• Publications of The Korean Astronomical Society
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• v.27 no.3
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• pp.49-59
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• 2012

KASI (Korea Astronomy and Space Science Institute) has developed an SLR (Satellite Laser Ranging) system since 2008. The name of the development program is ARGO (Accurate Ranging system for Geodetic Observation). ARGO has a wide range of applications in the satellite precise orbit determination and space geodesy research using SLR with mm-level accuracy. ARGO-M (Mobile, bistatic 10 cm transmitting/40 cm receiving telescopes) and ARGO-F (Fixed stationary, about 1 m transmitting/receiving integrated telescope) SLR systems development will be completed by 2014. In 2011, ARGO-M system integration was completed. At present ARGO-M is in the course of system calibration, functionality, and performance tests. It consists of six subsystems, OPS (Optics System), TMS (Tracking Mount System), OES (Opto-Electronic System), CDS (Container-Dome System), LAS (Laser System) and AOS (ARGO Operation System). In this paper, ARGO-M system structure and integration status are introduced and described.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.1
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• pp.30.1-30.1
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• 2013

The sizes of galaxies are known to be closely related with their masses, luminosities, redshifts and morphologies. However, when we fix these quantities and morphology, we still find large dispersions in the galaxy size distribution. We investigate the origin of these dispersions for red early-type galaxies, using two SDSS-based catalogs. We find that the sizes of faint galaxies (${\log}(M_{dyn}/M_{\odot})$ < 10.3 or $M_r$ >-19.5) are affected more significantly by luminosity, while the sizes of bright galaxies (${\log}(M_{dyn}/M_{\odot})$ > 11.4 or $M_r$ <-21.4) are by dynamical mass. At fixed mass and luminosity, the sizes of low-mass galaxies (${\log}(M_{dyn}/M_{\odot})$ ~ 10.45 and $M_r$~-19.8) are relatively less sensitive to their colors, color gradients and axis ratios. On the other hand, the sizes of intermediate-mass (${\log}(M_{dyn}/M_{\odot})$ ~ 10.85 and $M_r$~-20.4) and high-mass (${\log}(M_{dyn}/M_{\odot})$ ~ 11.25 and $M_r$~-21.0) galaxies significantly depend on those parameters, in the sense that larger red early-type galaxies have bluer colors, more negative color gradients (bluer outskirts) and smaller axis ratios. These results indicate that the sizes of intermediate- and high-mass red early-type galaxies are significantly affected by their recent minor mergers or rotations. Major dry mergers also may have influenced on the size growth of high-mass red early-type galaxies.

• 한국태양에너지학회:학술대회논문집
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• 2009.04a
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• pp.19-26
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• 2009

This study is performed by method for the influx of natural light in underground space. to solve the several negative underground issues make the covered courtyard and high reflected wall toward the adjacent space. for illuminance level test of sunken garden space, the adjacent space size is $15M{\times}9M{\times}12M$ sunken Garden with space to install the ceiling on the size of the companion light performance analysis, and seasonal changes derived by the light of changes in performance. In addition, increase the distance of the wall and the adjacent space and estimate the average at true time P.M12. The resulting data indicate that the road was an average lux DESKTOP RADIANCE of the modeling and analysis was conducted.

• Bulletin of the Korean Mathematical Society
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• v.51 no.4
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• pp.957-964
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• 2014

In this paper, we prove that there is no branch point in the Lorentz space (M, d) which is the limit space of a sequence {($M_{\alpha},d_{\alpha}$)} of compact globally hyperbolic interpolating spacetimes with $C^{\pm}_{\alpha}$-properties and curvature bounded below. Using this, we also obtain that every maximal timelike geodesic in the limit space (M, d) can be expressed as the limit curve of a sequence of maximal timelike geodesics in {($M_{\alpha},d_{\alpha}$)}. Finally, we show that the limit space (M, d) satisfies a timelike triangle comparison property which is analogous to the case of Alexandrov curvature bounds in length spaces.

• Journal of Astronomy and Space Sciences
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• v.4 no.1
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• pp.55-63
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• 1987

세계 제 2 차대전이 끝난 이후로부터 40여년간, 현대 관측천문학을 이끌어 온 Palomar 산의 500cm 반사망원경은 드디어 차세대망원경에게 leadership을 넘겨주게 되었다. 자금염출이 여의치 않아 그동안 부진했던 초대형망원경 건설이 드디어 boom을 일으키게 된 것이다. 가주공과대학의 10m 반사망원경이 제작 중에 있고, Ohio주립대학도 10m 쌍통반사망원경 건립을 추진 중에 있고, 일본도 7.5m 반사망원경 건립을 검토 중이다. 한국은 1.5m~2m 반사망원경 제작이 구체화되어가고 있으니, 1970년, 불과 40cm 반사경 1대만 갖고 고군분투하던 그때를 초기하면 실로 감계무량하다 아니할 수가 없다. 그러나 NASA는 또 한편, 차세대망원경으로서 Space Shuttle을 이용하여 위성망원경을 발사할 계획을 1965년에서부터 구상하여 수차에 걸친 발의·부결을 거듭한 끝에, 드디어 1977년, 미국회의 건조인준을 얻었다.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.50.2-50.2
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• 2018

