• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.96.2-96.2
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• 2014

Using solar occultation data obtained by Cassini/Visual Infrared Mapping Spectrometer (VIMS), we were able to retrieve the 1 - 5 mm optical-depth spectra of the Titanian haze, for which only selected wavelength and altitudinal ranges were previously analyzed. We found that the gross 1 - 5 mm shapes of the retrieved haze spectra are significantly different from the spectra of tholin samples in the literature. We also derived the vertical variation of the spectral structure of the $3.3-3.4{\mu}m$ absorption feature of the Titan haze from the VIMS data recorded between 250 and 700 km altitude. We found a marked change between 480 and 580 km in the relative amplitudes of the 3.33 and $3.38{\mu}m$ features which are characteristic of aromatic (double C=Cchains or rings) or aliphatic (single C-C chains) structural groups, respectively. Dicussions on this spectral and altitudinal variation will be presented.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.1
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• pp.51.1-51.1
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• 2012

We observed low-z quasar PG1426+015 (z=0.086), using the near-IR high resolution echelle spectrometer, IRCS, at the SUBARU 8.2 m telescope. Using an Adoptive Optics system, the full width at half maximum of the point spread function was about 0.3 arcsec, which can effectively separate the quasar spectra from the host galaxy spectra. We also maximize the total exposure time up to several hours per target, and develop data reduction methods to increase the signal-to-noise ratios. This poster presents the data reduction processes and sample spectra from the quasar and its host galaxy. These spectral lines will be used to study the physical mechanism of quasars, and the velocity dispersions of the stars in the bugle of the host galaxy.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.1
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• pp.62.1-62.1
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• 2013

The Cassini/Visual Infrared Mapping Spectrometer (VIMS) observed the sun through the atmosphere of Titan, and provided vertically-resolved 63 spectra from 49 km to 987 km for the 1 - 5 micron range (Bellucci, 2008). Bellucci et al. (2009) analyzed selected spectral ranges where the band absorptions of $CH_4$ and CO are strong by constructing synthetic spectra including $CH_4$ and CO lines, but without including haze absorptions in their synthetic spectra. Kim et al. (2011) and Sim et al. (2013) were able to extract detailed spectral features of fundamental (Dv = 1) and overtone (Dv = 2) bands of the haze from the VIMS spectra by excluding the adjacent influences of strong $CH_4$ absorptions using a radiative transfer program, which includes effects of absorption and emission of lines of these molecules, and absorption and scattering of haze particles. In this presentation, we extend our detailed analyses to other remaining wavelengths in order to provide the spectral characteristics of the Titanian haze for the entire 1 - 5 micron range and to identify any additional haze spectral features and an unidentified feature near 4.3 microns reported by Bellucci et al. (2009).

• Bulletin of the Korean Chemical Society
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• v.14 no.1
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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$^{-1}$.

• Journal of the Korean Chemical Society
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• v.49 no.3
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• pp.261-268
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• 2005

• Journal of Astronomy and Space Sciences
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• v.11 no.2
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• pp.165-174
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• 1994

We have investigated the chemical composition of dust grains in novae by computing the model spectra for the novae that showed temporary infrared developments shortly after their optical explosions. We find that a simple spherical dust shell models with hot blackbody central sources fit observations fairly well. Optical properties of dust grains deduced from modeling of AGB stars have been used for present calculations. We find that amorphous carbon grains appear to be the major infrared re-emission sources for the carbon-rich nova shells, and the silicate grains for the oxygen-rich nova shells.

• Journal of the Korean Chemical Society
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• v.29 no.3
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• pp.252-256
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• 1985

Absolute infrared intensities are predicted for the vibrational bands of gas-phase SiF$_2$ using a fluorine atomic polar tensor transferred from various fluorine compounds. The predicted relative intensities agree well with published spectra of gas-phase SiF$_2$.

• Proceedings of the PSK Conference
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• 2003.04a
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• pp.289.1-289.1
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• 2003

Three types of near infrared spectrometer, a photo diode array type, a dispersive type and a FT type, were evaluated and compared the systematic difference in blood glucose measurement. The fundamental study was performed by adding glucose to buffer solution and bovine blood as the preceding study of non-invasive blood glucose. Spectra were collected using a 1.0 mm optical pathlength quartz cell by transmittance method. (omitted)

• Proceedings of the PSK Conference
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• 2003.04a
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• pp.290.2-290.2
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• 2003

Skin Moisture is an important factor in skin health. Measurement of moisture content can provide diagnostic information on the condition of skin. In this study, a photo diode array type near infrared spectroscopy was used to determine skin moisture. Diffuse reflectance spectra were collected and transformed to absorbance using 1-nm stepsize over the wavelength range of 1100 nm to 2200 nm. (omitted)

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.55.1-55.1
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• 2011

Luminous infrared galaxies (LIRGs; $L_{IR}$ > ${10^{11}}_{Lsun}$) are the most powerful objects in the local Universe. Previous work suggested that dust re-processing of starburst and/or active galactic nuclei (AGN) activity, triggered by galaxy interactions, is responsible for their enormous infrared emission. To understand the nature of LIRGs, it is essential to determine their spectral types. Optical spectral types of 115 ultraluminous infrared galaxies in the southern sky are presented using CTIO observations. The AGN fraction is on average 50% and increases with infrared luminosity. Near-infrared spectral types of 36 LIRGs are also presented based on AKARI observations. In the sample, 12 optically elusive buried AGNs are found. To investigate the evolutionary sequence of LIRGs, star formation histories of ~6000 LIRGs in the SDSS and IRAS/AKARI matched sample are derived by comparing observed optical spectra and stellar population models. AGN-dominated LIRGs are currently massive relative to starburst-dominated LIRGs, which originates from an enhancement of star formation at intermediate-ages. For ~1100 early-type LIRGs, optical and NIR fundamental planes (FPs) are constructed. The FP of LIRGs is significantly different from that of normal early-type galaxies, but the difference is minimized in low luminous and AGN-like LIRGs. These findings support that the importance of AGN is growing as infrared luminosity increases and that LIRGs follow at least in the high mass regime the standard evolutionary scenario: starburst LIRGs evolve into AGN LIRGs and finally into normal early-type galaxies.