• Nuclear Engineering and Technology
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• 제54권6호
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• pp.2204-2212
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• 2022

Recently, the demand for alpha imaging detectors for quantifying the distributions of alpha particles has increased in various fields. This study aims to reconstruct a high-resolution image from an alpha imaging detector by applying a super-spatial resolution method combined with the maximum-likelihood expectation maximization (MLEM) algorithm. To perform the super-spatial resolution method, several images are acquired while slightly moving the detector to predefined positions. Then, a forward model for imaging is established by the system matrix containing the mechanical shifts, subsampling, and measured point-spread function of the imaging system. Using the measured images and system matrix, the MLEM algorithm is implemented, which converges towards a high-resolution image. We evaluated the performance of the proposed method through the Monte Carlo simulations and phantom experiments. The results showed that the super-spatial resolution method was successfully applied to the alpha imaging detector. The spatial resolution of the resultant image was improved by approximately 12% using four images. Overall, the study's outcomes demonstrate the feasibility of the super-spatial resolution method for the alpha imaging detector. Possible applications of the proposed method include high-resolution imaging for alpha particles of in vitro sliced tissue and pre-clinical biologic assessments for targeted alpha therapy.

• 천문학회지
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• 제36권spc1호
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• pp.145-149
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• 2003

LIST is the Lyman-$\alpha$ Imaging Solar Telescope, a project funded by the Korean government to fly on the second Korean Science and Technology research Satellite (STSat-2) due to launch in December 2005. The Principal Investigator is Dr. Minhwan Jang of Kyung-Hee University and of the Space Payload Research Center (SPARC), a consortium of Korean universities and institutions formed to develop scientific research projects in space. The purpose of the LIST project is to design, build, and operate an instrument on STSat-2 which will make images of the Sun from Earth orbit at the wavelength of the Hydrogen Lyman-a emission line at 121.6 nm. LIST has a simple design concept comprised of a small telescope to image the full disk of the Sun onto a CCD detector and a set of filters to isolate the 121.6 nm wavelength.

• 한국방사선학회논문지
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• 제13권4호
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• pp.573-579
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• 2019

환자 피폭선량 관리에 입사표면선량(ESD, entrance surface dose)이 국내외적으로 진단참고준위(국내 흉부촬영 $340{\mu}Gy$)로 사용되고 있지만, ESD측정을 위해서는 선량계가 필요하다. 하지만 대부분 병의원에서는 선량계가 구비되어 있지 않고 정기검사 시 전문 업체 측정에 의해 확인할 수 있다. 따라서 본 연구에서는 흉부 디지털촬영에서 사용자가 쉽게 ESD를 예측할 수 있는 방법에 대해 알아보았다. 흉부 디지털촬영에서 평판형 디텍터(FP, Flat-panel detector)와 IP (Imaging plate detector)를 대상으로 하였고, ESD는 선량계(XI-Platinum, Unfors, Sweden)를 흉부 팬텀(07-646 Duke QC chest phantom, Supertech, Elkhart, USA)의 중앙 표면에 부착시킨 후, 튜브와 디텍터를 180cm 거리를 유지시켜 각 노출조건 조합(관전압과 노출선량)에서 3회 반복측정한 후 평균값을 얻었다. 흉부 팬텀 영상의 다이콤 헤더 정보에서 FP영상은 선량면적곱(DAP, dose-area product)을 확인하였고, IP영상에서는 노출 지수(EI, exposure index)를 확인하였다. 단순선형회귀분석을 통해 FP촬영에서 DAP로부터, IP촬영에서 EI로부터 ESD를 예측할 수 있는 회귀방정식($y={\alpha}+{\beta}X$, ${\alpha}$=직선의 절편, ${\beta}$=직선의 기울기)을 구하였다. FP가 IP 보다 유의하게 낮은 선량을 보였고($85.7{\mu}Gy$ vs. $124.6{\mu}Gy$, p=0.017), 두 디텍터 모두 ESD와 화질 간에 높은 양의 상관성을 보였다. FP에서 수정된 R 제곱(adjusted R2)은 0.978로 ESD의 변동은 DAP 변동에 의해 97.8%의 높은 설명력을 보였다. 단순 회귀식은 $ESD=0.407+68.810{\times}DAP$ 이었다. 위의 회귀식을 이용하여 국내 권고선량($340{\mu}Gy$)과 같은 DAP를 추정한 결과($DAP=0.021+0.014{\times}340{\mu}Gy$), DAP는 4.781 이었다. IP에서 수정된 R 제곱(adjusted R2)은 0.645로 ESD의 변동은 EI 변동에 의해 64.5%의 설명력을 보였다. 단순 회귀식은 $ESD=-63.339+0.188{\times}EI$ 이었다. 위의 회귀식을 이용하여 국내 권고선량($340{\mu}Gy$)과 같은 EI를 추정한 결과($EI=565.431+3.481{\times}340{\mu}Gy$), EI는 1748.97 이었다. 흉부 디지털 촬영에서는 팍스 워크스테이션 영상의 다이콤 헤더 정보에서 ESD를 사용자가 쉽게 예측할 수 있다.

