• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 1998년도 한국우주과학회보 제7권1호
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• pp.26.2-26
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• 1998

No Abstract.See Full-text

• 천문학논총
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• 제15권spc1호
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• pp.119-126
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• 2000

The BOES (BOAO Echelle Spectrograph), a fiber-fed echelle spectrograph of the BOAO 1.8 m telescope, has been designed and now is being manufactured. The BOES follows a white pupil design collimated with two off-axis parabolic mirrors. The 136mm collimating beam leaving the 41.59 grooves/mm R4 echelle grating is refocused near the narrow folding mirror. Through the two cross-disperser prisms and $\phi250 mm(f/1.5)$ transmission camera, the beam images on EEV $2k\times4k$ CCD. The BOES can take the wavelength range of 3700 to $10100{\AA}$ at a single spot with spectral resolution R = 20000 to 40000 depending on the fiber set employed. We describe the key sciences and performance, current status of construction, and future plan of the BOES.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2000년도 한국우주과학회보 제9권2호
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• pp.54-54
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• 2000

No Abstract, See Full Text

• 한국공간구조학회논문집
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• 제16권2호
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• pp.47-54
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• 2016

It is very important to calculate natural frequency of the observatory tower correctly because it is keenly affected by wind response vibration due to its large slenderness ratio, weight and small damping ratio. Additionally, suggestion equation of natural frequency being used in the design phase has considerable difference between actual measured value thereby making it inappropriate to be used in the serviceability design of the observatory tower. Therefore, this paper conducted an ambient vibration measuring on 10 observatory towers through mobile-phone application thereby calculating the natural frequency and comparing the result with the domestic and foreign standards and that of the eigen-value analysis. This paper suggested approximate equation of the natural frequency of the observatory tower; T=0.0266H. The square of the corelation coefficient is 0.940, which is high.

• 천문학회보
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• 제25권1호
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• pp.54-54
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• 2000

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2003년도 한국우주과학회보 제12권2호
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• pp.41-41
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• 2003

Satellite formation flying is currently an active area of research in the aerospace engineering. There are many categories for this research such as the determination of initial conditions, formation keeping, configuration and reconfiguration. In this study, a tracking controller using sliding mode techniques is designed to control a satellite for the satellite formation flying. In general, Hill's equations are used to describe the relative motion of the follower satellite with respect to the leader satellite. But, the modified Hill's equations considering J2 perturbation were used for the design of sliding mode controller. Sliding mode control law causes the chattering phenomenon because it is a discontinuous control. Dead-zone was used to avoid the chattering. The Extended Kalman filter was applied to estimate the state vector based on the measurements of relative distance and velocity between two satellites.

• Journal of Astronomy and Space Sciences
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• 제14권2호
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• pp.259-268
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• 1997

천문대에서 개발 중에 있는 CCD를 사용한 극미 광 영상장비의 시험모델 개발과 현재까지의 결과를 논의하였다. 고도의 저 잡음 도와 안정성이 요구되는 천문관측용 극미 광 영상장비는 자외선에서 가시 광 및 근 적외선 영역에 이르기까지 매우 넓은 파장영역에서 관측을 수행할 수 있는 장비로서 여러 분야에 널리 사용되고 있다. 그러나 현재가지 국내에서는 이 장비의 핵심부분인 controller의 자체설계 기술이 확보되어 있지 않은 실정이다. 이 연구에서 개발된 시스템의 전자 부는 한 개의 EPLD(Erasable Programable Logic Device)에 구현된 controller와, 그 외에 analog driver, video processor로 이루어져 있으며 CCD의 암잡음을 줄이기 위한 방법으로 액체질소 냉각방식을 사용하고 있다. 전체적인 제어와 자료처리는 범용성을 고려하여 개인용 컴퓨터(PC)를 이용하였다. 액체질소 냉각용 cryostat와 CCD 소자를 제외한 대부분이 자체 설계제작 되어진 이 시스템으로 실험실과 소백산천문대에서 시험영상을 얻는데 성공하였다.

