• 수산해양교육연구
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• 제26권6호
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• pp.1442-1450
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• 2014

The aim of this study is to develop a model for the alternative selection in port privatization using Brainstorming, the ISM and AHP methods. For this, 30 detailed attributing factors were identified by both previous studies and port users, Also, 13 attributing evaluation factors were identified by a group of port experts using the brainstorming method. These were made into a model of hierarchical structure with 3 levels, taking 1 goal factor, 5 evaluation factors and 7 alternative factors using the ISM method. The collected date of questionnaires through the AHP method were analyzed with a group of port experts for an empirical analysis. The result of the hierarchical level 2 shows that profitability is the most important factor, followed by public interest, management professionality, service quality and financial soundness. The analysis results of hierarchical level 3 shows that commercialization is the most important factor.

• 천문학회지
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• 제33권1호
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• pp.37-45
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• 2000

We have investigated the properties of the high-latitude cloud MBM 7 using the 3 mm transitions of CO, CS, HCN, $HCO^+,\;C_3H_2,\;N_2H^+$, and SiO. The molecular component of MBM 7 shows a very clumpy structure with a size of $\le$0.5 pc, elongated along the northwest-southeast direction, perpendicularly to an extended HI component, which could be resulted from shock formation. We have derived physical properties for two molecular cores in the central region. Their sizes are 0.1-0.3 pc and masses 1-2 M$\bigodot$ having an average volume density $\~2{\times}10^3 cm^{-3}$ at the peak of molecular emission. We have tested the stability of the cores using the full version of the virial theorem and found that the cores are stabilized with ambient medium, and they are expected not to be dissipated easily without external perturbations. Therefore MBM 7 does not seem to be a site for new star formation. The molecular abundances in the densest core appear to be much less (by about one order of magnitude) than the 'general' dark cloud values. If the depletions of heavy elements are not significant in the HLCs compared with those in typical dark clouds, our results may suggest different chemical evolutionary stages or different chemical environments of the HLCs compared with dense dark clouds in the Galactic plane.

• 천문학회지
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• 제49권6호
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• pp.255-259
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• 2016

We estimate the fractal dimension of the ${\rho}$ Ophiuchus Molecular Cloud Complex, associated with star forming regions. We selected a cube (${\upsilon}$, l, b) database, obtained with J = 1-0 transition lines of $^{12}CO$ and $^{13}CO$ at a resolution of 22" using a multibeam receiver system on the 14-m telescope of the Five College Radio Astronomy Observatory. Using a code developed within IRAF, we identified slice-clouds with two threshold temperatures to estimate the fractal dimension. With threshold temperatures of 2.25 K ($3{\sigma}$) and 3.75 K ($5{\sigma}$), the fractal dimension of the target cloud is estimated to be D = 1.52-1.54, where $P{\propto}A^{D/2}$, which is larger than previous results. We suggest that the sampling rate (spatial resolution) of observed data must be an important parameter when estimating the fractal dimension, and that narrower or wider dispersion around an arbitrary fit line and the intercepts at NP = 100 should be checked whether they relate to firms noise level or characteristic structure of the target cloud. This issue could be investigated by analysing several high resolution databases with different quality (low or moderate sensitivity).

• 천문학회지
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• 제44권5호
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• pp.201-208
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• 2011

The NGC 1333 IRAS 4B region is observed in the 6.9 mm and 1.3 cm continuum with an angular resolution of about 0.4 arcseconds. IRAS 4BI is detected in both bands, and BII is detected in the 6.9 mm continuum only. The 1.3 cm source of BI seems to be a disk-like flattened structure with a size of about 50 AU. IRAS 4BI does not show any sign of multiplicity. Examinations of archival infrared images show that the dominating emission feature in this region is a bright peak in the southern outflow driven by BI, corresponding to the molecular hydrogen emission source HL 9a. Both BI and BII are undetectable in the mid-IR bands. The upper limit on the far-IR flux of IRAS 4BII suggests that it may be a very low luminosity young stellar object.

• 천문학논총
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• 제32권1호
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• pp.113-116
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• 2017

A significant number of the parameters of a gamma-ray burst (GRB) and its host galaxy are calculated from the afterglow. There are various methods obtaining extinction values for the necessary correction for galactic foreground. These are: galaxy counts, from HI 21 cm surveys, from spectroscopic measurements and colors of nearby Galactic stars, or using extinction maps calculated from infrared surveys towards the GRB. We demonstrate that AKARI Far-Infrared Surveyor sky surface brightness maps are useful uncovering the fine structure of the galactic foreground of GRBs. Galactic cirrus structures of a number of GRBs are calculated with a 2 arcminute resolution, and the results are compared to that of other methods.

