• 천문학회지
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• 제52권2호
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• pp.49-55
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• 2019

The New Vacuum Solar Telescope (NVST) is the largest solar telescope in China. When using CCDs for imaging, equal-thickness fringes caused by thin-film interference can occur. Such fringes reduce the quality of NVST data but cannot be removed using standard flat fielding. In this paper, a correction method based on multi-scale decomposition and adaptive partitioning is proposed. The original image is decomposed into several sub-scales by multi-scale decomposition. The region containing fringes is found and divided by an adaptive partitioning method. The interference fringes are then filtered by a frequency-domain Gaussian filter on every partitioned image. Our analysis shows that this method can effectively remove the interference fringes from a solar image while preserving useful information.

• 천문학회보
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• 제44권1호
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• pp.58.1-58.1
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• 2019

Gravitational-wave (GW) sources for the next decades would be in majority binaries consisting of neutron stars and/or black holes reside in the extragalactic environment. For example, GW170817 was the first extragalactic neutron star - neutron star binary found by GW observations and it was proved the power of multi-messenger astronomy (MMA) including the KMTNet observations. With the ever increased sensitivity, the $3^{rd}$ observation run (O3) led by the advanced LIGO and advanced Virgo this year aims to search for more 'standard' populations as well as 'exotic' ones expected by stellar evolution. I will present highlights of on-going efforts by researchers in Korea and those in abroad for estimating physical parameters of a source. Mass, spin, distance, and location are prerequisite information to constrain theoretical understanding of the source formation and evolution. Furthermore, these information are to be shared with the international community for follow-up multi-messenger observations. I will present the observational accuracy expected for the future GW observations and discuss their implications. If time allows, I will make a few remarks on prospects of O3 with KAGRA collaborations, which many domestic researchers are closely involved in.

• 천문학회보
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• 제43권2호
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• pp.41.3-42
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• 2018

Redshift space distortion (RSD) is known as a powerful cosmological probe. The large-scale RSD has been detected by various redshift surveys and continues to be a major target of ongoing surveys. On the other hand, the small-scale RSD, called finger-of-god (FoG) effect, also has cosmological information, because different cosmological parameters cause different halo mass functions and viriarized velocities. We define the "length" of FoG and examine its dependence on cosmological parameters using the Multiverse simulation. We also use the SDSS DR7 data to see how strong constraints current data sets could provide. It is found that the volume-limited subsample D5, consisting of ~100,000 galaxies at z~0.08, yields $\Delta \Omega_m ~ 0.02$.

• 한국정보통신학회논문지
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• 제21권4호
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• pp.846-854
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• 2017

본 논문에서는 과거부터 사용되고 있는 천측 기법을 현대의 IT기술과 접목시켜, 컴파스의 오차를 줄일 수 있는 방안을 제안하였다. 천측을 이용하여 진북을 추출할 수 있는 알고리즘을 정리하여, 이를 적용할 수 있도록 엔코더와 방위환을 결합하고, 각종 표시기 및 연산을 위해 임베디드 시스템을 설계하여 이를 구현하였다. 그 결과 약 $0.2^{\circ}$ 정도의 오차로 진북을 추출할 수 있었을 뿐만 아니라, 기존에 천측을 통해 대략 5분 이상 소요되던 시간적 불편함도 편의적인 분석과 함께 5초 미만으로 줄일 수 있음을 알 수 있었다. 특히 기존 자이로컴파스의 오차는 물론 IMO의 방위 기준 등을 분석하여 이들의 허용 오차가 $0.5^{\circ}$ 이하라는 것을 제시하여, 본 논문의 결과가 실제 적용에서 각종 컴파스의 오차를 줄일 수 있는 가치 있는 결과임을 확인할 수 있었다.

• 정보관리연구
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• 제39권4호
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• pp.155-171
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• 2008

한국천문연구원의 지역천문대인 보현산천문대, 소백산천문대, 레몬산천문대의 관측자료 활용을 용이하게 해주는 통합관리 시스템을 구축하였다. 관측자료는 생산된 천문대 각각에 아카이브로 보관하며, 통합시스템에는 관측자료에 관한 MySQL 테이블만 저장한다. 지역천문대와 통합시스템에는 각각 관리자가 있어 자료의 보관 및 헤더정보 추출, 테이블 생성 및 웹 페이지 관리 등을 역할 분담하여 수행한다. 사용자는 통합시스템의 웹 검색페이지 한곳에서 모든 천문대의 관측자료를 검색할 수 있으며 다운로드 또한 검색결과 페이지에서 가능하다. 통합시스템에서 독립된 각각의 천문대 아카이브로 쿼리를 보내 검색하는 방식은 가상천문대의 기본개념과 동일하다. 이와 같이 본 연구는 국제가상천문대 사업에 참여하는 한국가상천문대 구축 작업의 일환이기도 하다.

