• 한국어류학회지
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• 제6권2호
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• pp.160-171
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• 1994

놀래기과(科) (family Labridae) 어류의 측선(測線) 감각공(感覺孔) 비늘의 형태(形態)는 타원형 (ellipse), 5각형 (pentagonal), 6각형 (hexagonal)의 3가지형으로 분류될 수 있었으며 대부분이 6각형을 나타내었는데 실용치 (Cirrhilabrus temminckii)가 타원형을 나타내었고 옥두놀래기 (Xyrichtys dea), 호박돔 (Choerodon azurio), 흑돔 (Semicossyphus reticulatus), 사랑놀래기 (Bodianus oxycephalus)가 5각형을 나타내었다. 6각형인 황놀래기 (Pseudolabrus japonicus), 놀래기 (Halichoeres tenuispinnis)는 비교적 수심이 깊은곳에 서식하며 주위환경에 잘 반응하는 종으로 이들의 감각관(感覺管)은 가늘고 긴 감각기(感覺技)가 잘 발달되어 있는 반면 5각형의 사랑놀래기, 혹돔과 6각형인 청줄청소놀래기 (Labroides dimidiatus), 꼬치놀래기 (Cheilio inermis), 실놀래기 (Suezichthys gracilis), 무지개놀래기 (Stethojulis interupta terina), 용치놀래기 (Halichoeres poecilopterus)는 감각관(感覺管)이 비교적 크고 감각기(感覺技)의 분지가 적어서 원시형을 나타내고 있었다. 또한 감각공(感覺孔)의 크기는 흑돔, 꼬치놀래기, 청줄청소놀래기, 놀래기가 비늘폭의 25.0 %이상으로 다른 놀래기과(科) 어류(魚類)의 12.5%보다 상대적으로 컸으며 반면 옥두놀래기인 경우 5.8 %로 작았다. 이러한 놀래기과(科) 어류(魚類)가 가진 측선감각공(側線感覺孔)의 다양한 형태는 이들의 서식(棲息) 환경과 측선(測線) 감각공(感覺孔) 비늘의 감각관(感覺管)의 발달 사이에 깊은 관계가 있음을 알 수 있었다.

• 천문학회보
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• 제44권1호
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• pp.33.3-33.3
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• 2019

Automatic, yet reliable methods to find and classify barred galaxies are going to be more important in the era of large galaxy surveys. Here, we introduce a new approach to classify barred galaxies by analyzing the butterfly pattern that Buta & Block (2001) reported as a bar signature on the potential map. We make it easy to find the pattern by moving the ratio map from a Cartesian coordinate to a polar coordinate. Our volume-limited sample consists of 1698 spiral galaxies brighter than Mr = -15.2 with z < 0.01 from the Sloan Digital Sky Survey/DR7 visually classified by Ann et al. (2015). We compared the results of the classification obtained by four different methods: visual inspection, ellipse fitting, Fourier analysis, and our new method. We obtain, for the same sample, different bar fractions of 63%, 48%, 36%, and 56% by visual inspection, ellipse fitting, Fourier analysis, and our new approach, respectively. Although automatic classifications detect visually determined, strongly barred galaxies with the concordance of 74% to 86%, automatically selected barred galaxies contain different amount of weak bars. We find a different dependence of bar fraction on the Hubble type for strong and weak bars: SBs are preponderant in early-type spirals, whereas SABs are in late-type spirals. Moreover, the ellipse fitting method often misses strongly barred galaxies in the bulge-dominated galaxies. These explain why previous works showed the contradictory dependence of the bar fraction on the host galaxy properties. Our new method has the highest agreement with visual inspection in terms of the individual classification and the overall bar fraction. In addition, we find another signature on the ratio map to classify barred galaxies into new two classes that are probably related to the age of the bar.

