• Publications of The Korean Astronomical Society
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• v.29 no.3
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• pp.53-58
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• 2014

We improved the antenna efficiency of the Taeduk Radio Astronomy Observatory (TRAO) 13.7-m radio telescope by adjusting the antenna panels based on digital photogrammetric measurements. First of all, we measured the surface accuracy of the main reflector of this antenna at three elevation angles of $35^{\circ}$, $45^{\circ}$, and $60^{\circ}$. We performed a total of four sets of the photogrammetric measurements and panel adjustments. When adjusting the panels, we positioned the antenna to the zenith and applied the measured data sets at the elevation of $45^{\circ}$. We found that the antenna surface accuracy has been improved by a factor of ~ 3 times after the final adjustment in comparison with the value before the adjustments. And we also found that the antenna surface accuracy tended to be slightly better at the elevation angles of $35^{\circ}$ and $60^{\circ}$ than that at the elevation angle of $45^{\circ}$. After the final panel adjustment, the aperture and beam efficiencies of the telescope have has been improved from 35% to 44%, and from 41% to 51%, respectively.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.1
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• pp.77.1-77.1
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• 2013

WouldYouLike[우주:라이크]는 연세대학교 천문우주학과와 생활디자인과 학생들을 중심으로 천문우주학 대중화를 위해 활동하는 단체이다. 비영리 학생 단체인 만큼 학생들 스스로가 학습한 내용을 직접 요약하고 이를 바탕으로 일반 대중들이 쉽게 접하고 읽을 수 있는 천문우주학 콘텐츠를 제작하는 것을 목표로 하고 있다. 지난 해 봄 약 500여명의 연세대와 이화여대 학생들에게 시행한 관련 설문조사를 시작으로 6월과 12월에 약 30여 페이지 분량의 천문우주관련 소식을 담은 잡지를 발간하였다. 창간호 1300여부와 2호 550부는 연세대를 중심으로 주변 대학교에 배부되었으며 SNS를 이용한 온라인 버전도 약 1900여명의 사람들에게 공개되었다. 천문우주과학의 최신 소식을 전하고 천체사진을 찍는 방법을 소개하는 등 대중의 관심을 끌 내용부터 명왕성의 행성 직위 박탁, 천문대 탐방, IAU 탐방 등 다양한 관련 내용을 담았다. 현재는 3호를 제작중이며 4월말 발간을 목표로 하고 있다. 여기서는 지금까지의 활동 및 앞으로의 계획을 소개하고 천문우주학 전공자들의 의견을 받아 추후의 활동에 반영할 수 있도록 한다.

• The Journal of the Korea institute of electronic communication sciences
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• v.12 no.6
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• pp.1009-1018
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• 2017

We developed new Digital Sampler for KVN(: Korean VLBI Network). The sampler has 1024MHz sampling frequency with 2bits/sample. The sampler's input reference frequencies are 1pps(: pulse per second) and 10MHz, also UTC(: Universal Time Coordinated) time information out with 1PPS signal, synchronized. The output of sampling data is adapted VSI(: VLBI Standard Interface) specification including the time information. In order to confirm the performance of the sampler, we carried out the astronomical radio observation test in Ulsan Radio Observatory of KVN. It was confirmed the stable performance. In this paper, We introduce the new developed sampler and present the observational test result.

• Journal of the Korean earth science society
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• v.38 no.1
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• pp.1-10
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• 2017

The symbiotic star AG Peg is a nebulous binary system that consists of giant star (GS) and white dwarf (WD). We investigated the HI Balmer emission lines of the symbiotic nova AG Peg, observed in 1998, 2001, and 2002 at Lick Observatory. The $H{\alpha}$ and $H{\beta}$ line profiles consist of blue-shifted, red-shifted, and broad components of which intensities and width showed notable changes. The HI emission line profiles that represent the kinematics of the gaseous nebula appear to be mainly from an accretion disk in relatively large radius from the WD. Considering the line of an observer's sight, both GS and WD are located at the sky plane side by side during the 1998 observation, while the WD is in front of GS during 2002 but the WD in rear during 2001. Such a relative position and the spectral line intensity variation imply that a fairly constant outflow occurs into WD from GS which caused to maintain the rotating thick accretion disk structure responsible for the observed spectral lines.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.1
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• pp.60.1-60.1
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• 2016

