• 천문학회보
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• 제42권1호
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• pp.39.3-39.3
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• 2017

To see scientific potential of MIRIS Paschen-${\alpha}$ ($Pa{\alpha}$) Galactic Plane Survey (MIPAPS), we have selected a portion, Galactic longitude from $+96^{\circ}$ to $116^{\circ}$, and inspected $Pa{\alpha}$ detections for 212 sources in WISE H II region catalog. We also list up $35Pa{\alpha}$ large features and $32Pa{\alpha}$ point-like blobs, which have not been cataloged in WISE catalog. For all the sources, we have performed the photometry of $Pa{\alpha}$ emission line, and obtained their $Pa{\alpha}$ intensities and $Pa{\alpha}$ fluxes. For the quantitative comparison, we also make the $H{\alpha}$ mosaic image of the same region by using IPHAS data which have been globally calibrated and released recently. Comparing MIPAPS $Pa{\alpha}$ fluxes with the IPHAS $H{\alpha}$ fluxes enables us to estimate dust extinction and spectral types of ionizing sources. We present the results for some sources.

• 한국컴퓨터그래픽스학회논문지
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• 제6권1호
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• pp.37-50
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• 2000

본 논문에서는 R. T. Farouki에 의하여 소개된 평면 곡선들에 대한 복소수화된 표현법을 사용하여 주어진 임의의 평면 다항식 곡선을 복소수 계수를 갖는 한 다항식으로 나타내고 이 식을 대수학의 기본정리에 따라 복소수체 상에서 완전히 인수분해한 다음 그 근들을 관찰하여 주어진 곡선이 평면 다항식 피타고리안 호도그라프(PH) 곡선이 되기 위하 필요충분 조건을 새로운 방법으로 밝히고, 이를 3차원 민코브스키 공간 $R^{2,1}$ 상의 다항식 곡선에 적용, 이 곡선이 PH 곡선이 되기 위한 필요충분을 보다 간결한 형태로 나타내고 이를 통하여 3차원 민코브스키 공간 $R^{2,1}$ 상의 가능한 다항식 PH 곡선들의 유형이 모두 결정된다는 것을 보인다.

• Architectural research
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• 제13권3호
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• pp.19-29
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• 2011

Visibility of a space have been defined in several different ways: such as the axial line covering a convex space, a convex space defining the fattest shape in a space and an Isovist field formed by a field of vision at a given vantage point. Isovist fields are referred to as a descriptive medium to describe a movement by reviewing and analyzing geometric properties in them. Many descriptive methods for analysis of three-dimensional isovist are applied to analyzing the morphological properties in a 3D space more realistically. Although these models are regarded as a more advanced method for describing spatial properties, they have pros and cons such as complex mathematical calculations and somewhat arbitrary calibration in addition to huge consumption of memory space. These difficulties lead to the development of a three-dimensional visual accessibility model that explores the implication of building shape on the calculation of isovist fields drawn on a 2D plane. We propose a conceptual framework of how to measure the isovist field not as a 3D volume but as a combination of 2D plane on the ground with the 3D building shape of it's facade.

• 천문학회보
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• 제38권1호
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• pp.76.2-76.2
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• 2013

SPICA(SPace Infrared Telescope for Cosmology and Astrophysics) is an infrared space observatory with cooled telescope of 3 m aperture. Because of its large aperture, near- and mid-infrared instruments onboard SPICA require fine guidance with attitude accuracy less than 0.1 arcsecond. The FPC-G is a focal plane camera to achieve this high attitude accuracy and KASI is leading its development. The SPICA project is now under the Risk Mitigation Phase 2 (RMP2) and one of major risks is to satisfy the requirement of pointing and attitude control. To assess the impacts of disturbance sources on the attitude control and devise methods to mitigate possible risks, a software simulator of the FPC-G is under the development. In this presentation, we report the status of development of the simulator and the development plan during the RMP2.

