• Journal of The Korean Astronomical Society
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• v.21 no.2
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• pp.155-171
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• 1988

We have examined how sensitively the extinction value determined by the method of star-count depends on such factors as the plate limit, the size of counting reseau, the non-linearity in the number distribution of stars with magnitude, and the angular resolution demanded by the given problem. We let the Poisson distribution portray the statistical nature of the countings, and chose the region containing the globule Barnard 361 as an example field. Uncertainties due to various combinations of the factors are presented in graphic forms: (1) Dynamic range in the extinction measurements is evaluated as a function of reseau size for varying plate limits. (2) Statistical errors involved in the star-count are analized in terms of the signal-to-noise ratio, the plate limit and the reseau size. (3) Systematic error due to the non-linearity in the number distribution are thoroughly analized. (4) Finally, a methodology is presented for correcting the systematic error in the observed radial density gradient. These graphs are meant to be used in selecting proper size of the reseau and in estimating errors inherent to the star-count analysis.

• The Bulletin of The Korean Astronomical Society
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• v.14
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• pp.7.3-8
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• 1989

• The Bulletin of The Korean Astronomical Society
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• v.10
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• pp.6.3-7
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• 1985

• Journal of The Korean Astronomical Society
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• v.22 no.1
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• pp.63-79
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• 1989

Current estimates, based on the same star-count analysis, of the distance to the globule Bamard 361 range from 300 pc to 650 pc. All the problems associated with the estimates have been fully rectified in this study, and a modification has been made to the classical Wolf diagram to improve the accuracy in the distance determination. A reference field was carefully selected close to the globule but well outside the globule boundary, and star counts for this field were performed on the blue POSS plate in order to set up the reference magnitude sequence appropriate to the general area of B 361. From the reference sequence, the stellar density function has been derived specifically for the direction toward the globule. Correction was made for the general interstellar extinction, and the luminosity function with the Wielen's dip was adopted. The resulting density function clearly reveals the existence of the local Cygnus-Orion arm in the direction of B 361 at about 700 pc away from the Sun. Analysis of the star-count data for the program field locates the globule at distance $600{\pm}50$ pc ; thus, the globule is an object located in the Cygnus-Orion arm, residing somewhat toward its leading edge.

• Journal of Astronomy and Space Sciences
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• v.19 no.1
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• pp.19-24
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• 2002

The five space density distribution D(z) wish distance perpendicular to the Galactic plane were combined. The scale heights and the local densities at z = 0 of the thin disk, thick disk, and the halo components were estimated from the nonlinear least square fits of exponential law. The scale heights of the thin disk, thick disk, and the halo components were estimated to be $260{\pm}90$ pc, $660{\pm}220$ pc, and $3.6{\pm}1.4$ kpc, respectively. The density ratio of each components to the thin disk component at the galactic plane, i.e., z = 0.0, were also derived as 1 :0.07:0.002. Our model fit suggests that the thick disk component has a local density of 6.9% relative to the thin disk.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.1
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• pp.60.2-60.2
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• 2014

The dust cloud around ${\lambda}$-Orionis is seen to be circular symmetric with the large angular extent (${\sim}8^{\circ}$). However, whether the three dimensional structure of the cloud is shell or torus ring is not yet fully resolved. We studied the structure of the dust cloud using a three-dimensional Monte-Carlo simulation code, MoCafe (Monte Carlo radiative transfer). The dust density structure of the cloud was inferred based on the star-count method. We assumed that the cloud is a spherical shell or a torus ring and calculated the radial profiles of scattered light originating from a central OB association. Comparison of the results with the S2/68 ultraviolet observations indicates that the cloud is a spherical shell. We also compared the Av map around ${\lambda}$-Orionis with the optical depth obtained based on the star-count.

• The KIPS Transactions:PartC
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• v.11C no.5
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• pp.645-652
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• 2004

In this paper, we aggregate multi-links information between boundary nodes using the line segment scheme that aggregates topology in-formation within PG referring bandwidth and delay parameter. The proposed scheme can search multi-links efficiently using the depth priority method based on hop count instead of searching all links. To do this, we propose a modified line segment algorithm using two line segment method that represents two points which consist of delay-bandwidth pair to reduce topology information and provide a flexibility to the multi pie-links aggregation. And we apply it to current star topology aggregation. To evaluate performance of the proposed scheme, we compare/analyze the current method with the proposed scheme with respect to call success rate, access time and crankback rate. Through the simulation result analysis, the proposed star topology aggregation scheme presents the better performance than existing scheme.

• Electronics and Telecommunications Trends
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• v.8 no.4
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• pp.143-156
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• 1993

ISDN 을 구축하기 위한 망구조로 ISDN 의 다양한 서비스 수용 관점에서 Single Star 형 망구조가 가장 잠재력이 우수한 구조로 평가되고 있으며 Single Star 형 구조로 구축될 때 High Count Optical Fiber Cable 과 광커넥터 (단심, 다심) 가 요구된다. 그중 광커넥터는 광 가입자 망의 구축을 위해 필수적인 부품으로서 기술 추세는 다심화, 복합 기능화, 소형화, 저가격화, 고성능화, 고신뢰성화의 방향으로 진행되고 있다. 본 고에서는 향후 국내에서 적용 가능한 광케이블용 다심 광커넥터 개발을 위하여 외국에서 개발되어 있는 제품의 정렬원리, 정렬 구조 및 제조기술을 분석하였으며 또한 국내의 수요를 분석하였다. 수요 분석은 과거의 생산 실적 자료가 없는 이유로 정량적 분석법보다는 전화 가입자 수요 자료와 가입자 선로의 광케이블 계획, 그리고 광 CATV 가입자 예측 자료를 이용한 정성적인 방법을 적용하였다.

• Bulletin of the Korean Space Science Society
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• 1993.04a
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• pp.12-12
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• 1993

암혹성운 B5 영역의 중심 부분을 분자흡수선 BSCO의 6cm와 방출선인 2mmE 관측하였다. 관측은 독일의 Bonn에 있는 전파망원경과 미국의 Arizona주의 Kit Peak에 있는 전파망원정을 사용하였다. 본 관측 결과에서 얻어진 antenna temperature (Ta)의 분포를 mappin 하였다. 이 두 종류의 판측을 상호 비교한 결과 최대 황도의 위치가 서로일치하지 않음을 확인하였다. 6cm의 관측결과는 star count 방법에 의하여 결정된 extionction map에 나타나는 중심지역과 거의 일치하나, 2mm 관측은 B5 내에 있는 적외선광인 IRS 1의 위치와 일치하였다. 본 연구에서는 다른 분자선 관측 결과와 비교하므로써 H2CO의 관측 결과를 분석하였다.

• ETRI Journal
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• v.36 no.2
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• pp.293-300
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• 2014

As the system-on-chip (SoC) design becomes more complex, the test costs are increasing. One of the main obstacles of a test cost reduction is the limited number of test channels of the ATE while the number of pins in the design increases. To overcome this problem, a new test architecture using a channel sharing compliant with IEEE Standard 1149.1 and 1500 is proposed. It can significantly reduce the pin count for testing a SoC design. The test input data is transmitted using a test access mechanism composed of only input pins. A single test data output pin is used to measure the sink values. The experimental results show that the proposed architecture not only increases the number of sites to be tested simultaneously, but also reduces the test time. In addition, the yield loss owing to the proven contact problems can be reduced. Using the new architecture, it is possible to achieve a large test time and cost reduction for complex SoC designs with negligible design and test overheads.