국립청소년우주센터 덕흥천문대의 NYSC 1m 망원경은 청소년을 대상으로 관측제안서를 공개모집하고, 청소년의 전문적인 천문관측을 지원하고 있다. 2017년 한 해, 접수된 청소년의 관측제안은 총 10건이었다. 이외에도 덕흥천문대는 양질의 관측자료를 국내 연구팀과의 공동연구를 통해 제공하고 있으며, 공동연구 장기관측과제 3건을 운영 중에 있다. 덕흥천문대 관측팀은 청소년 관측 및 공동연구를 지원하는 것과 더불어 망원경의 상태를 상시 점검하고 있다. 스티커 및 $CO_2$ 분사를 이용한 경면 세척을 진행하였고, 2017년 하반기에는 1m 망원경의 성능을 최대로 발휘할 수 있도록 CCD 카메라를 Princeton Instruments의 SOPHIA 2048B로 교체하였다. 그리고 앞으로 덕흥천문대에서 진행할 향후 운영 계획에 대해서도 논하고자 한다.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.50.1-50.1
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• 2018

We present the development of tools for Echelle spectrograph of NYSC 1-m telescope. The eShel spectrograph(Shelyak) has operated at Deokheung Optical Astronomy Observatory since 2016. We carried out test observation in 2016 and completed the preprocessing and wavelength calibration of the spectroscopic data using IRAF. Based on the reduction process in IRAF, PySpecW, a set of tools for spectroscopic data was developed in 2017. PySpecW was optimized for NYSC 1m telescope, and written in Python for youth to use easily on any OS. PySpecW consists of preprocessing, aperture tracing, aperture extraction, wavelength calibration, and dispersion correction for extracted spectra.

• Journal of KIISE:Software and Applications
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• v.34 no.5
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• pp.397-406
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• 2007

The problem of finding an optimal alignment between sequence A and B can be solved by dynamic programming algorithm(DPA) efficiently. But, if the length of string was longer, the problem might not be solvable because it requires O(m*n) time and space complexity.(where, $m={\mid}A{\mid},\;n={\mid}B{\mid}$) For space, Hirschberg developed a linear space and quadratic time algorithm, so computer memory was no longer a limiting factor for long sequences. As computers's processor and memory become faster and larger, a method is needed to speed processing up, although which uses more space. For this purpose, we present an algorithm which will solve the problem in quadratic time and linear space. By using division method, It computes optimal alignment faster than LSA, although requires more memory. We generalized the algorithm about division problem for not being divided into integer and pruned additional space by entry/exit node concept. Through the proofness and experiment, we identified that our algorithm uses d*(m+n) space and a little more (m*n) time faster than LSA.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.1
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• pp.61.3-62
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• 2016

An asteroid family is a group of asteroidal objects in the proper orbital element space (a, e, and i), considered to have been produced by a disruption of a large parent body through a catastrophic collision. Family members usually have similar surface properties such as spectral taxonomy types, colors, and visible geometric albedo with a same dynamical age. Therefore an asteroid family could be called as a natural Solar System laboratory and is also regarded as a powerful tool to investigate space weathering and non-gravitational phenomena such as the Yarkovsky/YORP effects. We carry out time series photometric observations for a number of asteroid families to obtain their physical properties, including sizes, shapes, rotational periods, spin axes, colors, and H-G parameters based on nearly round-the-clock observations, using several 0.5-2 meter class telescopes in the Northern hemisphere, including BOAO 1.8 m, LOAO 1.0 m, SOAO 0.6 m facilities in KASI, McDonald Observatory 2.1 m instrument, NARIT 2.4 m and TUG 1.0 m telescopes. This study is expected to find, for the first time, some important clues on the collisional history in our Solar System and the mechanisms where the family members are being transported from the resonance regions in the Main-belt to the near Earth space.

• The Bulletin of The Korean Astronomical Society
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• v.40 no.1
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• pp.86.4-87
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• 2015

We will soon complete the installation of 1m telescope at Deokheung Optical Astronomy Observatory (DOAO), National Youth Space Center (NYSC). Before the test observation with NYSC 1m telescope, we present the specs of the 1M telescope and observational conditions of the DOAO site, such as the seeing data at DOAO and the atmospheric extinction coefficients obtained from the observations of standard stars and stellar clusters with 120mm and 150mm refractor in 2014. Since atmospheric extinction coefficients depend on the observational instruments as well as the atmospheric conditions of the site, the improved data with NYSC 1m telescope will be obtained right after the completion of 1M telescope installation. We are planning to invite all astronomers to use 1m telescope for their sciences via regular proposal processes in this year.