• Publications of The Korean Astronomical Society
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• v.20 no.1 s.24
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• pp.117-124
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• 2005

We plan to install the polarimetric optics in the AGU(acqusition and guiding unit) of the 1.8 m telescope at the BOAO(Bohyunsan Optical Astronomy Observatory). With this, the spectropolarimetric observations with the resolution of 45,000 and 60,000 in 4,000 to $8,000{\AA}$ ange could be done by the BOES(BOao Echelle Spectrograph). If we use the precision radial velocity measurement capability of the BOES, the accuracy of the magnetic field intensity measurements with this new BOES stokesmeter will be much increased. We present here the design concept of the BOES stokesmeter. Some details on the optics, mechanical parts, fiber parts and the lab test procedures of this stokesmeter are explained.

• Publications of The Korean Astronomical Society
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• v.19 no.1
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• pp.65-70
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• 2004

An imaging spectrograph concept optimized for extended far-ultraviolet emission sources is presented. Although the design was originally developed for FIMS aboard the first Korean science satellite STSAT-l launched on September 27, 2003, no rigorous theoretical background of the spectrograph design has been published. The spectrograph design employs an off-axis parabolic cylinder mirror in front of a slit that guides lights to a diffraction grating. The concave grating provides moderate spatial resolution over a large field of view. This mapping capability is absent in most astronomical instruments but is crucial to the understanding of the nature of a variety of astrophysical phenomena. The aberration theory presented in this paper can be extended to holographic gratings in order to improve the spatial as well as the spectral resolutions.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.125.1-125.1
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• 2011

After a short description of the observatory, this presentation will highlight some of the most recent scientific achievements based on CFHT observations and how they benefit from the current instrumentation and novel observing modes proposed to the CFHT users. We will then move to the mid-term future with the development of new spectroscopic capabilities (visible wide-field FTS or near-IR spectro-polarimetry) and the study of a novel wide-field imager in the visible using Ground-Layer AO to provide unprecedented image quality on a large field of view. As an option for the long-term future, the concept of a next generation 10-m class telescope to replace the current CFHT 3.6-m will be described. An emphasis will be given on how CFHT is slowly morphing into an Asia-Pacific Rim observatory and on the role the Korean community could play in such an endeavor, from immediate access to first-class astronomical data to partnering with other nations in exciting developments.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.2
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• pp.48.2-48.2
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• 2018

본 연구에서는 한국천문연구원이 2008년 말부터 운영하고 있는 찾아가는 이동천문대 '스타-카'를 이용한 과학문화 확산 프로그램의 효율성을 높이기 위한 방안을 모색해 보았다. 기존의 프로그램은 과학관에서 전통적으로 사용하고 있는 PUST(Public Understand of S&T) 방식으로 일반적인 강연 및 관측 프로그램의 진행 등으로 구성되어 진행되어 왔다. 본 연구는 STEAM 등 최근 과학교육 및 과학대중화 활동에서 사용하고 있는 시도 중의 하나인 PEST(Public Engagement with S&T)를 활용하여 스타-카 프로그램을 개선해서 실제 현장에서 적용한 결과를 소개하려 한다. 개선된 프로그램으로 찾아가는 이동천문대 프로그램을 운용한 결과로 과학기술정보통신부(구 미래창조과학부)에서 '교육기부 대상' 및 '고객만족도 우수사례'로 선정된 바 그 사례를 소개해 볼 예정이다.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.90.1-90.1
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• 2011

We are developing empirical space weather (geomagnetic storms, solar proton events, and solar flares) forecast models based on solar information. These models have been set up with the concept of probabilistic forecast using historical events. Major findings can be summarized as follows. First, we present a concept of storm probability map depending on CME parameters (speed and location). Second, we suggested a new geoeffective CME parameter, earthward direction parameter, directly observable from coronagraph observations, and demonstrated its importance in terms of the forecast of geomagnetic storms. Third, the importance of solar magnetic field orientation for storm occurrence was examined. Fourth, the relationship among coronal hole-CIR-storm relationship has been investigated, Fifth, the CIR forecast based on coronal hole information is possible but the storm forecast is challenging. Sixth, a new solar proton event (flux, strength, and rise time) forecast method depending on flare parameters (flare strength, duration, and longitude) as well as CME parameter (speed, angular width, and longitude) has been suggested. Seventh, we are examining the rates and probability of solar flares depending on sunspot McIntosh classification and its area change (as a proxy of flux change). Our results show that flux emergence greatly enhances the flare probability, about two times for flare productive sunspot regions.

