• Fisheries and Aquatic Sciences
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• 제1권2호
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• pp.201-208
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• 1998

A protease, which had no tryptic and chymotryptic activity, was purified from the hepatopancreas of shrimp, P. japonicus, through ammonium sulfate fractionation, Q­Sepharose ionic exchange, benzamidine Sepharose 6B affinity, and Sephacryl S-100 gel chromatography. Molecular weight (M.W.) of the protease was estimated to be 24 kDa by gel filtration and showed a single peptide band by sodium dodecylsulfate polyacrylamide gel electrophoresis (SDS-PAGE). The protease had a low ratio of acidic to basic amino acids, which is different with pro teases from marine animals. The enzyme was partially inhibited by benzamidine, tosyl-L-lysine chioromethyl ketone (TLCK), phenylmethylsulfonyl fluoride (PMSF), soybean trypsin inhibitor (SBTI), and pepstatin. The enzyme did not have any activity against benzoyl-D,L-arginine p-nitroanilide (BAPNA) or benzoyl-L-tyrosine ethyl ester (BTEE) which is a specific substrate of trypsin and chymotrypsin, respectively. However, the enzyme showed activity forward N-CBZ-L-tyrosine p-nitrophenyl ester (CBZ-Tyr-pNE), N­CBZ-L-tryptophan p-nitrophenyl ester (CBZ-Trp-pNE), and N-CBZ-L-proline p-nitrophenyl ester (CBZ-Pro-pNE). The protease did not showed tryptic and chymotryptic activity, which was not reported in shrimp hepatopancreas.

• Journal of Astronomy and Space Sciences
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• 제34권4호
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• pp.303-314
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• 2017

With increased human activity in space, the risk of re-entry and collision between space objects is constantly increasing. Hence, the need for space situational awareness (SSA) programs has been acknowledged by many experienced space agencies. Optical and radar sensors, which enable the surveillance and tracking of space objects, are the most important technical components of SSA systems. In particular, combinations of radar systems and optical sensor networks play an outstanding role in SSA programs. At present, Korea operates the optical wide field patrol network (OWL-Net), the only optical system for tracking space objects. However, due to their dependence on weather conditions and observation time, it is not reasonable to use optical systems alone for SSA initiatives, as they have limited operational availability. Therefore, the strategies for developing radar systems should be considered for an efficient SSA system using currently available technology. The purpose of this paper is to analyze the performance of a radar system in detecting and tracking space objects. With the radar system investigated, the minimum sensitivity is defined as detection of a $1-m^2$ radar cross section (RCS) at an altitude of 2,000 km, with operating frequencies in the L, S, C, X or Ku-band. The results of power budget analysis showed that the maximum detection range of 2,000 km, which includes the low earth orbit (LEO) environment, can be achieved with a transmission power of 900 kW, transmit and receive antenna gains of 40 dB and 43 dB, respectively, a pulse width of 2 ms, and a signal processing gain of 13.3 dB, at a frequency of 1.3 GHz. We defined the key parameters of the radar following a performance analysis of the system. This research can thus provide guidelines for the conceptual design of radar systems for national SSA initiatives.

• 한국진공학회지
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• 제7권s1호
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• pp.15-19
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• 1998

Structural and optical properties of $In_xGa_{1-X}N$ as well as $In_{0.1}Ga_{0.9}N$/GaN single quantum we11 (SQW) grown on sapphire (0001) substrate with an based GaN using rf-plasma assisted MBE have been investigated. The quality of the InXGal.,N fdm was improved as the growth temperature increased. In PL measurements at low temperatures, the band edge emission peaks of $In_xGa_{1-X}N$ was shifted to red region as an indium cell and substrate temperature increased. For $In_{0.1}Ga_{0.9}N$/GaN SQW, the optical emission energy has blue shift about 15meV in PL peak, due to the confined energy level in the well region. And, the FWHM of the $In_{0.1}Ga_{0.9}N$/GaN SQW was larger than that of the bulk Ino,la.9N films. The broadening of FWHM can be explained either as non-uniformity of Indium composition or the potential fluctuation in the well region. Photoconductivity (PC) decay measurement reveals that the optical transition lifetimes of the SQW measured gradually increased with temperatures.