• 천문학논총
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• 제22권4호
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• pp.201-209
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• 2007

We have preliminarily designed two infrared optical systems of the multi-purpose infrared camera system (MIRIS) which is the main payload of STSAT-3. Each optical system consists of a Cassegrain telescope, a field lens and a 1:1 re-imaging lens system that is essential for providing a cold stop. The Cassegrain telescope is identical for both of two infrared cameras, but the field correction lens and re-imaging lens system are different from each other because of different bands of wavelength. The effective aperture size is 100mm in diameter and the focal ratio is f/5. The total length of the optical system is 300mm and the position of the cold stop is 25mm from the detector focal plane. The RMS spot size is smaller than $40{\mu}m$ over the whole detector plane.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2008년도 한국우주과학회보 제17권2호
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• pp.23.4-23.4
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• 2008

In March and April 2001, the apogee (~9 Re) of the Polar spacecraft was located near the subsolar magnetopause with its orbital plane nearly parallel to a magnetic meridian plane. Polar electric and magnetic field data acquired during the two-month interval of solar maximum have been used to study fundamental standing Alfven waves near the subsolar meridian plane (magnetic local time = 1000-1400 hours) at magnetic latitudes from the equator to $\pm45$ degrees and at L values between 7 and 12. In the frequency band from 1.5 to 10 mHz, fundamental mode oscillations were identified based on high coherence (more than 0.7) and an approximately 90-degree phase shift between the azimuthal magnetic and radial electric field components. The L dependence of the fundamental frequencies is studied, and the frequencies are compared with those observed near the solar minimum interval (Takahashi et al. 2001). We found that the average frequencies in solar maximum are lower than those in solar minimum by a factor of ~2. This implies that the mass density in solar maximum is higher than that in solar minimum by a factor of ~4. Since there is a positive correlation between solar irradiance and solar activity, we suggest that the ionosphere in solar maximum produces more ions and load magnetic flux tubes with more ions.

• 정보처리학회논문지:소프트웨어 및 데이터공학
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• 제4권10호
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• pp.465-472
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• 2015

본 논문에서는 시차공간상의 평면검출 방법을 제안하고 그 성능을 평가한다. 다양한 표면을 평면으로 근사하고 검출함으로써 시차공간에 나타난 장면을 간소화하고 수식화하여 다루기 쉽도록 한다. 또한 시차공간에서 근사적으로 구한 평면은 3차원 공간상에서 실측 크기로 표현 가능하고 장애물 검출 및 카메라 위치 추정에 활용할 수 있다. 먼저 스테레오 매칭 기술을 이용해 두 개의 영상으로부터 2차원 공간상에 좌표쌍마다 시차값을 가지는 시차공간을 생성한다. x 또는 y축의 전체적인 추이를 반영하도록 돕는 선 단순화 기법을 이용하여 시차값의 접선 기울기를 추정한다. 기울기 쌍의 조합에 따라 10개의 라벨을 시차공간의 좌표쌍에 부여한다. 상하좌우 방향으로 인접하고 동일한 라벨을 가지는 좌표쌍을 연결하여 군집을 생성하고 최소자승법을 이용해 각 군집에 대한 평면식을 추정한다. 시차공간 내에서 평면식을 만족하는 점들이 가장 많은 평면을 검출하고 이를 시차공간을 가장 잘 간소화한 N개의 평면으로 선택한다. 평면검출의 성능을 정량적으로 평가하였고 그 결과는 3차원 원뿔과 원통에서 각각 97.9%, 86.6% 품질을 보였다. 스테레오 비전 알고리즘의 성능을 평가하기 위해 대표적으로 이용되는 Middlebury와 KITTI 실험데이터로부터 제안된 평면검출 방법은 훌륭하게 평면을 검출하였다.

