• Bulletin of the Korean Chemical Society
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• 제12권2호
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• pp.228-238
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• 1991

Generalized multichannel quantum defect theory [C. H. Greene et al. Phys. Rev., A26, 2441 (1982)] is implemented to the vibrational predissociation of triatomic van der Waals molecules. As this is the first one of such an application, the dependences of the quantum defect parameters on energy and radius are examined carefully. Calculation shows that, in the physically important region, quantum defect parameters remain smoothly varying functions of energy for this system as in atomic applications, thus allowing us very coarse energy mesh calculations for the photodissociation spectra. The choice of adiabatic or diabatic potentials as reference potentials for the calculation of quantum defect parameters as done by Mies and Julienne [J. Chem. Phys., 80, 2526 (1984)] can not be used for this system. Physically motivated reference potentials that may be generally applicable to all kinds of systems are utilized instead. In principle, implementation can be done to any other predissociation processes with the same method.

• Bulletin of the Korean Chemical Society
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• 제19권3호
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• pp.319-323
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• 1998

The phodissociation dynamics of t-butyl hydroperoxide at 280-285 nm has been investigated by measuring laser induced fluorescence spectra of the fragment OH. Measured fractions of the available energy distributed among the fragments are ft=0.56, fr(OH)=0.044, fint(t-BuO)=0.40, and negligible populations of OH are found in vibrationally excited states. By analyzing the Doppler profiles of the spectra of OH, the positive ν-J vector correlation has been obtained. From the measured ν-J correlation and A" propensity in the two Λ-doublets of OH, it is concluded that the dissociation takes place directly from the repulsive surface induced by the σ* ← n transition with the fragment OH rotating in the plane perpendicular to the dissociating O-O bond axis.

• 대한화학회지
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• 제51권4호
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• pp.318-323
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• 2007

양성자가 결합된 티로신-알라닌 펩타이드 이온(YAH+)의 전자전이 광분해 스펙트럼을 이 이온의 가 장 낮은 에너지의 전자전이가 관측되는 34500~36700 cm-1 영역에서 얻었다. YAH+ 이온은 전자분무 이온화법 을 이용하여 기체상에서 생성하였고 생성된 이온의 저장 및 검출은 4중극자 이온 트랩과 반사판 비행시간 질 량분석기가 결합된 혼성 질량분석기를 이용하였다. 이온 트랩에 저장된 YAH+ 이온에 레이저 펄스를 쪼여주어 광분해 반응을 유발한 후 그 광분해 정도를 레이저 파장에 따라 측정함으로써 전자전이 광분해 스펙트럼을 얻 었다. 이 스펙트럼에는 두 개의 넓은 폭을 가진 피크가 관측되었으며 시간-의존 밀도함수 법(Time-dependent density functional method, TD-DFT)을 이용한 계산을 통해 각각 YAH+의 S1과 S2 전이로 지정하였다. 관측된 피 크들의 넓은 폭은 상온에서 존재 가능한 YAH+의 여러 이형태체들의 전자전이 간 겹침과 또한, 상온에서 형성 된 이온의 들뜬 진동에너지 준위로부터의 전자전이 즉, 뜨거운 띠(hot band)들 때문인 것으로 설명하였다.

• 천문학회지
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• 제38권2호
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• pp.253-256
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• 2005

We have constructed the Mount Fuji submillimeter-wave telescope at Nishiyasugawara (alt. 3725 m) near the summit of Mt. Fuji (alt. 3774 m). Thanks to the excellent condition of Mt. Fuji, we have successfully carried out the [CI] survey toward more than 40 square degrees of sky, including qrion MC, Taurus MC, Rosetta MC, DR 15, DR 21, NGC 1333, NGC 2264, W 3, W 44, W 51, L 134, p-Oph. Our [CI] survey have revealed that the [CI] 492 GHz emission widely extends to the molecular clouds. The spatial and velocity structures of the [CI] 492 GHz emission resemble those of 13CO J=l-0 in many molecular clouds, implying that [CI] 492 GHz and $^{13}CO$ J=1-0 are emitted from the same gas. The column density of $C^o$ linearly correlates with that of CO up to high Av, suggesting that $C^o$ exist in the deep interior of molecular clouds. In several regions, we have found that the distributions of $C^o$ and CO are different from each other. The $C^o$-rich area is found in the Hieles' cloud 2. The C+/CO/$C^o$ configuration is found in DR 15, p-Oph, M 17, Orion KL, and NGC 1333. These results indicate that an origin of $C^o$ is unrelated with the photodissociation process. We discuss the observed $C^o$ distributions in relation to the non-equilibrium chemistry.

• 천문학회보
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• 제39권2호
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• pp.81.2-81.2
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• 2014

We have analyzed the archival data of far ultraviolet (FUV) observations made for the region of GSH 006-15+7, a large shell-like structure discovered by Moss et al. (2012) from the H I velocity maps. FUV emission is seen enhanced in the lower supershell region and is believed to originate from dust scattering of interstellar photons. A corresponding Monte Carlo simulation indicates that the supershell is located at a distance of $1250^{+750}{_{-500}}$ pc, similar to the previous estimation of 1.5{\pm}0.5 kpc based on kinematic considerations. The spectrum obtained for the lower supershell exhibits molecular hydrogen fluorescence lines: a simulation model for this candidate photodissociation region (PDR) yields a rather high total hydrogen density of $n_H{\sim}30cm^{-3}$ with H2 column density of $N(H_2){=}^{1017.5-20.0}cm^{-2}$. It is argued that the region is in a transition stage from a warm to a cool neutral phase. Strong C IV emission is also seen in the spectrum, but it is not believed to be associated with the supershell as the corresponding spectral map shows a broad region of enhancement both inside and outside the supershell.

