• Journal of Astronomy and Space Sciences
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• v.21 no.4
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• pp.493-504
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• 2004

The history books of East Asia about astronomical phenomena have the more records of the solar eclipse frequently than any other ones. It is because traditionally, the solar eclipse moaned the fate of dynasty and the king's rule. The Sun, the biggest thing in the heaven symbolized the king, and the solar eclipse foresaw that the king had the problem in private including the body, and the country might suffer from difficulties in a great scale. So the king and all of the ministers used to gather to hold a ceremony named Gusikrye(구식례) which solar eclipse may pass safely. Consequently, kings always had concernments on collecting informations of solar eclipse. Inspite of importance of solar eclipse predictions, but at the beginning of the Choseon, the predictions of the solar eclipse didn't fit. King Sejong compiled the Chiljeongsan-naepion (칠정산내편) and the Chiljeongsan-oepyeon(칠정산외편) to calculate the celestial phenomena including the solar eclipse. By the publications of these two books, the calendar making system of Choseon was firmly established. The Chiljeongsan-oepyeon adopted Huihui calendar(회회력) of Arabia. The Solar eclipse predictions of Chiljeongsan-oepyeon were relative correct compared to modern method in early Choseon dynasty.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.1
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• pp.58.3-58.3
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• 2017

In a ${\Lambda}CDM$ universe, galaxies are believed to evolve by mergers and accretions. The debris resulting from such processes remains as diffuse, low-surface brightness structures, such as outer disks, stellar halos, and faint companions. These structures will give us fruitful insight into the recent mass assembly history of galaxies, but it is challenging to observe them due to their low surface brightness. In order to explore the structural properties of outskirts of nearby galaxies, we conduct deep wide-field imaging survey with KMTNet. Here we present a progress report of data reduction for the images of NGC 1291, a lenticular barred galaxy with outer rings. To achieve accurate flat fielding, we use dark sky flat and remove the sky gradient of each exposure with a polynomial fit. As a result, we are able to reach 1 sigma depth of ${\mu}_R{\sim}29.6\;mag\;arcsec^{-2}$. We expect to investigate the surface brightness profile of NGC 1291 in 1-D profile, and color-gradient in the outer part of the galaxy using the B- and R-band images.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.2
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• pp.46.2-46.2
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• 2017

We will present a discovery of an elliptical jellyfish galaxy in Abell 2670 (Sheen et al. 2017, ApJL, 840, L7). Our MUSE IFU spectra revealed a rotating gas disk in the center of the galaxy and long ionised gas tails emanating from the disk. Its one-sided tails and a tadpole-like morphology of star-forming blobs around the galaxy suggested that the galaxy is experiencing strong ram-pressure stripping in the cluster environment. Stellar kinematics with stellar absorption lines in the MUSE spectra demonstrated that the galaxy is an elliptical galaxy without any hint of a stellar disk. Then, the primary question would be the origin of the rich gas component in the elliptical galaxy. A plausible scenario is a wet merger with a gas-rich companion. In order to investigate star formation history of the system (the galaxy and star-forming blobs), we derived star-formation rate and metallicity from the MUSE spectra. Photometric UV-Optica-IR SED fitting was also performed using GALEX, SDSS, 2MASS and WISE data, to estimate dust and gas masses in the system. For a better understanding of star formation history and environmental effect of this galaxy, FIR/sub-mm follow-up observations are proposed.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.42.4-43
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• 2018