• 한국의학물리학회지:의학물리
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• 제18권3호
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• pp.144-148
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• 2007

최근 국내에서는 원거리에 있는 응급환자에 대한 원격의료서비스를 제공하기 위한 이동형 응급 의료 시스템에 대한 연구가 활발히 진행되고 있다. 본 연구의 목적은 응급구조 차에 탑재 할 수 있는 이동형 디지털 X선 촬영 장치를 구축하고 시스템으로부터 획득한 영상에 대하여 영상 성능평가의 주요인자인 MTF (modulation transfer function), NPS (noise power spectrum) 및 DQE (detective quantum efficiency)를 정량화함으로써 응급상황 시 임상적으로 효용성 있는 영상의 획득 가능성을 평가하는 것이었다. 이동형 X선 장치(Mobix-1000; LISTEM, Wonju, Korea)와 디지털 X선 detector 시스템 (Alpha-R4000; Teleoptic PRA, Kyiv, Ukraine)으로 구축된 영상시스템에 대하여 성능평가를 수행하였다. 측정결과로 10% MTF는 2.4 cycles/mm를 나타내었고, DQE (0)는 조건선량 0.19, 0.5 그리고 1.3 mR에 따라 각각 54%, 55%, 그리고 76%로 측정되었다. 본 연구에서 획득한 영상평가 결과는 연구 중인 이동형 디지털 X선 촬영 장치의 응급 원격 의료에의 사용가치를 확인 할 수 있는 기초자료로서 이용될 수 있을 것으로 판단된다.

• 한국염색가공학회:학술대회논문집
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• 한국염색가공학회 2011년도 제44차 학술발표회
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• pp.63-63
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• 2011

The donor-${\pi}$-acceptor (D-${\pi}$-A) chromophoric dye system has received great attention in variety fields such as electroluminescent materials, sensors and optoelectronic devices. There are many research activities focused on the development for abovementioned application materials with the high-performance properties. In the previous work, we are reported that novel D-${\pi}$-A dye, 2-[4-(9H-carbazol-9-yl)benzylidene]-2,3-dihydroinden-1-one, is successfully attained and exhibited a positive fluorescence solvatochromism. In this work, the molecular structure and packing geometry of 2-[4-(9H-carbazol-9-yl)benzylidene]-2,3-dihydroinden-1-one was discussed by their conformational structure. Their single yellow prism crystal having approximate dimensions of $0.30{\times}0.10{\times}0.10$ mm was carried out with a Rigaku RAXIS RAPID imaging plate area detector with graphite monochromated $CuK_{\alpha}$ radiation. Their crystal structure were solved by using the CrystalStructure crystallographic software package.

• 천문학회보
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• 제35권1호
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• pp.39.2-39.2
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• 2010