• 천문학회보
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• 제39권2호
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• pp.93.1-93.1
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• 2014

The reflection nebula NGC 7023 is a typical example of a photodissociation region (PDR), which consists of high density molecular gas that is exposed to an intense UV radiation field. The source of the UV photons in NGC 7023 is the young pre-main-sequence Be star HD 200755. We present our near-infrared high-resolution (R ~ 40,000) spectrum of NGC 7023, covering a region of $1{\times}15$ arcseconds, observed during the commissioning runs of IGRINS (Immersion GRating near-INfrared Spectrometer). The spectrum shows many strong narrow emission lines that arise from the molecular rovibrational transitions of H2. From the intensity ratios between these H2 lines, we investigate physical conditions within the PDR such as the temperature, density, and pressure. The high spectral resolution of IGRINS allows us to resolve the velocity field of the PDR. In addition, we compare the IGRINS spectrum to Cloudy PDR model.

• 천문학회보
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• 제39권2호
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• pp.92.2-92.2
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• 2014

NGC 6822 is a dwarf irregular galaxy in the Local Group. Unlike clouds in the Large Magellanic Cloud and the Small Magellanic Cloud, molecular clouds in NGC 6822 are not influenced by the Galactic tidal force. Therefore the star forming processes are only dictated by local conditions. Hubble V is the brightest of the several bright H II region complexes in NGC 6822. The core of Hubble V, surrounded by a molecular cloud complex, contains compact clusters of bright blue stars. During the commissioning runs of the new high-resolution near-infrared spectrometer, IGRINS (Immersion GRating near-INfrared Spectrometer), we observed Hubble V and detected many emission lines from the H II regions and from the photodissociation region at the interface between the ionized gas and the molecular cloud. In this presentation, we report preliminary results of the IGRINS observations. We discuss the implications of the observed lines ratios and kinematics for our understanding of the evolution of star forming molecular clouds.

• 천문학회보
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• 제41권2호
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• pp.40.1-40.1
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• 2016

We present the far-ultraviolet fluorescent molecular hydrogen ($H_2$) emission map observed with FIMS/SPEAR for ~76% of the sky. The fluorescent $H_2$ emission is found to be saturated by strong dust extinction at the optically thick, Galactic plane region. However, the extinction-corrected intensity of fluorescent $H_2$ emission is found to have strong linear correlations with the well-known tracers of the cold interstellar medium, such as the E(B-V) color excess, neutral hydrogen column density N(HI), $H{\alpha}$ emission, and CO $J=1{\rightarrow}0$ emission. The all-sky molecular hydrogen column density map is also obtained using a photodissociation region model. We also derive the gas-to-dust ratio, hydrogen molecular fraction ($f_{H2}$), and $CO-to-H_2$ conversion factor ($X_{CO}$) of the diffuse interstellar medium. The gas-to-dust ratio is consistent with the standard value $5.8{\times}10^{21}atoms\;cm^{-2}mag^{-1}$, and the $X_{CO}$ tends to increase with E(B-V), but converges to the Galactic mean value $1.8{\times}10^{20}cm^{-2}K^{-1}km^{-1}s$ at optically thick regions with E(B-V)>2.0.

• 한국전기전자재료학회:학술대회논문집
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• 한국전기전자재료학회 2004년도 추계학술대회 논문집 Vol.17
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• pp.506-509
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• 2004

We have investigated the generation of pretilt angle for a nematic liquid crystal (NLC) alignment with in-situ photoalignment method on polyimide (PI) surfaces using thin plastic substrates. The LC aligning capabilities and pretilt angle of the thin plastic substrates by in-situ photoalignment method were better than that of the glass substrate by general photoalignment. Also, the LC pretilt angle increased with increasing heating temperature and exposure time. And EO characteristics of photoaligned TN-LCDs using in-situ photodissociation method on glass substrate and on plastic substrate are also excellent.

• 천문학회보
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• 제42권1호
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• pp.38.2-38.2
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• 2017

We present the observational study toward the multiple outflows around $LkH{\alpha}$ 234 star formation region. The high-resolution, near-IR spectral mapping using the Immersion Grating Infrared Spectrograph (IGRINS) allowed us to distinguish at least four separate outflows with the molecular hydrogen ($H_2$) and forbidden iron ([Fe II]) emission lines. The outflow associated with the radio continuum source VLA 3B is detected in both H2 and [Fe II] emission, while the outflows driven by MM 1, VLA 2 sources were only detected in $H_2$, indicating the different physical conditions of outflows. We confirm the axis of VLA 3B jet, the position angle of ${\sim}240^{\circ}$. We firstly identified the redshifted, near-IR H2 outflow associated with VLA 2, which is coincident with the previous detections of $H_2O$ masers. From the $H_2$ line ratios, we interpret the gas properties of the shock excited blue- and redshifted components, and UV excited surrounding photodissociation region. We also discuss the origin of the high-velocity (|VLSR| > $150km\;s^{-1}$) $H_2$ emission.