• 천문학논총
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• 제19권1호
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• pp.65-70
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• 2004

An imaging spectrograph concept optimized for extended far-ultraviolet emission sources is presented. Although the design was originally developed for FIMS aboard the first Korean science satellite STSAT-l launched on September 27, 2003, no rigorous theoretical background of the spectrograph design has been published. The spectrograph design employs an off-axis parabolic cylinder mirror in front of a slit that guides lights to a diffraction grating. The concave grating provides moderate spatial resolution over a large field of view. This mapping capability is absent in most astronomical instruments but is crucial to the understanding of the nature of a variety of astrophysical phenomena. The aberration theory presented in this paper can be extended to holographic gratings in order to improve the spatial as well as the spectral resolutions.

• Journal of Ecology and Environment
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• 제47권4호
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• pp.187-192
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• 2023

The United States (US) National Science Foundation's (NSF's) National Ecological Observatory Network (NEON) is a continental-scale observation facility, constructed and operated by Battelle, that collects long-term ecological data to better understand and forecast how US ecosystems are changing. All data and samples are collected using standardized methods at 81 field sites across the US and are freely and openly available through the NEON data portal, application programming interface (API), and the NEON Biorepository. NSF led a decade-long design process with the research community, including numerous workshops to inform the key features of NEON, culminating in a formal final design review with an expert panel in 2009. The NEON construction phase began in 2012 and was completed in May 2019, when the observatory began the full operations phase. Full operations are defined as all 81 NEON sites completely built and fully operational, with data being collected using instrumented and observational methods. The intent of the NSF is for NEON operations to continue over a 30-year period. Each challenge encountered, problem solved, and risk realized on NEON offers up lessons learned for constructing and operating distributed ecological data collection infrastructure and data networks. NEON's construction phase included offices, labs, towers, aquatic instrumentation, terrestrial sampling plots, permits, development and testing of the instrumentation and associated cyberinfrastructure, and the development of community-supported collection plans. Although colocation of some sites with existing research sites and use of mostly "off the shelf" instrumentation was part of the design, successful completion of the construction phase required the development of new technologies and software for collecting and processing the hundreds of samples and 5.6 billion data records a day produced across NEON. Continued operation of NEON involves reexamining the decisions made in the past and using the input of the scientific community to evolve, upgrade, and improve data collection and resiliency at the field sites. Successes to date include improvements in flexibility and resilience for aquatic infrastructure designs, improved engagement with the scientific community that uses NEON data, and enhanced methods to deal with obsolescence of the instrumentation and infrastructure across the observatory.

• 전자공학회논문지D
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• 제36D2호
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• pp.20-30
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• 1999

85-115GHz 주파수 범위의 100GHz 대역과 125-175GHz 주파수 범위를 갖는 150GHz 대역을 동시에 관측하기 위한 헤테로다인 방식의 이중채널 수신기에 사용될 단측파대 여파기의 이론을 제시하고 이를 근거로 설계, 제작한 후 성능을 측정하였다. 여파기의 이론은 편파 회전 특성을 갖는 Martin-Puplett 간섭계의 원리를 도입하여 전개하였다. 설계와 제작은 빔의 전송손실을 최소화하고 중간주파수와 관련된 경로차를 고려하여 두 빔의 결합 손실을 최소화하는데 주안점을 두었다. 두 주파수 대역을 동시에 관측하기 위해서는 우주전파가 각각 다른 빔의 경로로 전송되어야 하므로 두 개의 단측파대 여파기가 각각 제작되었다. 주파수에 따른 여파기의 이론적인 최적 경로차와 중간주파수 및 대역폭을 계산하였다. 네트웍 분석기와 자체에서 제작한 빔 측정장치를 이용하여 여파기의 성능을 측정하고 이론치와 비교하였다. 주파수에 따른 최적 경로차에 대한 이론치와 측정치를 비교해 본 결과 거의 일치하는 특성을 보여 제시된 설계 이론의 타당성과 정밀한 제작이 검증되었고, 두 대역 여파기의 이미지 제거비는 약 22dB이상을 갖는 우수한 성능을 보였다. 제작된 여파기는 이중채널 수신기에 설치되어 우주전파를 성공적으로 관측함으로서 그 성능이 입증되었다.