• 천문학논총
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• 제19권1호
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• pp.101-107
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• 2004

This paper describes the digital back-end system for getting the data to analyze the user observation mode by digitalize the analog data after receiving the space radio using the radio telescope, The received analog data will be digitalized by high-speed sampler with 1 Gsps for 4 channel frequency band of millimeter wave, and the digital data will be transported through the fiber-optic digital transmission system and WDM(wavelength division multiplex) to observation building, The wideband digital FIR(Finite Impulse Response) filters analyze the data for user observation mode to record the data in high-speed recorder with 1 Gbps. In this paper, we introduce the overall system configuration and features combined by various information and communication technology in radio astronomy briefly, which will be adopted by KVN(Korean VLBI Network).

• 대한지구과학교육학회지
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• 제5권1호
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• pp.1-7
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• 2012

The purpose of this study was to restore So-ganui(小簡儀), which is a unique astronomical instrument during Sejong period, so that its educational application can be sought. To achieve it, researcher researched the observation principle of our ancestors and the structure of So-ganui, and then restored So-ganui. The result is as following. First, So-ganui is the astronomical observation instrument which can not only measure the position of the celestial bodies in terms of function but also find out the height and distance of topography, and get the time. Second, restoration So-ganui is suitable for the students to learn as an inquiry activity of the observation information in the science curriculum and it would be used as the learning materials for the proper understanding of the science and measurement principle of our ancestors. This study would contribute to raising the level of pride in our scientific culture for the students and succeed the heritage of the science and culture.

• 천문학논총
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• 제30권2호
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• pp.709-711
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• 2015

In modern Astronomy the vernal equinoctial (VE) point is taken as the starting point for measuring celestial longitudes. Due to the precession of equinoxes, the above point is receding back along the ecliptic. As a result, the longitudes of fixed stars are increasing every year. In ancient India, the Hindu astronomers did not favour the idea of fixed stars changing their longitudes. In order to stabilize the zodiac, they had taken as the origin a point which is fixed on the ecliptic and as such is quite different from the VE point. This initial point being a fixed one, the longitude of stars measured from this origin remain invariable for all time. There was an epoch in the past when this initial point coincided with the VE point and thus the epoch may be called the zero-year. There is controversy over the determination of the zero-year. The reasons for the choice for the fixed zodiacal system by the Hindu astronomers as well as the epoch of zero-year have been found out on the basis of information available in various astronomical treatises of ancient India written in Sanskrit.

• 천문학회보
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• 제44권1호
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• pp.63.1-63.1
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• 2019

Solar system small bodies are unusual objects in astronomical survey data in that they are moving on the celestial sphere. In addition, even in a normal status, their magnitudes are changing over time, firstly because their relative positions with respect to the Sun and Earth are continually changing, secondly because they are rotating bodies with non-spherical shapes. Furthermore, some of them might exhibit unexpected activities, which could be caused by mass ejection or disintegration. Detections and observations of such activities are challenging due to their abrupt nature. Therefore, continuous monitoring observations of large number of Solar system small bodies are required to systematically obtain detailed/transient information about them. Since 2018/2019 winter, we have launched a new project using Korea Microlensing Telescope Network (KMTNet) for detecting such transient phenomena of Solar system objects. Our main goal is to monitor the magnitudes and detect sudden brightness changes. We also plan to discover interesting new objects, and monitor rotational brightness oscillations of asteroids. We intend to monitor the magnitudes of ~ 20,000 known Solar system small bodies per night, and acquire lightcurves of ~ 1,000 asteroids.

• 천문학회보
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• 제40권1호
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• pp.61.3-62
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• 2015

Remote-sensing observation is one of the observation methods that provide valuable information, such as composition and surface physical conditions of solar system objects. The Hayabusa spacecraft succeeded in the first sample returning from a near-Earth asteroid, (25143) Itokawa. It has established a ground truth technique to connect between ordinary chondrite meteorites and S-type asteroids. One of the scientific observation instruments that Hayabusa carried, Asteroid Multi-band Imaging Camera(AMICA) has seven optical-near infrared filters (ul, b, v, w, x, p, and zs), taking more than 1400 images of Itokawa during the rendezvous phase. The reflectance of planetary body can provide valuable information of the surface properties, such as the optical aspect of asteroid surface at near zero phase angle (i.e. Sun-asteroid-observer's angle is nearly zero), light scattering on the surface, and surface roughness. However, only little information of the phase angle dependences of the reflectance of the asteroid is known so far. In this study, we investigated the phase angle dependences of Itokawa's surface to understand the surface properties in the solar phase angle of $0^{\circ}-40^{\circ}$ using AMICA images. About 700 images at the Hayabusa rendezvous phase were used for this study. In addition, we compared our result with those of several photometry models, Minnaert model, Lommel-Seeliger model, and Hapke model. At this conference, we focus on the AMICA's v-band data to compare with previous ground-based observation researches.