• 한국산학기술학회논문지
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• 제19권5호
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• pp.89-97
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• 2018

과거 병원은 치료만 목적으로 하여 최소한의 공용공간을 확보하여 계획되었지만, 현대 병원은 치유환경의 중요성이 높아지면서 공용공간이 늘어나고, 환자와 보호자와 의료진을 고려하여 계획된다. 또한 로비형태가 홀형에서 발전하여 스트리트형이나 컨코스형으로 계획되면서 공용면적이 증가했다. 과거병원과 다르게 접수, 대기, 수속공간에서 발전하여 현대병원은 상업,취미,문화공간으로 사용된다. 본 연구의 목적은 종합병원의 치유환경 요소를 선행연구에서 도출하여 치유환경 평가방법을 분석의 틀로 세워, 병원 로비공간의 치유환경을 로비 평면형태를 중심으로 분석, 평가한다. 병원 로비는 여러 행위가 이루어지는 중요한 공간으로, 병원 로비 평면타입별 각 3개의 사례를 비교분석한다. 연구의 결과로 스트리트형이 홀형보다 로비치유환경이 더 좋은 것으로 나타났지만 접근성, 옥상정원, 휴게공간의 분석결과는 비슷하다. 이는 사례대상이 대형종합병원이기에 충분한 공간이 계획되어 로비형태와 크게 관련 없는 요소로 사료된다. 스트리트형 중에서도 아트리움이 선형인 사례가 4면형 아트리움보다 오픈체적비가 크기에 로비의 공간감과 자연채광 유입효과가 크다. 또 로비평면이 홀형일 때, 단면이 중정형이면 오픈체적비가 큰 것을 보아 로비의 평면 형태도 중요하지만, 단면형태도 중요한 것으로 분석된다.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2010년도 한국우주과학회보 제19권1호
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• pp.26.4-27
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• 2010

The main payload of STSAT-3 (Science and Technology Satellite 3), MIRIS (Multipurpose InfraRed Imaging System) is the first Korean infrared space mission to explore the near-infrared sky with a small astronomical instrument, which is being developed by KASI. The 8-cm passively cooled telescope with a wide field of view (3.67 deg. $\times$ 3.67 deg.) will be operated in the wavelength range from 0.9 to $2{\mu}m$. It will carry out wide field imaging and the emission line survey. The main purposes of MIRIS are to perform the Cosmic Infrared Background (CIB) observation at two wide spectral bands (I and H band) and to survey the Galactic plane at $1.88{\mu}m$ wavelength, the Paschen-$\alpha$ emission line. CIB observation enables us to reveal the nature of degreescale CIB fluctuation detected by the IRTS (Infrared Telescope in Space) mission and to measure the absolute CIB level. The Pashen-$\alpha$ emission line survey of Galactic plane helps us to understand the origin of Warm Ionized Medium (WIM) and to find the physical properties of interstellar turbulence related to star formation. Here, we also discuss the observation plan with MIRIS.

• 천문학회보
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• 제37권2호
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• pp.97.2-97.2
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• 2012

The main payload of Science and Technology Satellite 3 (STSAT-3), Multipurpose InfraRed Imaging System (MIRIS) is the first Korean infrared space mission to explore the near-infrared sky with a small astronomical instrument developed by KASI. The 8-cm passively cooled telescope with a wide field of view (3.67 deg. ${\times}$ 3.67 deg.) will be operated in the wavelength range from 0.9 to $2{\mu}m$. It will carry out wide-band imaging and the Paschen-${\alpha}$ emission line survey. After the calibration of MIRIS in our laboratory, MIRIS has been delivered to SaTReC and successfully assembled into the STSAT-3. The main purposes of MIRIS are to perform the observation of Cosmic Infrared Background (CIB) at two wide spectral bands (I and H band) and to survey the Galactic plane at $1.88{\mu}m$ wavelength, the Paschen-${\alpha}$ emission line. CIB observation enables us to reveal the nature of degree-scale CIB fluctuation detected by the IRTS (Infrared Telescope in Space) mission and to measure the absolute CIB level. The MIRIS will continuously monitor the seasonal variation of the zodiacal light towards the both north and south ecliptic poles for the purpose of calibration as well as the effective removal of zodiacal light. The Pashen-${\alpha}$ emission line survey of Galactic plane helps us to understand the origin of Warm Ionized Medium (WIM) and to find the physical properties of interstellar turbulence related to star formation. Here, we also discuss the observation plan with MIRIS.