• 천문학회지
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• 제37권4호
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• pp.211-216
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• 2004

We present the results of an H I aperture synthesis mosaic of the Large Magellanic Cloud (LMC), made by combining data from 1344 separate pointing centers using the Australia Telescope Compact' Array (ATCA) and the Parkes multibeam receiver. The resolution of the mosaiced images is 50" (<15 pc, using a distance to the LMC of 55kpc). This mosaic, with a spatial resolution .15 times higher than that which had been previously obtained, emphasises the turbulent and fractal structure of the ISM on the small scale, resulting from the dynamical feedback of the star formation processes with the ISM. We also have done a widefield panoramic survey of H$\alpha$ emission from the Magellanic Clouds with an imager mounted on the 16-inch telescope at Siding Spring Observatory. This survey produced H$\alpha$ images which are equal to the ATCA survey in area coverage and resolution. This survey allows us to produce a continuum-subtracted image of the entire LMC. In contrast with its appearance in the H$\alpha$ image, the LMC is remarkably symmetric in H I on the largest scales, with the bulk of the H I residing in a disk of diameter 8. $^{\circ}4$ (7.3 kpc) and a spiral structure is clearly seen. The structure of the neutral atomic ISM in the LMC is dominated by H I filaments combined with numerous shells and holes.

• 전기전자학회논문지
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• 제17권3호
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• pp.385-392
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• 2013

본 논문에서는 근접물체에 둔감하도록 평면 안테나의 송신단과 수신단 사이의 분리도를 개선하는 회로구조를 제안하였으며 5.8GHz ISM 대역에서 생체신호를 검출하는 도플러 레이다 센서에 적용하였다. 방사패치를 중심으로 2개의 3dB $90^{\circ}$ 전력분배기 들을 송신경로와 수신경로에 배치하여 평형회로 구조를 구성하였다. 이는 안테나에 근접된 물체가 있어도 높은 송수신 분리도 및 우수한 입출력 반사계수를 제공한다. 제안된 회로구조에 대한 이론 전개와 시뮬레이션을 통해 타당성을 확인하였고 제작된 시제품을 측정하여 입증하였다. 인체가 2mm까지 접근하여도 ISM대역에 걸쳐 송신단과 수신단에서 16dB 이상의 반사손실과 최소 30dB 이상의 분리도가 측정되었다.

• 한국통신학회논문지
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• 제40권5호
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• pp.944-949
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• 2015

본 논문에서는 단일 패치 안테나에 다중 포트를 결합하여 무선 통신 기기의 응용에 적합한 MIMO구조의 패치 안테나를 제안하였다. 제안된 MIMO 패치 안테나는 비 유전율 4.5, 손실 탄젠트 0.0035, 두께 1.52 mm를 갖는 TRF-45 기판을 통해 설계되었으며, 안테나의 중심 주파수는 ISM (Industrial Scientific and Medical) 대역의 2.45 GHz이다. 제안된 MIMO 패치 안테나는 2.16 ~ 2.66 GHz 대역에서 500 MHz의 대역폭을 보였으며, 비 대역폭은 24.1%이다. 안테나의 반사손실 및 정재파비 결과는 제안된 대역에서 2.45 GHz의 ISM 대역에서 -62.05 dB, 1.01이다. 대역폭에 포함된 각각의 대역은 2.3 GHz의 WiBro 대역은 -17.43 dB, 1.33, 2.4 GHz의 WiFi 대역은 -31.89 dB, 1.05, 2.5 GHz의 WiMax 대역은 -36.47 dB, 1.03이다. 대역폭에 포함된 대역의 방사패턴 분석은 지향성의 패턴을 보였으며, 2.3 GHz의 WiBro 대역은 4.22 dBi, 2.4 GHz의 WiFi 대역은 4.12 dBi, 2.45 GHz의 ISM 대역은 4.06 dBi, 2.5 GHz의 WiMax 대역은 3.96 dBi의 이득을 보였다.

• 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.

• 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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• 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.

• 천문학회지
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• 제40권3호
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• pp.61-65
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• 2007

The 2-1 and 5-4 transitions of SiO have been observed toward the Sgr B2 region, including the Principal Cloud(the GMC containing Sgr B2(M)) and its surroundings. The morphology and velocity structure of the SiO emission show a close resemblance with the HNCO Ring feature, identified by Minh & Irvine(2006), of about 10 pc in diameter, which may be expanding and colliding with the Principal Cloud. Three SiO clumps have been found around the Ring, with total column densities $N_{SiO}{\sim}1{\times}10^{14}cm^{-2}$ at the peak positions of these clumps. The fractional SiO abundance relative to $H_2$ has been estimated to be ${\sim}(0.5-1){\times}10^{-9}$, which is about two orders of magnitude larger than the quiet dense cloud values. Our SiO observational result supports the existence of an expanding ring, which may be triggering active star formations in the Principal Cloud.

• 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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• 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.