태양과 같은 별의 형성기작은 질량이 큰 별의 형성기작에 비해 비교적 잘 연구되어 왔다고는 하지만, 이 또한 온전한 이해와는 거리가 먼 상황이며 여전히 논란의 대상이다. IRAS, Spitzer와 같은 적외선우주망원경으로 얻어진 원시성의 광도함수는 일반적으로 받아들여졌던 별탄생 이론으로 설명되지 못한다는 것이 밝혀졌고, 이에 새로운 별탄생 이론이 필요하게 되었다. 새롭게 받아들여지고 있는 별탄생 모델은 Episodic Accretion 모델로서, 원시행성계원반에서 원시성으로 질량 강착이 간헐적이면서 폭발적으로 일어난다는 것이다. 이러한 모델의 관측적 증거의 하나는 FU Orionis와 같은 천체로서, T-Tauri 단계에 있는 원시성이 본래의 밝기보다 약 100배, 즉 가시광에서 5등급 이상 폭발적으로 밝아진 천체이다. 질량강착의 과정은 행성형성의 초기조건을 결정하는 원시행성계원반의 물리적, 화학적 특성을 결정하므로, 그 이해가 중요하다. 따라서 본 연구팀은 Episodic Accretion이 원시행성계원반과 원시항성풍의 형성과 진화에 어떤 역할을 하는지 연구하기 위하여, 보현산 천문대의 고분산 분광기인 BOES를 이용하여, 최근에 폭발을 일으킨 원시성인 HBC 722와 2MASS J06593158-0405277을 모니터링 관측을 해왔으며, 이전에 알려진 6개의 FU Orionis 형 천체들도 관측하였다. 여기서는 그 결과를 발표하고자 한다.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.1
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• pp.87-87
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• 2014

조선 전기 세종(世宗, 1418-1450)에 의해 천체관측기기와 천문역법을 개발하는 사업이 있었다. 이 때 조선의 천문대인 간의대가 건설되었고, 더불어 소간의, 일성정시의, 현주일구, 천평일구, 정남일구, 앙부일구 등 다수의 소형화된 천문의기가 개발되었다. 이보다 앞서 중국 원(元)왕조의 최신 관측기기였던 간의, 규표, 혼천의, 혼상 등을 제작하였는데, 이 과정에서 습득한 기술적 경험을 바탕으로 소형화된 천문의기 새롭게 발전시킨 것으로 보인다. 당시 천문의기를 구성하는 것에는 천구의 도수를 눈금으로 새긴 원형의 환(環)이나 구형의 혼(渾)이 있었다. 조선에서는 시헌력을 도입하기 전까지 천구의 도수(주천도수)를 365.25 등분하였고, 하루 12시진을 백각으로 나누었으며, 이를 각각 주천도분환과 백각환에 눈금을 새기었다. 당시에는 환의 둘레에 주천도수와 백각을 새기는 기술적인 어려움이 있었다. 이러한 제작 상의 문제를 해결하는 방법으로, 본 연구에서는 도수나 시각의 각거리를 일정한 길이의 단위로 설정하여 원주를 등분하였을 것으로 가정하였다. 즉 조선의 소형화된 천문의기는 주천도의 1도나 백각의 1각을 일정한 길이의 단위인 푼이나 치의 정수배로 하여 환의 둘레에 주천도수와 백각의 눈금을 새겼을 것으로 추정하였다. 만일 주천도의 1도 각거리를 1푼으로, 백각의 1각 각거리를 1푼으로 하는 표준 변환을 적용하면, 각각 환의 지름이 1.16치, 0.32치가 된다. 이러한 방법이 현존하는 일성정시의나 소간의의 세 종류의 환과 현주일구의 백각환의 특성과 잘 일치함을 보이고 있다. 이 연구의 결과는 향후 소형화된 천문의기의 구조적인 재원을 연구할 때나 출처가 불분명한 의기의 크기를 이해하는데 주요한 역할을 할 수 있을 것으로 기대한다.

