• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.65.1-65.1
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• 2010

성간난류에 대해 간략히 소개하고 최근의 관측결과를 살펴본다. 최근 연구 결과에 의하면 성간난류는 은하자기장의 생성에 기여하며 별 생성에 결정적인 역할을 한다. 성간난류는 다양한 형태로 나타날 수 있다. 예를 들어 성간매질에는 여러 가지 상(phase)이 존재하며 상이 달라지면 난류의 성질이 달라지며 난류의 구조도 달라진다. 매질이 달라지면 난류를 관측하는 방법도 달라질 수밖에 없다. 본 발표에서는 성간매질의 상(phase)에 따라 어떤 종류의 난류가 존재하며 어떤 관측을 통해 연구하는 지를 알아본다. 또한 성간공간에 실재하는 3차원 난류의 물리량과 천구면에 투영된 2차원 물리량 사이에는 어떤 관계가 있는지를 살펴본다.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.1
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• pp.27.3-27.3
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• 2017

One of the major discoveries in extragalactic astrophysics made over the past few years is the detection of ultra-diffuse galaxies, a new type of galaxies which appear to be far more numerous than normal galaxies, and which are giants in terms of size, yet dwarfs in terms of luminosity. These galaxies point to the huge discovery potential of the last niche that remains to be explored in observational parameter space: the sky at extremelylow surface brightness. Implications for objects in the Solar System, stellar physics, the interstellar medium, galaxies and cosmology will be addressed, along with the major challenges for pushing the frontiers in ground- and space-based observations.

• Journal of The Korean Astronomical Society
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• v.13 no.1
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• pp.9-14
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• 1980

The abundances of simple molecules are examined in terms of the time-dependent cloud evolution. The formation and destruction mechanisms of $H_2CO$ are reviewed. The average value of the fractional abundance of $H_2CO$ is derived to be in the range of $10^{-10}\;to\;5{\times}10^{-9}$. This is comparable to the observed values. The expected variations of the molecules formed from or destroyed by CO, CI, and $C^+$ whose abundances depend on the evolutionary state of the cloud are discussed.

• Publications of The Korean Astronomical Society
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• v.24 no.1
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• pp.1-8
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• 2009

A plane-parallel model of the diffuse Galactic light (DGL) is calculated assuming exponential disks of interstellar dust and OB stars, by solving exactly the radiative transfer equation using an iterative method. We perform a radiative transfer calculation for a model with generally accepted scale heights of stellar and dust distribution and compare the results with those of van de Hulst & de Jong for a constant slab model. We also find that the intensity extrapolated to zero dust optical depth has a negative value, against to the usual expectation.

• Bulletin of the Korean Space Science Society
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• 2004.10b
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• pp.49-49
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• 2004

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.553-557
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• 2015

This review summarises the current status of the Galactic TeV ($10^{12}$ eV) gamma-ray source population. It also briefly looks at the future beyond the current generation of TeV gamma-ray facilities, and highlights the role of the interstellar medium (ISM) in helping to resolve some of the challenges in interpreting the wealth of results which have been found in recent years.

• Bulletin of the Korean Chemical Society
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• v.21 no.7
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• pp.734-740
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• 2000

Density functional theory calculations are presented for the geometrical isomers of the cyanopolyacetylenes H(C≡C)n,,C≡N (n = I-3). The structures, hartmonic frequencies and dipole moments are computed, employing the 6-311G** basis set. The ener gies of barrier to isomerization (exchange of carbon and nitrogen atoms) are also computed in order to estimate the stability of the isomers in interstellar space.

• Journal of The Korean Astronomical Society
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• v.27 no.1
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• pp.55-60
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• 1994

The 3mm transitions to CO, $^{13}CO,\;CS,\;HCO^+$, and HCN have been observed toward the compact HII regions in W58 using the 14m Daeduk Radio Telescope (DRT). Some of the observed lines show high-velocity wings resulted from outflowing materials of the compact HII regions. We derive the beam averaged column densities of the observed species and compare their relative abundances. The $HCO^+$ abundance appears to be smaller by about an order of magnitude than those of 'typical' quiet molecular clouds. CS may be a good reference molecule in comparing relative abundances in different physical conditions.

• Publications of The Korean Astronomical Society
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• v.27 no.4
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• pp.353-356
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• 2012

We present new constraints on the cosmic optical background (COB) obtained from an analysis of the Pioneer 10/11 Imaging Photopolarimeter (IPP) data. After careful examination of the data quality, the usable measurements free from the zodiacal light are integrated into sky maps at the blue (${\sim}0.44{\mu}m$) and red (${\sim}0.64{\mu}m$) bands. Accurate starlight subtraction was achieved by referring to all-sky star catalogs and a Galactic stellar population synthesis model down to 32.0 mag. We find that the residual light is separated into two components: one component shows a clear correlation with the thermal $100{\mu}m$ brightness, whilst the other shows a constant level in the lowest $100{\mu}m$ brightness region. The presence of the second component is significant after all the uncertainties and possible residual light in the Galaxy are taken into account, thus it most likely has an extragalactic origin (i.e., the COB). The derived COB brightness is ($(1.8{\pm}0.9){\times}10^{-9}$ and $(1.2{\pm}0.9){\times}10^{-9}\;erg\;s^{-1}\;cm^{-2}\;sr^{-1}\;{\AA}^{-1}$ in the blue and red spectral regions, respectively, or $7.9{\pm}4.0$ and $7.7{\pm}5.8\;nW\;m^{-2}\;sr^{-1}$. Based on a comparison with the integrated brightness of galaxies, we conclude that the bulk of the COB is comprised of normal galaxies which have already been resolved by the current deepest observations. There seems to be little room for contributions from other populations including "first stars" at these wavelengths. On the other hand, the first component of the IPP residual light represents the diffuse Galactic light (DGL)-scattered starlight by the interstellar dust. We derive the mean DGL-to-$100{\mu}m$ brightness ratios of $2.1{\times}10^{-3}$ and $4.6{\times}10^{-3}$ at the two bands, which are roughly consistent with previous observations toward denser dust regions. Extended red emission in the diffuse interstellar medium is also confirmed.

• Publications of The Korean Astronomical Society
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• v.32 no.1
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• pp.77-81
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• 2017

A wide spectral coverage from near-infrared (NIR) to far-infrared (FIR) of AKARI both for imaging and spectroscopy enables us to efficiently study the emission from gas and dust in the interstellar medium (ISM). In particular, the Infrared Camera (IRC) onboard AKARI offers a unique opportunity to carry out sensitive spectroscopy in the NIR ($2-5{\mu}m$) for the first time from a spaceborn telescope. This spectral range contains a number of important dust bands and gas lines, such as the aromatic and aliphatic emission bands at 3.3 and $3.4-3.5{\mu}m$, $H_2O$ and $CO_2$ ices at 3.0 and $4.3{\mu}m$, CO, $H_2$, and H I gas emission lines. In this paper we concentrate on the aromatic and aliphatic emission and ice absorption features. The balance between dust supply and destruction suggests significant dust processing taking place as well as dust formation in the ISM. Detailed analysis of the aromatic and aliphatic bands of AKARI observations for a number of H ii regions and H ii region-like objects suggests processing of carbonaceous dust in the ISM. The ice formation process can also be studied with IRC NIR spectroscopy efficiently. In this review, dust processing in the ISM divulged by recent analysis of AKARI data is discussed.