• 천문학회지
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• 제34권4호
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• pp.341-343
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• 2001

Here were continue the MHD study started by Santillan et al (1999) for the interaction of high-velocity clouds (HVCs) with the magnetized thick gaseous disk of our Galaxy. We use the MHD code ZEUS-3D and perform 3D-numerical simulations of this interaction, and study the formation of head-tail structures in HVCs. Our results show that clouds located above 2 kpc from mindplane present velocity and column density gradients with a cometary structure that is similar to those observed in 21 cm emission

• 한국정보기술학회논문지
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• 제16권11호
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• pp.77-84
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• 2018

본 논문에서는 T-junction 전력 분배기를 이용한 원형 편파 마이크로스트립 패치 안테나를 제안하였다. 제안된 안테나의 동작 주파수는 2.4GHz의 ISM 대역이며, 패치 안테나의 두 가장자리에 $90^{\circ}$의 위상차를 급전하여 원형 편파를 유도하였다. 안테나의 구조는 일반적인 패치 안테나와 T-junction 전력 분배기로 구성된다. 안테나의 최적화를 위해 반사계수, 축비, 방사패턴 등이 분석된다. 안테나의 임피던스 대역폭은 2.39~2.43GHz 대역에서 40MHz의 대역폭이 관찰되었으며, 축비 대역폭은 2.398~2.410GHz 대역에서 약 12MHz의 대역폭이 관찰되었다. 안테나의 방사패턴은 우회전 원형 편파로 동작하였다. 또한 안테나의 이득은 XZ 및 YZ-평면에서 각각 2.04, 3.4㏈ic가 관찰되었다.

• 천문학회지
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• 제34권3호
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• pp.157-166
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• 2001

The molecular cloud associated with the H II region S301 has been mapped in the J = 1-0 transitions of $^{12}CO$ and $^{13}CO$ using the 13.7 m radio telescope of Taeduk Radio Astronomy Observatory. The cloud is elongated along the north-south direction with two strong emission components facing the H II region. Its total mass is $8.7 {\times} 10^3 M{\bigodot}$. We find a velocity gradient of the molecular gas near the interface with the optical H II region, which may be a signature of interaction between the molecular cloud and the H II region. Spectra of CO, CS, and HCO+ exhibit line splitting even in the densest part of the cloud and suggests the clumpy structure. The radio continuum maps show that the ionzed gas is distributed with some asymmetry and the eastern part of the H II region is obscured by the molecular cloud. We propose that the S301 H II region is at the late stage of the champagne phase, but the second generation of stars has not yet been formed in the postshock layer.

• 한국정보통신학회:학술대회논문집
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• 한국해양정보통신학회 2007년도 춘계종합학술대회
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• pp.580-583
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• 2007

본 논문에서는 슬롯 안테나 구조를 변형하여 ISM용 마이크로스트립 슬롯 안테나를 제안했다. 제안된 안테나는 기존의 슬롯 안테나 급전 구조에 변형된 급전선로를 이용하여 이중대역에서 공진주파수가 나타나도록 설계 제작하였다. 설계된 안테나는 2.45 GHz, 5 GHz의 중심 주파수에서 각각 8.23%, 4.8%의 대역폭을 갖고, 변형된 급전선로의 길이변화에 따라 대역폭과 공진주파수가 변화하였다. 또한, 제작된 안테나의 방사 패턴 특성은 각각 주파수에서 E면과 H면의 특성이 비교적 양호하게 측정되었다.

• 천문학논총
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• 제16권1호
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• pp.15-20
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• 2001

We observed the thermal transitions of SiO (J=I-0, 2-1) and $^{29}SiO$ (J=l-O) toward the Sgr A molecular clouds. The distribution and the velocity structure of SiO are very similar to previous results for 'quiet' interstellar molecules. We think· that the SiO has been well mixed with other molecules such as $H_2$ which may indicate that the formation of Sgr A molecular clouds was affected by the activities, such as shock waves or energetic photons, from the Galactic center in large scales. The total column density of SiO is about $4.1\times10^{14} cm^{-2}$ and the fractional abundance $SiO/H_2$ appears to be about 10 times larger than those of other clouds in the central region of our galaxy. The derived values are thought to be lower limits since the optical depths of the observed SiO lines are not very thin. The formation of SiO has been known to be critically related to shocks, and our results provide informative data on the environment of our Galactic center.