Most galaxies are believed to evolve through mergers and accretions. In particular, minor mergers and gas accretion appear to play an important role in galaxy evolution in the present-day Universe. Tidally-disrupted debris from such processes remain as diffuse, low-surface brightness structures because the dynamical timescale in the outskirts is significantly longer than that in the central regions. Although these structures will give us useful insight into the mass assembly history of galaxies, it is difficult to detect them due to their faint surface brightness. In order to investigate the structural properties of outskirts in nearby galaxies, we conduct deep and wide-field imaging survey with KMTNet. We present our observing strategy and an optimal data reduction process to recover faint extended features in the images of KMTNet. Using the imaging data of NGC 1291 obtained from KMTNet, we find that a peak-to-peak sky gradient can be reduced less than 0.4-0.6% of the original sky level in the entire image. We also find that we can reach the surface brightness of ${\mu}_{(B,1{\sigma})}$ ~ 29.5, ${\mu}_{(R,1{\sigma})}$ ~ 28.5 mag $arcsec^{-2}$ in one-dimensional profile, that is mainly limited by the uncertainty in the sky determination. It indicates that deep imaging data of KMTNet is suitable to study the extended faint features of nearby galaxies, such as stellar halos, outer disks, and dwarf companions.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.126.1-126.1
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• 2011

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 unique capability of focal plane instruments onboard SPICA, it will enable us to resolve many astronomical key issues from the star-formation history of the universe to the planetary formation. The FPC (Focal Plane Camera) is a Korean-led near-infrared instrument as an international collaboration. Korean consortium for FPC proposed a key instrument responsible for a fine guiding (FPC-G). The back-up of FPC-G will make scientific observations as well. We have examined the legacy science programs for FPC and performed the feasibility study for the fine guiding system. Recently, the international review process is now in progress, in order to make a selection of the focal plane instruments. Here, we report the current status of SPICA/FPC project.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.61.3-61.3
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• 2018

To understand the assembly of the galaxy population in clusters today, it is important to first understand the impact of previous environments prior to cluster infall, namely preprocessing. We use 15 cluster samples from hydrodynamic zoom-in simulation YZiCS to determine the significance of preprocessing focusing primarily on the tidal mass loss of dark matter halos. We find ~48% of the cluster member halos were once satellites of another host. The preprocessed fraction is not a clear function of cluster mass. Instead, we find it is related to each individual cluster's recent mass growth history. We find that the total mass loss is a clear function of time spent in a host. However, two factors can considerably increase the mass loss rate. First, if the satellite mass is approaching the mass of its host. Second, when the halo suffers tidal mass loss at a higher redshift. The preprocessing provides an opportunity for halos to experience tidal mass loss for a more extended period of time than would be possible if they simply fell directly into the cluster, and at earlier epochs when hosts were more destructive to their satellites.

• The Bulletin of The Korean Astronomical Society
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• v.46 no.1
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• pp.39.2-40
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• 2021

본 연구는 《숭전역서》 혹은 《서양신법역서》 이후, 하국종(何國宗, ? -1767)과 매각성(梅殼成, 1681-1764) 등에 의해 기술된 《역상고성》 상하편에 실린 <일전역리>, <일전역법>, <일전표>를 바탕으로 태양의 운동을 자세히 살펴보았다. 《숭전역서》 <일전역리>에서는 티코브라헤의 혼합모형을 기반에 두었지만 태양의 운동은 톨레미(Ptolemy)의 이심모델(Eccentric model)과 차이가 없다. 그러나 <일전표>에 수록된 가감차의 값은 이퀀트모델(Equant model)을 기초로 한 것이었다. 《신법산서》 <일전표>에는 이 모델에 의한 계산법을 소개하고 있으나 계산의 오류를 범하였다. 태양 실측과의 어긋남, 태양의 운동을 기술하는 여러 상수들이 다시 얻어짐에 따라 《역상고성》 상하편의 <일전역리>에서는 코페르니쿠스 모델을 기초로 한 본륜-균륜 모델을 채택하고 있다. 이 모델을 기초로 한 가감차 계산 과정에 조금의 수학적 오류가 있지만 계산 결과에는 영향을 미치지 않았다. 그리고 <일전표>에 제시된 가감차값은 바로 이 모델을 기반으로 한 값들이다. <일전역법>에 제시된 동지 이후 태양의 실제 경도를 구하는 방법이 매우 구체적이다. 이 방법은 이후 《역상고성후편》의 <일전역법>도 그대로 따르고 있는데 다만 《역상고성후편》의 <일전역리>는 케플러의 타원모델을 채택하고 있다. 태양의 황경을 구하는 현재의 방법과 비교해보면 《역상고성》 <일전역법>에서는 그 기준이 동지이고 현재의 방법은 춘분점이라는 것만 다를 뿐이고, 방법은 동일하다. 다만 필요한 상수 값들이 시간에 따라 아주 느리게 변하기에 이 값들의 보정이 필요할 뿐이다. 이 방법은 조선에서 집필된 《세초류휘》, 《시헌기요》, 《추보속해》, 《추보첩례》에도 사용한 모델과 상수들은 다르지만 동일한 방법을 요약하고 있다.