• 천문학회지
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• 제50권5호
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• pp.139-149
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• 2017

The Korea Astronomy and Space Science Institute plans to develop a coronagraph in collaboration with National Aeronautics and Space Administration (NASA) and to install it on the International Space Station (ISS). The coronagraph is an externally occulted one-stage coronagraph with a field of view from 3 to 15 solar radii. The observation wavelength is approximately 400 nm, where strong Fraunhofer absorption lines from the photosphere experience thermal broadening and Doppler shift through scattering by coronal electrons. Photometric filter observations around this band enable the estimation of 2D electron temperature and electron velocity distribution in the corona. Together with a high time cadence (<12 min) of corona images used to determine the geometric and kinematic parameters of coronal mass ejections, the coronagraph will yield the spatial distribution of electron density by measuring the polarized brightness. For the purpose of technical demonstration, we intend to observe the total solar eclipse in August 2017 with the filter system and to perform a stratospheric balloon experiment in 2019 with the engineering model of the coronagraph. The coronagraph is planned to be installed on the ISS in 2021 for addressing a number of questions (e.g., coronal heating and solar wind acceleration) that are both fundamental and practically important in the physics of the solar corona and of the heliosphere.

• 한국전자파학회논문지
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• 제23권11호
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• pp.1297-1306
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• 2012

본 논문에서는 77 GHz 차량용 레이더 시스템에 필요한 레이더 송신기를 설계하였다. 130 nm RF CMOS 공정을 이용하여 설계한 13 GHz 주파수 합성기로 6 체배기를 내장한 상용의 화합물 전력 증폭기를 구동하여 77 GHz 송신 신호를 발생시켰다. 13 GHz 주파수 합성기는 6 체배용 전력 증폭기를 구동하기 위해 4 dBm 출력을 내는 주입 잠금 버퍼를 내장하고 있다. 제작한 77 GHz 레이더 송신기 모듈은 주파수 조정 범위 내에서 출력 전력이 최소 13.99 dBm이고, 중심 주파수 대비 기준 스퍼의 크기는 -36.45 dBc이다. 또한, 76.5 GHz 중심 주파수의 1 MHz 오프셋에서 -81 dBc/Hz의 위상 잡음 특성을 보인다.

• 전기전자학회논문지
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• 제7권2호
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• pp.223-229
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• 2003

본 논문에서는 2.4GHz와 5.8GHz 대역의 무선 랜카드에 사용되는 듀얼 역-F형 내부 안테나의 설계 값에 따른 안테나 특성을 분석하였다. 노트북용 WLAN card의 PCB 기판에 인쇄된 형태로 설계하여 안테나의 길이, 단락 스터브의 두께, 피드선과 단락 스터브 사이의 간격, 안테나와 접지면 사이의 간격, 안테나의 두께 및 기판의 두께와 기판의 유전율에 따른 특성 변화를 연구하였다. 설계 값에 따른 특성변화 그래프로부터 설계 값을 튜닝하여 최적의 안테나를 설계하였다. 설계된 안테나는 VSWR이 1.6과 1.14이며, 주파수 대역폭은 170MHz와 500MHz 이며, 최대이득 3.5dBi 의 값을 얻었다.

• 천문학회보
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• 제37권2호
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• pp.141.1-141.1
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• 2012

CIBER (Cosmic Infrared Background ExpeRiment) is a sounding-rocket borne experiment which is designed to find the evidence of the First stars (Pop.III stars) in the universe. They are expected to be formed between the recombination era at z ~ 1100 and the most distant quasar (z ~ 8). They have never been directly detected due to its faintness so far, but can be observed as a background radiation at around $1{\mu}m$ which is called the Cosmic Near-Infrared Background (CNB). The CIBER is successfully launched on July 10, 2010 at White Sands Missile Range, New Mexico, USA. It consists of three kinds of instruments. One of them is a LRS (Low Resolution Spectrometer) which is a refractive telescope of 5.5 cm aperture with spectral resolution of 20 ~ 30 and wavelength coverage of 0.7 to $2.0{\mu}m$ to measure the spectrum of the CNB. Since LRS detects not only CNB but also stellar components, we can study their spectral features with the broad band advantage especially at around $1{\mu}m$ which is difficult at ground observations because of the atmospheric absorption by water vapor. I identified around 300 stars from observed six fields. If we can classify their spectral types with SED fitting, we can study their physical conditions of the stellar atmosphere as well as making a stellar catalogue of continuous stellar spectrum.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2010년도 한국우주과학회보 제19권1호
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• pp.40.3-40.3
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• 2010

