주과학회보 제13권1호
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• pp.99-99
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• 2004

We detected and analyzed molecular hydrogen fluorescence in the Taurus Cloud using the Far-ultraviolet Imaging Spectrograph (FIMS) on the STSAT-1 which was launched at SeP. 27 2003. FIMS is optimized for observing diffuse emission lines in the interstellar medium in the wavelength bands of 900-l150 and 1300-1700 angstrom. The Taurus region is a local molecular cloud which is good for studying molecular hydrogen fluorescence emissions. (omitted)

• 천문학회보
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• 제35권1호
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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.

• 한국세라믹학회지
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• 제38권9호
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• pp.817-821
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• 2001

새로운 형광체로 역스피넬 구조를 갖는 $Mg_{2-x}MN_xSnO_4$ 조성을 선정하여 고상반응에 의하여 제조하였다. $Mg_2SnO_4:Mn$의 광발광 특성이 147nm 파장의 진공 자외선 여기하에 측정되었다. Mn의 첨가에 의하여 $Mg_2SnO_4$ 형광체는 500nm 파장에 발광 중심을 가지며 매우 높은 발광강도를 나타내었다. 이것은 스피넬 구조의 산소 사면체 배위에 위치하는 Mg 자리를 치환하여 들어가는 $Mn^{2+}$ 이온의 $^4T_1$ 상태로부터 $^6A_1$ 상태로의 에너지 전이에 의한 발광으로 해석되었다. 진공 자외선 여기하에 최대의 발광강도를 나타내는 Mn 활성제의 농도는 0.25mol%이었고, 잔광시간은 10ms 이하인 것으로 조사되었다.

• 천문학회보
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• 제37권2호
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• pp.99.1-99.1
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• 2012

We report the results of our analysis of far ultraviolet (FUV) observations made for the broad region around the ${\alpha}$ Vir (Spica) including the interaction zone of the Loop I and the Local Bubble. We employed the datasets of the GALEX and the FIMS, which made observations at similar FUV wavelengths. First, we noted that the GALEX image was enhanced in the southern region where the interaction zone exists. We attribute this enhanced FUV emission to dust scattering of the stellar photons, mostly from the background field stars with small contributions from the central star Spica. While the region is optically thin in general, the FUV intensity did not correlate well with the dust extinction level, indicating that the local radiation field has significant fluctuations. On the other hand, the GALEX FUV intensity well with the $H{\alpha}$ intensity as well as the dust extinction level in the northern part. In fact, the neutral hydrogen column density correlated very well with the dust extinction level throughout the whole region in consideration. The relationship between the neutral hydrogen column density and the color excess was estimated to be ${\sim}7{\times}10^{21}atoms\;cm^{-2}$, which is a little higher than the previous observations made for a diffuse interstellar medium. The spectral analyses of the FIMS observations showed the enhanced C IV emission throughout the whole region, indicating that the C IV emission arises by the interaction of the hot gases with the shell boundaries. A simple model showed that a large portion of the C IV emission comes from the Loop I side of the interaction zone, compared to the Local Bubble side. The FIMS spectrum also showed indications of the molecular hydrogen fluorescence lines for the interaction zone.