• Journal for History of Mathematics
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• v.36 no.2
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• pp.21-34
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• 2023

Spherical trigonometry refers to the geometry related to spherical triangles. It has been an important tool for studying astronomy since ancient times. In trigonometry, concepts such as trigonometric functions naturally emerge from the relationship between arcs and chords of a circle. In this paper, we briefly examine the origin of spherical trigonometry. To introduce the basics of spherical trigonometry, we present fundamental and important theorems such as Menelaus's theorem, the law of sines and the law of cosines on a sphere, along with their proofs. Furthermore, we discuss the educational value and potential applications of spherical trigonometry.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.2
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• pp.45.1-45.1
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• 2016

우리나라 대부분의 과학관에는 천문시설이 갖추어져 있고, 천문분야 전시와 교육이 어느 정도는 이루어지고 있다. 하지만 자연사박물관에서는 천문분야가 주요 분야로 인정받고 있지 못하고 그 내용도 빈약한 편이다. 수도권에서 매우 중요한 역할을 하고, 연간 35만 명 정도의 관람객이 방문하고 있는 서대문자연사박물관에도 일부 천문 전시가 있긴 하지만 다른 분야에 비해 매우 빈약하다. 자연의 역사를 다루는 자연사박물관에서 우주의 탄생으로 보여주는 천문학은 중요한 역할을 차지할 여지가 있고, 실제 해외 유명 자연사박물관에서는 천문 분야가 큰 비중을 차지하고 있다. 국립자연사박물관의 건설도 추진되고 있는 상황에서 자연사박물관에서의 천문전시와 교육이 어떤 방향으로 이루어져야 할지 논의해 보았으면 한다.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.1
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• pp.41.1-41.1
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• 2014

Although the link between activity in the nuclei of galaxy and galactic mergers has been under scrutiny for several years, it is still unclear to what extent and for which populations of active galaxies merger-triggered activity is relevant. The environment of AGN allows an indirect probe of the past merger history and future merger probability of these systems, suffering less from sensitivity issues while extending to higher redshifts, compared to traditional morphological studies of AGN host galaxies. Here we present results from our investigation of the environment of radio selected sources out to redshift z=2. We employ the first data release J-band catalog from the new near-IR Infrared Medium-Deep Survey (IMS) and 1.4 GHz radio data from the Faint Images of the Radio Sky at Twenty-cm (FIRST) survey and a deep dedicated VLA survey of the VIMOS field, covering a combined total of ~20 sq. degrees. Given the flux limit of the combined radio catalog (0.1 mJy), we probe a radio luminosity range of 10^36-10^44 erg/s. Using the second and fifth closest neighbor density parameters, we test whether active galaxies inhabit denser environments and study these overdensities in terms of both distance to the AGN and its luminosity. We find evidence for a sub-population of radio-selected AGN that resides in significantly overdense environments at small scales, although we do not find significant overdensities for the bulk of our sample. We do not recover any dependence between the AGN radio-luminosity and overdensities. We show that radio-AGN inhabiting the most underdense environments in the field have vigorous ongoing star formation. We interpret these results in terms of the triggering and fuelling mechanism of radio-AGN.