• Journal of Information Management
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• v.39 no.4
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• pp.155-171
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• 2008

We constructed the integrated management system of distributed astronomical data of Bohyunsan Optical Astronomy Observatory(BOAO), Sobaeksan Optical Astronomy Observatory (SOAO), and Mt. Lemmon Optical Astronomy Observatory(LOAO). The observed data was stored in the archive of the observatory and MySQL table is saved in the integrated management system. There are data archive managers in the observatories and they manage the integrated management system such as data storing, head information extraction, table generation, and management of web pages, etc. The users can search and download all the data in the integrated management system web page. The concept of this system - send queries from web page to the observatory archives - is the same of the basic concept of virtual observatory. This research is one of the main work in the Korean virtual observatory which is take part in the international virtual observatory alliance.

• Journal of the Korean earth science society
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• v.33 no.2
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• pp.183-199
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• 2012

Previous Earth Science textbooks have mostly lacked the latest astronomical phenomena frequently being reported in mass media such as popular science magazines. One of the main directions in the revision of the 2009 National Curriculum of Korea is to actively include those phenomena. Furthermore, despite a close link between astronomy and physics, the concept of modern physics has not been actively introduced in Earth Science textbooks and at the same time the linkage of physics to astronomy has rarely been studies in physics textbooks. Therefore, the concept of integration among different fields in science is emphasized in the new National Curriculum. Transient phenomena in the high energy astrophysical objects are examples that reflect such issue. The purpose of this study is to introduce transferring a real-time data and making imaging of astronomical observations using e-Science. As a first step, we performed the first experiment for a large data transfer of astronomical observation between Korea and Japan using KOREN, a National Research and Education Test Network. We introduce actively on-going fields of e-Science in observational activities of astronomy and astrophysics, and their close interrelationship with scientific inquiry activities and public outreach activities. We discuss our experiment in the scientific and educational aspects to the primitive e-Science activity in the Korean astronomical society and, in turn, provide a prospective view for its application to the scientific inquiry activities and public outreach activities in the upcoming commercial Gbps-level internet environments.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.2
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• pp.66.1-66.1
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• 2016

We developed an observation control software for the IGRINS (Immersion Grating Infrared Spectrograph) silt-viewing camera module, which points the astronomical target onto the spectroscopy slit and sends tracking feedbacks to the telescope control system. The point spread function (PSF) is not always symmetric. In addition, bright targets are easily saturated and shown as a donut shape. It is not trivial to define and find the center of the asymmetric PSF especially on a slit mask. We made a center balancing algorithm (CBA) following the concept of median. The CBA derives the expected center position along the slit-width axis by referencing the stray flux ratios of both upper and lower sides of the slit. We compared efficiencies of the CBA and those of a two-dimensional Gaussian fitting (2DGA) through simulations from observation images in order to evaluate the center finding algorithms. Both of the algorithms are now applied in observation and users can select the algorithm.

• Journal of The Korean Astronomical Society
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• v.29 no.spc1
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• pp.395-396
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• 1996

We developed a telescope control system called ASTROS for the VST1 and VST2, which are specially designed radio telescopes to make a survey and have a 60-cm main dish. ASTROS is designed on the distributed intelligence concept and structurized programming. The hardware of the system is composed of several intelligent devices connected with de facto standard interfaces and main control unit is PC. The program is coded in the C language and its structure is object oriented in order to make easy to replace the component devices. ASTROS is now running on two twin telescopes, VST1 and VST2. VST1 is installed at Nobeyama in Japan and VST2 is installed at La Silla in Chile. They are making a galactic plane survey in CO (J=2-1) with 9 arcmin beam semi-automatically.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.1
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• pp.93.2-93.2
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• 2012

Point Spread Function (PSF) is one of the most important optical characteristics for describing the performance of a telescope. And a concept of subpixelization is inevitable in evaluating the undersampled PSF (Shin and Sakurai 2009). Then, the internal structure of Yohkoh SXT CCD pixel is not uniform: For the top half of pixel area, the X-ray should pass a so-called gate structure where the charges are transferred to an output amplifier. This gate structure shows energy-dependent sensitivity (Tsuneta et al. 1991). For example, for Al-K (8.34 A) X-ray emission, the transmission of the polysilicon gate is about 0.9. Also, for the peak coronal response of the SXT thin filters, around 17 angstrom (0.729 keV), the transmission of the gate is about 0.6, falling off sharply towards longer wavelengths. It should be noted that this spectrally dependent non-uniform response of each CCD pixel will certainly have a noticeable effect on the properties of the PSF at longer wavelengths. Therefore, especially for analyzing the undersampled PSF of low energy source, a careful consideration of non-uniform internal pixel structure is required in determining the shape of the PSF core. The details on the effect of gate structure will be introduced in our presentation.