• Publications of The Korean Astronomical Society
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• v.27 no.3
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• pp.95-103
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• 2012

We analyzed the current status of the telescope control system (TCS2) of the 1.8 m telescope in Bohyunsan Optical Astronomy Observatory (BOAO), and suggest a new TCS (TCS3) for the long term development of BOAO. The TCS2 was constructed in 1998 to replace the TCS1 which was installed with the telescope itself at the commencement of BOAO. One of the important parts of TCS is PMAC (Programmable Multi-Axis Controller), which is a general-purpose multi-axis motion controller. PMAC provides the direct interactive communication environment permitting users to command the controller directly with simple operations. This makes the setup, debugging, and diagnostics very easy. The TCS2 was operated stable for a long time, but the hardware and TCS computers have been deteriorated and are out of date now. The new TCS3 needs to be constructed based on a modern computer system. And functions such as pre-calculations of telescope limiting position, interworking with virtual observatory tools, and using GUI, etc should be added. Construction of the TCS3 will be a step creating a better observation environment for the Korean astronomical society.

• Journal of the Korean earth science society
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• v.43 no.1
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• pp.1-22
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• 2022

We provide a detailed description of the installation and operation of a remote spectroscopic meteor observation system at Unjangsan optical astronomy observatory. Three light-sensitive charge-coupled device cameras were installed, and two cameras had a diffraction grating attached to the front of the lens. Station employ sensitive "Watec-902H2" cameras in combination with f/1.2 lenses were installed in November 2019. Diffraction gratings for spectral observations were used at 500 l/mm. Observations were conducted from November 2019 to June 2020. We employed the SonotaCo UFO software suite for meteor detection. Subsequently, meteor spectra were analyzed using field-tested RSpec software. To analyze the observation images, astronomical calibration and photometric calibration were performed, and the chemical elements of the meteor were determined. The study results are presented along with the system setup installation and operation experience. Brief information regarding the origin of the meteor was also provided based on the results.

• Journal of the Korean earth science society
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• v.37 no.7
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• pp.389-397
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• 2016

In order to investigate the light curve difference in visual and infrared wavelength of ${\delta}$ Scuti variable Bo Lyn, observations were performed using BOAO 1.8m reflecting telescope and an infrared detector, KASINICS, with J, H, and Ks filters. Infrared light curves of total 7 nights were obtained between March and April in 2011, and those were compared to the V-filter light curve to examine the differences in period, time of maximum light, amplitude, and shape. From the periodic analysis of infrared light curve, a single frequency of $f_1=10.712cycle/day$, $P=0.09335{\pm}0.00002days$ was obtained, and there was no difference in the period along different wavelengths. In the infrared light curve, a frequency of $2f_1$ was detected. This frequency well explains the asymmetric shape of light curve, one of the characteristics of high-amplitude ${\delta}$ Scuti variables. We compared the locations of the measured infrared maxima and the predicted maxima of V-filter, finding that the times of maxima were delayed about 0.3 phase at infrared wavelengths. Amplitude ratios were adopted to be ${\Delta}J/{\Delta}V=0.328$, ${\Delta}H/{\Delta}V=0.216$, and ${\Delta}Ks/{\Delta}V=0.211$, with the range of variation being smaller at longer wavelengths. It seems that the differences in the times of maxima and amplitude occurred because the changes in brightness of a pulsating variable star are mainly caused by the change in temperature.

• Journal of the Korean earth science society
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• v.38 no.6
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• pp.405-420
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• 2017

We investigated the H I, He II and O III emission lines of the symbiotic star AG Peg, using the spectroscopic data secured at different phases in three periods at the Lick Observatory. We measured FWHM and the intensity of six O III Bowen lines and studied the efficiency of fluorescence mechanism. The mean FWHM of O III normal and Bowen lines observed during three time periods did not make much difference, while Bowen line intensities are about 4.0 times higher than the normal lines. Comparing the predicted and the observed ratios, we found that the observed intensities are higher than predicted intensities, except for O III ${\lambda}$ 3759.87. The O III ${\lambda}$ 3791.26 and 3754.67 intensity ratios observed only in 2001 are in good agreement with the predictions by Saraph and Seaton (1980). We obtained the Bowen efficiency parameter (R)=0.47 for 2002, but we could not find R for the other two periods of time. Because of this, based on the 2002 efficiency result, we calculated the intensity ratio of O III normal and Bowen lines relative to He II ${\lambda}$ 4685.68 and derive the efficiency variation with time period. The result showed that the efficiency is the highest in 1998 and the lowest in 2001. We conclude that the efficiencies with phase are caused by the electron temperature changes in the ionized gas. The efficiencies of AG Peg are likely to increase along with electron temperature. Our analysis results may be useful in understanding the physical conditions of the ionized shell in symbiotic star and the intensity ratio and efficiency variation.