The most frequently suggested source for Pi2 pulsations in the inner magnetosphere (L < 4) is standing fast-mode waves trapped in the plasmasphere (i.e., plasmaspheric resonances). They have been considered as the source of low-latitude Pi2 pulsations. The plasmaspheric resonance model suggests that compressional fast-mode waves can be detected at all local times inside the plasmasphere provided reflection of the wave energy is efficient. Until now, however, there are no reports about compressional Pi2s observed in the dayside inner magnetosphere. That is, there is longitudinal limit of inner magnetosphere. In February 2008, THEMIS probes were near dawn and/or dusk sides, which are the transition regions between the nightside and dayside, in the inner magnetosphere (L = 2-4) when low-altitude Pi2s were identified at Bohyun (L = 1.35) station in Korea. Using the THEMIS electric field data, we examined if Pi2s are excited by longitudinally localized disturbances. We found that compressional Pi2s having high coherence with a low-latitude Pi2 pulsation occur on dawnside. However, any compressional pulsations in the Pi2 frequency band were not detected on duskside. This indicates that compressional Pi2s disappear near the duskside. Our observations are discussed with spatial plasmaspheric structure and possible Pi2 mechanisms.

• 한국진공학회:학술대회논문집
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• 한국진공학회 2013년도 제45회 하계 정기학술대회 초록집
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• pp.245.2-245.2
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• 2013

Solution processed organic photovoltaic devices have relatively less attention compared to polymer photovoltaic devices even though they have high possibility to be developed because they have both advantages of polymer and organic, such as solution processable, no synthetic batch dependence of photovoltaic performance, high purity and high charge carrier mobility as well as relatively high efficiency (~7%). In addition, solution processed organic photovoltaic devices have an advantage of easiness to study the relationship between the molecular structure and photovoltaic performance due to its simple structure. In this work, five isoindigo based low band gap donor-acceptor-donor (D-A-D) small molecules with different electron donating strength were synthesized for investigating the relationship between the molecular structure and photovoltaic performance, especially, investigating the effects of different electron donating effect of donor group in isoindigo backbone to photovoltaic device performance. The variation of electron donating strength of donor group strongly affected the optical, thermal, electrochemical and photovoltaic device performances of isoindigo organic materials. The highest power conversion efficiency of ~3.2% was realized in bulk heterojuction photovoltaic device consisted of the ID3T as donor and PC70BM as acceptor. This work demonstrates the great potential of isoindigo moieties as electron deficient units as well as guideline for synthesis of donor-acceptor-donor (D-A-D) small molecules for realizing highly efficient solution processed organic photovoltaic devices.

• 한국진공학회:학술대회논문집
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• 한국진공학회 2013년도 제45회 하계 정기학술대회 초록집
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• pp.231-231
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• 2013

ZnO은 hexagonal wurtzite 구조를 갖는 직접 천이형 화합물 반도체로서, 상온에서 3.37 eV 정도의 wide band gap energy를 가지고 있으며, 60 meV의 큰 엑시톤 결합 에너지(exciton binding energy)를 갖는다. 또한 동종 기판이 존재하고 열, 화학적으로 안정한 상태이며 습식 식각이 가능한 장점으로 인해 각광받고 있다. 또한, ZnO 박막은 우수한 전기 전도성을 나타내며 광학적 투명도가 우수하기 때문에 투명전극으로 많이 이용되어 왔고, 태양 전지(solar cell), 가스 센서, 압전소자 등 많은 분야에서 사용되고 있다. 이와 같은 ZnO박막을 안정적인 쇼트키 다이오드 특성을 얻기 위해서는 쇼트키 배리어 장벽의 형성이 필수적이다. Mg을 ZnO에 첨가하여 MgZnO 박막을 형성할 경우, 금속의 일함수와 MgZnO의 전자친화력 차이가 증가하여 더 큰 쇼트키 장벽 형성이 가능하며, 금속의 일함수가 큰 물질을 사용해야 한다. 또한, 박막의 결함이 적은 박막을 형성해야 하는 에피탁셜 박막이 필요하다. SiC는 높은 포화 전자 드리프트 속도(${\sim}2.7{\times}107$ cm/s), 높은 절연 파괴전압(~3 MV/cm)과 높은 열전도율(~5.0W/cm) 특징을 가지고 있으며, MgZnO/Al2O3의 격자 불일치는 ~19%인 반면에 MgZnO/SiC의 격자 불일치는 ~6%를 가진다. 금속의 일함수가 큰 Ag 금속은 열처리가 될 경우 AgOx가 될 경우 더욱 안정적인 쇼트키 장벽을 형성될 수 있을 것으로 판단된다. 본 연구에서는 쇼트키 접합을 형성하기 위해 금속의 일함수가 큰 Ag 금속을 사용하였으며, Al2O3 기판과 6H-SiC 기판위에 MgZnO(30 at.%) 박막을 증착하였다. 증착 후에 Ag를 증착 한 뒤 급속 열처리를 하였다. 열처리된 MgZnO의 경우 열처리 하지않은 소자보다 약 $10^5$ 이상의 우수한 on/off 특성을 보였다.