• 천문학회보
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• 제42권2호
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• pp.43.4-44
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• 2017

Bar fractions depend on the properties of host galaxies. However, the observational studies did not provide consistent tendency. We investigated the bar fractions and their dependence on properties of host galaxies using three bar classifications: visual inspection, ellipse fitting method and Fourier analysis from a volume-limited sample of 1,698 disk galaxies brighter than Mr=-15.2 within z = 0.01 from the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7). We found two causes to make the discrepancy in previous studies. One is caused by the difficulty in automatically identifying bars for bulge-dominated galaxies. In particular, ellipse fitting methods could miss early-type barred galaxies when a large bulge weakens the transition between a bar and disk. The other is caused by the difference in the correlation between the bar types and host morphology for strong bars and weak bars. Strong bars are preponderant in early-type spirals which are red, bulge-dominated and highly concentrated, whereas weak bars are frequent in late-type spirals which are blue, disk-dominate and less-concentrated. Therefore, how much weak bars they contain affects the trend of bar fraction on host galaxy properties. We also discuss the effect of host properties on the formation, evolution, and destruction of bars.

• 한국정밀공학회:학술대회논문집
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• 한국정밀공학회 2004년도 추계학술대회 논문집
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• pp.261-264
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• 2004

This paper presents the design and test of elliptical vibration assisted cutting tool post. It is actuated by two piezoelectric actuators which are connected to the moving part through the elastic hinge with its role of imposing the preliminary pressures. These two actuators are located at right angles so that the resulting tool tip moves like a two-dimensional ellipse. Also, the tool post is activated within the region of linear actuation in order to overcome the distorted elliptical motion. For the precise measurement of the displacement of the tool tip, three-dimensional experimental apparatus was designed and the strokes of the tool post in major and minor axes were measured. The results show that the tool post can produce the variety of vibration locus from a circle with a radius of 5 ${\mu}{\textrm}{m}$ to an ellipse with a major axis, a =10 ${\mu}{\textrm}{m}$, and a minor axis, b =2.5 ${\mu}{\textrm}{m}$

• 천문학회보
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• 제39권2호
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• pp.70.1-70.1
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• 2014

We analyze a newly discovered galaxy-galaxy scale gravitational lens system, FLS 1718+59 in the Spitzer First Look Survey (FLS) field. A background galaxy (z = 0.245) is severely distorted by a foreground galaxy (z = 0.08), via gravitational lensing. We analyze this system by several methods, including surface brightness fitting (Galfit and Ellipse), gravitational lens modeling (gravlens), and spectral energy distribution fitting (Magphys). From Galfit and Ellipse we measure properties of the lens galaxy, such as the effective radius and the average surface brightness inside it, the ellipticity, and the position angle. gravlens gives us the total mass inside the Einstein radius ($R_{Ein}$), and Magphys provides us an estimate of the stellar mass inside $R_{Ein}$. By comparing these obtained parameters, we confirm that the lens galaxy is an elliptical galaxy on the Fundamental Plane, and calculate the stellar mass function inside $R_{Ein}$, and discuss the implications of the results regarding the initial mass function.

• Journal of Mechanical Science and Technology
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• 제18권1호
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• pp.92-105
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• 2004

A new algorithm for planning a collision-free path based on algebraic curve is developed and the concept of collision-free Path Space (PS) is introduced. This paper presents a Geometry Mapping (GM) based on two straight curves in which the intermediate connection point is organized in elliptic locus ($\delta$, $\theta$). The GM produces two-dimensional PS that is used to create the shortest collision-free path. The elliptic locus of intermediate connection point has a special property in that the total distance between the focus points through a point on ellipse is the same regardless of the location of the intermediate connection point on the ellipse. Since the radial distance, a, represents the total length of the path, the collision-free path can be found as the GM proceeds from $\delta$=0 (the direct path) to $\delta$=$\delta$$\_$max/(the longest path) resulting in the minimum time search. The GM of elliptic workspace (EWS) requires calculation of interference in circumferential direction only. The procedure for GM includes categorization of obstacles to .educe necessary calculation. A GM based on rectangular workspace (RWS) using Cartesian coordinate is also considered to show yet another possible GM. The transformations of PS among Circular Workspace Geometry Mapping (CWS GM) , Elliptic Workspace Geometry Mapping (EWS GM) , and Rectangular Workspace Geometry Mapping (RWS GM), are also considered. The simulations for the EWS GM on various computer systems are carried out to measure performance of algorithm and the results are presented.

