• 천문학회보
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• 제34권2호
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• pp.54.1-54.1
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• 2009

• 천문학회보
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• 제34권1호
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• pp.191.2-191.2
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• 2009

• 천문학회보
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• 제34권1호
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• pp.152.2-152.2
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• 2009

• 천문학회보
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• 제34권1호
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• pp.71.2-71.2
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• 2009

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2009년도 한국우주과학회보 제18권1호
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• pp.57.2-57.2
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• 2009

• 대순사상논총
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• 제34집
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• pp.1-26
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• 2020

九天應元雷聲普化天尊在臺灣道教中, 被奉為雷部至上之神 ; 在韓國大巡真理會中, 卻是其宗教信仰的至上神。而九天應元雷聲普化天尊也因為在兩個宗教中具有相同名稱, 不禁讓人想知道, 在不同宗教卻出現相同名稱的神祇, 兩者之間是否指的是同一位神?亦或是兩者之間是否具有一定的關聯性?九天應元雷聲普化天尊在兩個宗教中, 所負含的意義為何?諸如此類的相關問題, 有必要先進行基礎性的釐清。而宗教經典即是釐清基礎性問題的基石。宗教經典對於具有該宗教情愫的人而言, 通常具有一定的神聖性, 權威性與教化性, 這些宗教經典的特性, 經常可由經典中人物的話語或經文字句中看出端倪, 因此, 本文亦試圖從兩宗教的經典中開始著手研究。本文從韓國大巡真理會與道教正一派的兩部關於「九天應元雷聲普化天尊」之經典 《典經》 與 《玉樞寶經》 著手, 探究兩部經典中, 解析 關於九天應元雷聲普化天尊, 在兩部經典中的神聖形象, 權威形象與教化形象, 並對九天應元雷聲普化天尊在兩部經典中的形象進行比較, 試圖探究兩者異同性。本文基於釐清「九天應元雷聲普化天尊在兩宗教中的異同」的終極目標下, 於本文中先進行第一步的經典分析探究。本文內容大致分為四大部分, 第一部分為, 探究兩部經典的內涵, 包含經典的由來, 內涵與價值。第二部分為, 兩部經典中九天應元雷聲普化天尊之三種經典形象, 包含神聖形象, 權為形象與教化形象。第三部分為, 兩部經典中九天應元雷聲普化天尊之三種經典形象比較。最後, 以兩教間的發展演化, 歷史關係, 為兩部經典中的九天應元雷聲普化天尊之存在價值做些許論述。

• 천문학회보
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• 제41권2호
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• pp.31.2-31.2
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• 2016

We present our study of the correlation between the UV luminosity and the merging activities of nearby galaxies (d < 300 Mpc). Our study uses ~600 UV-selected galaxies with deep optical imaging data, where the UV selection is made using the GALEX Atlas of Galaxies (Gil de Paz et al. 2007) and the updated UV catalog of nearby galaxies (Yu Bai et al. 2015). Deep optical images allow us to classify merger features using visual inspection, and we also estimate unobscured SFR using UV continuum luminosity. The fraction of galaxies with merger features in each UV luminosity bins are obtained to see if how the fraction of galaxies with merging features changes as a function of UV luminosity, Finally, we will show, above what UV luminosity (or SFR), the merging mechanism becomes an important process in enhancing star formation of galaxies.

• 천문학회보
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• 제35권2호
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• pp.35.2-35.2
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• 2010

It is crucial to understand the dust properties in the early universe since they provide important clues about how the early cosmic star formation should be interpreted in the presence of dust extinction. GRB 071025 is an unusually red GRB that occured at high redshift, offering an unique opportunity to study the dust properties in the early universe. We investigate the extinction properties of GRB 071025 through the analysis of RIJHK data obtained with the 1-m telescope at Mt. Lemmon Optical Astronomy Observatory (LOAO) and Simultaneous Quad Infrared Imaging Device (SQIID) on the Kitt-Peak Mayall 4-m telescope. Our dataset is independent from that in a previous work (Perley et al. 2010) where a small systematic photometric errors could complicate the interpretation. After determining the temporal power law exponent with five I-band frames from LOAO, we construct a multi-band monochromatic SED of the GRB afterglow. By using various extinction laws, we find that the SED is best fitted with models that incorporate SNe II dust and derive a photometric redshift of 4.99(+0.12/-0.03). Our results strongly support the prior claim that dusts in GRB 071025 originate mainly from supernovae, implying SNe II predominantly contributed to the dust enrichment in the early universe (z ~ 5).

• 천문학회보
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• 제43권1호
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• pp.37.4-38
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• 2018

The HULQ project proposes to use gravitational lensing to determine the masses of QSO host galaxies, an otherwise difficult goal. If these host galaxy masses, along with their SMBH masses from single-epoch measurements, are estimated for a substantial number of QSOs at various redshifts, the co-evolution of SMBHs and their host galaxies can be studied for a large portion of the history of the universe. To determine the feasibility of this study, we present how to estimate the number of sources lensed by QSO hosts, i.e. the number of lensing QSO host galaxies (hereafter QSO lenses). SMBH masses in the literature are transformed into the velocity dispersions of their host galaxies using the M_BH -sigma relation, and in turn the Einstein radii for each QSO -source redshift combination is calculated, assuming singular isothermal spherical mass distributions. Using QSOs and galaxies as potential sources, the probability of a QSO host galaxy being a QSO lens is calculated, as a function of limiting magnitude. The expected numbers of QSO lenses are estimated for ongoing and future wide-imaging surveys, and the Hyper Suprime-Cam Wide survey is illustrated as an example.

• 천문학회보
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• 제41권1호
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• pp.70.2-70.2
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• 2016

Star formation in galaxies is one of the key factors in galaxy evolution. It is believed that star formation is triggered and enhanced by mergers among galaxies or secular evolution. However, how much these two mechanisms contribute on star formation is not well known yet. Recently, many other studies show observational evidences of faint merger features(tidal tails, stellar streams) around nearby galaxies with deep optical imaging. This study aims to investigate the fraction of star forming galaxies exhibiting faint features to total galaxies. We are analyzing samples of 76 star forming galaxies (NUV < -18) to find merger features from stacked B, R band frames taken at Maidanak 1.5m, McDonald 2.1m telescope and g, r frames from Canada-France-Hawaii Telescope (CFHT) MegaCam archival data. With the fraction, we can expect to know the contribution of mergers on star formation to galaxies.