In this paper, I present the domestic development of near infrared camera systems for the ground telescope and the space satellite. These systems are the first infrared instruments made for astronomical observation in Korea. KASINICS (KASI Near Infrared Camera System) was developed to be installed on the 1.8m telescope of the Bohyunsan Optical Astronomy Observatory (BOAO) in Korea. KASINICS is equipped with a $512{\times}512$ InSb array enable L band observations as well as J, H, and Ks bands. The field-of-view of the array is $3.3'{\times}3.3'$ with a resolution of 0.39"/pixel. It employs an Offner relay optical system providing a cold stop to eliminate thermal background emission from the telescope structures. From the test observation, limiting magnitudes are J=17.6, H=17.5, Ks=16.1 and L(narrow)=10.0 mag at a signal-to-noise ratio of 10 in an integration time of 100 s. MIRIS (Multi-purpose InfraRed Imaging System) is the main payload of the STSAT-3 in Korea. MIRIS Space Observation Camera (SOC) covers the observation wavelength from $0.9{\mu}m$ to $2.0{\mu}m$ with a wide field of view $3.67^{\circ}{\times}3.67^{\circ}$. The PICNIC HgCdTe detector in a cold box is cooled down below 100K by a micro Stirling cooler of which cooling capacity is 220mW at 77K. MIRIS SOC adopts passive cooling technique to chill the telescope below 200K by pointing to the deep space (3K). The cooling mechanism employs a radiator, a Winston cone baffle, a thermal shield, MLI of 30 layers, and GFRP pipe support in the system. Opto-mechanical analysis was made in order to estimate and compensate possible stresses from the thermal contraction of mounting parts at cryogenic temperatures. Finite Element Analysis (FEA) of mechanical structure was also conducted to ensure safety and stability in launching environments and in orbit. MIRIS SOC will mainly perform the Galactic plane survey with narrow band filters (Pa $\alpha$ and Pa $\alpha$ continuum) and CIB (Cosmic Infrared Background) observation with wide band filters (I and H) driven by a cryogenic stepping motor.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2008년도 한국우주과학회보 제17권2호
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• pp.27.1-27.1
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• 2008

KASI (Korea Astronomy and Space Science Institute) is developing a compact wide-field survey space telescope system, MIRIS (The Multi-purpose IR Imaging System) to be launched in 2010 as the main payload of the Korea Science and Technology Satellite 3. Through recent System Design Review (SDR) and Preliminary Design Review (PDR), most of the system design concept was reviewed and confirmed. The near IR imaging system adopted short F/2 optics for wide field low resolution observation at wavelength band 0.9~2.0 um minimizing the effect of attitude control system. The mechanical system is composed of a cover, baffle, optics, and detector system using a $256\times256$ Teledyne PICNIC FPA providing a $3.67\times3.67$ degree field of view with a pixel scale of 51.6 arcsec. We designed a support system to minimize heat transfer with Muti-Layer Insulation. The electronics of the MIRIS system is composed of 7 boards including DSP, control, SCIF. Particular attention is being paid to develop mission operation scenario for space observation to minimize IR background radiation from the Earth and Sun. The scientific purpose of MIRIS is to survey the Galactic plane in the emission line of Pa$\alpha$ ($1.88{\mu}m$) and to detect the cosmic infrared background (CIB) radiation. The CIB is being suspected to be originated from the first generation stars of the Universe and we will test this hypothesis by comparing the fluctuations in I (0.9~1.2 um) and H (1.2~2.0 um) bands to search the red shifted Lyman cutoff signature.

• 천문학논총
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• 제24권1호
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• pp.53-64
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• 2009

MIRIS is the main payload of the STSAT-3 (Science and Technology Satellite 3) and the first infrared space telescope for astronomical observation in Korea. MIRIS space observation camera (SOC) covers the observation wavelength from $0.9{\mu}m$ to $2.0{\mu}m$ with a wide field of view $3.67^{\circ}\times3.67^{\circ}$. The PICNIC HgCdTe detector in a cold box is cooled down below 100K by a micro Stirling cooler of which cooling capacity is 220mW at 77K. MIRIS SOC adopts passive cooling technique to chill the telescope below 200 K by pointing to the deep space (3K). The cooling mechanism employs a radiator, a Winston cone baffle, a thermal shield, MLI (Multi Layer Insulation) of 30 layers, and GFRP (Glass Fiber Reinforced Plastic) pipe support in the system. Optomechanical analysis was made in order to estimate and compensate possible stresses from the thermal contraction of mounting parts at cryogenic temperatures. Finite Element Analysis (FEA) of mechanical structure was also conducted to ensure safety and stability in launching environments and in orbit. MIRIS SOC will mainly perform Galactic plane survey with narrow band filters (Pa $\alpha$ and Pa $\alpha$ continuum) and CIB (Cosmic Infrared Background) observation with wide band filters (I and H) driven by a cryogenic stepping motor.