• Journal of Astronomy and Space Sciences
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• 제15권2호
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• pp.373-389
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• 1998

천문대 X-선 연구팀에서는 3년의 연구기간 동안(1995 - 1997)천체 X-선 관측시스템을 자체개발 하였다. 이 관측 시스템은 한국 항공우주연구소에서 개발된 2단 과학로켓에 탑재되어, 1998년 6월 11일 오전 10시(KST) 태안의 한 발사 장에서 발사되었다. 이 실험의 목적은 X-선 관측 시스템의 성능시험과 X-선 배경복사 관측으로 설정되었다. 로켓은 성공적으로 발사되었고, 발사 후 약 140초 동안 각종 데이터들을 지상 국으로 전송하였다. 수신된 데이터들을 분석한 결과 X-선 관측시스템은 최종 도달고도에 이르기까지 정상적으로 동작하지 못하였음을 알 수 있었다. X-선 검출기부는 발사 후 약 32초까지 그리고 신호 처리부는 발사 후 약 55.7초까지 정상적인 동작을 하였다. 이 연구에서는 55.7초까지의 데이터들을 바탕으로 X-선 관측시스템에 대한 기능점검을 수행하였으며, 이에 대한 결과를 보고하고 시스템의 오 동작 원인에 대한 토의를 하였다.

• 천문학회보
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• 제35권1호
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• pp.39.1-39.1
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• 2010

We are developing a CCD camera named CQUEAN (Camera for Quasars in Early Universe) to search for quasars at z > 7. CQUEAN has a 1024*1024 deep depletion CCD chip and will be attached to 2.1m Otto-Struve Telescope at McDonald Observatory, USA. Although commercial software for the CCD camera is provided by the vendor, we are going to develop our own software to control the other instruments as well, to carry out efficient observation. There are four major parts in our software: Instrument control part controls the camera and filter wheel to obtain imaging data. Quick look window is to display acquired imaging data for quick inspection. Telescope control part interfaces with Telescope Control System (TCS) to move the telescope and to get time or coordinate information. Finally, Observation scripting facility part carries out a series of short exposures in a batch. The whole software will be written in python on linux platform, using the instrument control software libraries provided by the vendors.

• 천문학회보
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• 제35권2호
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• pp.56.2-56.2
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• 2010

The SPICA (SPace Infrared Telescope for Cosmology & Astrophysics) project is a next-generation astronomical mission optimized for mid- and far-infrared observation with a cryogenically cooled 3m-class telescope. Due to its high angular resolution and unprecedented sensitivity, SPICA will enable us to resolve many key issues in the present-day astronomy. As an international collaboration, KASI proposed the near-infrared instrument which is composed of two parts; (1) science observation with the capability of imaging and spectroscopy covering $0.7{\mu}m$ to $5{\mu}m$ (FPC-S) (2) fine guiding to stabilize and improve the attitude (FPC-G). Here, we introduce the science programs proposed for SPICA/FPC-S.

• 대기
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• 제29권4호
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• pp.439-450
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• 2019

Present weather plays an important role not only for atmospheric sciences but also for public welfare and road safety. While the widely used state-of-the-art visibility and present weather sensor yields present weather, a single type of measurement is far from perfect to replace long history of human-eye based observation. Truly automatic present weather observation enables us to increase spatial resolution by an order of magnitude with existing facilities in Korea. 8 years of human-eyed present weather records in 19 sites over Korea are compared with visibility sensors and auxiliary measurements, such as humidity of AWS. As clear condition agrees with high probability, next best categories follow fog, rain, snow, mist, haze and drizzle in comparison with human-eyed observation. Fog, mist and haze are often confused due to nature of machine sensing visibility. Such ambiguous weather conditions are improved with empirically induced criteria in combination with visibility and humidity. Differences between instrument manufacturers are also found indicating nonstandard present weather decision. Analysis shows manufacturer dependent present weather differences are induced by manufacturer's own algorithms, not by visibility measurement. Accuracies of present weather for haze, mist, and fog are all improved by 61.5%, 44.9%, and 26.9% respectively. The result shows that automatic present weather sensing is feasible for operational purpose with minimal human interactions if appropriate algorithm is applied. Further study is ongoing for impact of different sensing types between manufacturers for both visibility and present weather data.

• 한국광학회지
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• 제11권1호
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• pp.6-12
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• 2000

위성에 탑재된 지구관측용 카메라는, 지상의 망원경과 같은 원리로, 우주상공에서 지표면 관측을 자동적으로 수행하고 관측정보를 지상으로 전달해 주는 장치다. 이용 목적에 따라 카메라의 해상도 또는 분해능, 관측대역, 관측폭, 위성의 궤도 등의 규격이 결정된다. 고해상도는 카메라 관련 제반 기술 및 경험이 부족한 국내의 여건에 적합한 소형 위성용 고해상도 카메라의 규격을 제시하며 이에 따른 광학 설계와 제작, 조립 및 측정오차를 제시한다.

• 천문학회보
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• 제38권2호
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• pp.82.1-82.1
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• 2013

The SPICA (SPace Infrared Telescope for Cosmology & Astrophysics) project is a next-generation infrared space telescope optimized for mid- and far-infrared observation with a cryogenically cooled 3m-class telescope. Owing to unprecedented sensitivity and high spatial resolution, the focal plane instruments are expected to perform the confusion-limited observation. The SPICA will challenge to reveal many astronomical key issues from the star-formation history of the universe to the planetary formation. The Korean 5contribution to SPICA as an international collaboration is the development of the near-infrared instrument, FPC (Focal Plane Camera). The Korean consortium for FPC proposed a key system instrument for the purpose of a fine guiding (FPC-G) complementing the AOCS (Attitude and Orbit Control System). The back-up instrument of FPC-G, FPC-S will be responsible for the scientific observations as well. Through the international review process, we have revised the scientific programs and made the feasibility study for the fine guiding system. Here, we report the current status of SPICA/FPC project.