• Journal of Magnetics
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• 제16권4호
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• pp.363-367
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• 2011

We have designed, fabricated and demonstrated a novel micro-system for programmable magnetic actuation using magnetic elliptical pathways on Si substrates. Lithographically patterned soft NiFe ellipses are arranged sequentially perpendicular to each other as stepping stones for the transport of magnetic beads. We have measured the magnetization curve of the ellipsoid ($9\;{\mu}m{\times}4\;{\mu}m{\times}0.1\;{\mu}m$) elements with respect to the long and short axes of the ellipse. We found that the magnetization in the long axis direction is larger than that in the short axis direction for an applied field of ${\leq}$ 1,000 Oe, causing a force on carriers that causes them to move from one element to another. We have successfully demonstrated a micro-system for the magnetic actuation of biomolecule carriers of superparamagnetic beads (Dynabead$^{(R)}$ 2.8 ${\mu}m$) by rotating the external magnetic field. This novel concept of magnetic actuation is useful for future integrated lab-on-a-chip systems for biomolecule manipulation, separation and analysis.

• Journal of Radiation Protection and Research
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• 제15권2호
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• pp.51-56
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• 1990

대기로 방출된 방사성 물질의 대기 확산 형태를 파스킬의 대기안정도에 따른 모델인 타원형 근사화 모델로 가정하고 인체가 받을 수 있는 감마선에 의한 피폭선량률을 계산하였다. 이 결과를 대기 확산 기본 모델인 가우스플룸 모델을 적용하여 계산한 결과 및 이미 발표된 원형 근사화 모델에 의한 결과와 비교하여 보았다. 제시한 타원형 근사화 모델을 이용하여 피폭선량을 계산한 결과는 가우스플룸 모델의 결과와 비슷하고, 원형 근사화 모델의 경우보다 오차가 적었으며, 동시에 기본 모델인 가우스 플룸 모델과 비교할 때 1/40 정도의 계산 시간이 걸렸다.

• 한국수자원학회논문집
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• 제41권4호
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• pp.405-412
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• 2008

본 연구에서는 지역빈도해석 기법 중 하나인 FORGEX 기법을 이용하여 확률강우량을 추정하였다. 기존의 원형 네트워크와 1:1.5, 1:2의 비율을 갖는 타원형 네트워크가 한국의 강우자료에 적합한 방법인지를 판단하기 위해 3 가지 경우를 비교 분석하였다. 이 분석을 위해서 남한지역의 376개 지점의 연최대강우자료를 추출하고, 이 자료들을 연최대자료의 중간값으로 표준화하였다. 네트워크는 분석 대상 지점을 중심으로 형성되며, pooled points와 netmax 자료를 각 네트워크에서 매년 추출한다. 그리고 성장곡선(growth curve)을 유도하고 주어진 재현기간에 따른 확률강우량을 추정한다. 지점빈도해석과 지역빈도해석의 대표적인 기법인 홍수지수법(index flood method), FORGEX 기법이 적용되었고, 이를 통해 얻은 결과를 비교 분석하였다. 또한 36개 지점에 원형과 타원형 네트워크를 이용한 FORGEX 기법을 적용하였고, 그 결과를 비교 분석하였다. 결과적으로 대상지점의 지점빈도해석으로 구한 확률강우량과 지역빈도해석으로 구한 확률강우량의 차이가 적을 때 원형과 타원형 네트워크의 추정된 확률강우량의 차이도 적었다. 그러나 지점빈도해석의 결과와 홍수지수법 결과의 차이가 클 때 원형과 타원형 네트워크로 추정된 확률강우량의 차이도 컸다. 타원형 네트워크가 더 많은 지점을 포함할 때, 타원으로부터 추정된 확률강우량 값은 원으로 구해진 값보다 높은 정확도를 보였다. 그리고 타원의 비율이 1:2일 때가 1:1.5보다 홍수지수법으로 구한 확률강우량 값에 가까웠다. 그러므로 1:2 비율의 타원을 적용한 FORGEX 기법이 한국의 지역빈도해석에 적합한 방법이라 할 수 있다.

• 한국농공학회:학술대회논문집
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• 한국농공학회 1998년도 학술발표회 발표논문집
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• pp.419-424
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• 1998

The deduction methods for forced displacement depths caused by sea dike construction often assumed the shape of forced displacements and heaving. To investigate the shape of forced displacements and heaving, a model tests was performed. Results of the tests are as follows; 1) The shape of forced displacements can be assumed ellipse. 2) The shape of heaving can not be assumed uniform shape like a circle and Extents of heaving was varied with the loading height and width. 3) The shape of forced displacements caused by step construction, pebble embankments and soil embankments, also investigated.