• 지구물리와물리탐사
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• 제16권2호
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• pp.91-96
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• 2013

이 연구는 탐사 중 흔들리는 측정기기의 기울어짐을 2축 경사계와 GNSS 나침반으로 보정하는 방법에 관한 연구이다. 3성분 자력탐사와 같이 벡터로 측정하는 경우에는 관측 장비의 이동, 기울어짐, 요동 등에 따라 기울어진 관측 좌표계 위에서 측정된다. 이 측정값들을 측지 좌표계 위의 값으로 바꾸기 위해서는 측정면의 회전각이 필요하다. 이 논문에서는 2축 경사계로 얻은 두 방향의 경사각과 GNSS 나침반으로 얻은 방위각을 이용하여 관측 좌표면의 경사를 얻은 후, 이것을 회전 변환에 직접 쓰이는 성분각으로 변환할 수 있도록 유도하였다. 이 연구에서 개발한 2축 경사계와 GNSS 나침반을 이용하여 측지 좌표계로 변환하는 방법을 이용하여 실제로 배 위에서 측정한 3성분 자력 탐사 값을 측지 좌표계로 변환하였다.

• 우주기술과 응용
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• 제4권2호
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• pp.105-120
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• 2024

현대 천문학에서의 대형 기기 개발은 많은 자원과 인력이 소모되기 때문에 시스템 엔지니어링 및 프로젝트 관리 능력은 현장에서 필수적인 역량이다. 우리는 관측 가능한 실습용 분광기를 제작하고 관측하여 시스템 엔지니어링 경험을 쌓을 수 있는 학부 교육프로그램을 제안한다. 한국천문연구원의 우주인력양성사업의 일환으로 충남대에서 진행된 파일럿 프로그램은 '창의천문기기 개발 및 관측'이라는 가칭으로 총 24명의 학생들이 수강하였으며, 5개 조에서 분광기를 만들어 태양, 달, 별 등의 스펙트럼을 측정하고 연구를 진행하였다. 학생들의 기기 개발과정은 수차례의 리뷰회의를 통하여 가이드 되었으며 개발과정과 문서화된 결과를 통해 성적을 배분하였다. 기기개발 학생들은 이 기회를 통해 시스템 엔지니어링의 기본 원리뿐 아니라 프로젝트 매니지먼트, 광학설계, 기계설계 등에 대해 전반적으로 익힐 수 있었다.

• Ocean and Polar Research
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• 제35권3호
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• pp.229-237
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• 2013

We measured two-dimensional (2-D) oxygen distribution in the surface sediment layer of intertidal sediment using a simple and inexpensive planar oxygen optode, which is based on a color ratiometric image approach. The recorded emission intensity of red color luminophore light significantly changed with oxygen concentration by $O_2$ quenching of platinum(II)octaethylporphyrin (PtOEP). The ratios between the intensity of red and green emissions with oxygen concentration variation demonstrated the Stern-Volmer relationship. The 2-D oxygen distribution image showed microtopographic structure, diffusivity boundary layer and burrow in surface sediment layer. The oxygen penetration depth (OPD) was about 2 mm and the one-dimensional vertical diffusive oxygen uptake (DOU) was 12.6 mmol $m^{-2}d^{-1}$ in the undisturbed surface sediment layer. However, those were enhanced near burrow by benthic fauna, and the OPD was two times deeper and DOU was increased by 34%. The simple and inexpensive oxygen planar optode has great application potential in the study of oxygen dynamics with high spatiotemporal resolution, in benthic boundary layers.

• Journal of Astronomy and Space Sciences
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• 제34권1호
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• pp.45-54
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• 2017

This study examines the scale unique instruments used for astronomical observation during the Joseon dynasty. The Small Simplified Armillary Sphere (小簡儀, So-ganui) and the Sun-and-Stars Time-Determining Instrument (日星定時儀, Ilseong-jeongsi-ui) are minimized astronomical instruments, which can be characterized, respectively, as an observational instrument and a clock, and were influenced by the Simplified Armilla (簡儀, Jianyi) of the Yuan dynasty. These two instruments were equipped with several rings, and the rings of one were similar both in size and in scale to those of the other. Using the classic method of drawing the scale on the circumference of a ring, we analyze the scales of the Small Simplified Armillary Sphere and the Sun-and-Stars Time-Determining Instrument. Like the scale feature of the Simplified Armilla, we find that these two instruments selected the specific circumference which can be drawn by two kinds of scales. If Joseon's astronomical instruments is applied by the dual scale drawing on one circumference, we suggest that 3.14 was used as the ratio of the circumference of circle, not 3 like China, when the ring's size was calculated in that time. From the size of Hundred-interval disk of the extant Simplified Sundial in Korea, we make a conclusion that the three rings' diameter of the Sun-and-Stars Time-Determining Instrument described in the Sejiong Sillok (世宗實錄, Veritable Records of the King Sejong) refers to that of the middle circle of every ring, not the outer circle. As analyzing the degree of 28 lunar lodges (lunar mansions) in the equator written by Chiljeongsan-naepyeon (七政算內篇, the Inner Volume of Calculation of the Motions of the Seven Celestial Determinants), we also obtain the result that the scale of the Celestial-circumference-degree in the Small Simplified Armillary Sphere was made with a scale error about 0.1 du in root mean square (RMS).