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

• Proceedings of the KGS Conference
• /
• 2002.05a
• /
• pp.95-98
• /
• 2002

본 연구는 안동지역에 있어서 이른바 명당이라고 하는 음택 풍수 경관을 조사하여 그 형태와 특징을 살펴보고자 하였다. 안동문화원에서 펴낸 $\boxDr$안동의 분묘$\lrcorner$ 에 나오는 분묘를 대부분 조사하고 이를 형기론적 입장에서 형국으로 분류하였다. 태백산에서 소백산을 잇는 낙동정맥 살의 문수산(1206m)에서 하나의 지맥이 남쪽으로 흘러 태자산, 박달산, 오적산, 학가산(870m), 보문산(643m), 검무산(331m)을 이루어내어 안동의 서쪽 산줄기를 형성하며, 태백산에서 백병산, 일월산, 주방산(주왕산), 보현산, 황학산, 오산으로 이어지는 산줄기가 우측을 이루어내어, 이들 우백호와 좌청룡이 안동군 풍천면의 구담리에서 마주하게 된다. 그 사이로 안동군, 예안현 등이 입지하였다. 이러한 안동의 산세에 따라 낮은 구릉, 완만한 사면 및 높은 배후 산지가 전개되며 낙동강 본류와 지류가 흘러 다양한 형국이 나타나게 된다. 안동의 경우는 날짐승(봉, 학, 꿩), 꽃(모란, 연꽃, 칡넝쿨), 길짐승(닭), 들짐승(거북, 뱀), 물건(등잔, 가마솥, 밥상), 용, 달 등이 33개가 나타난다. 이들의 분포를 살펴보면 크게 낙동강 본류 이북 쪽에 집중한다. 이들 명당은 고도 상으로 해발고도 200미터 부근에 대부분 입지한다. 무릇 명당이란 안산과 조산을 넘어 득수가 잘 이루어져야 하므로 낙동강 본류를 중심으로 하고 그 지류를 향하여 분포하는 것은 당연하다 이들 명당의 형태와 공통된 특징을 살펴본 결과 명당은 반개방성, 중첩성, 안정성, 조화성, 균형성의 5가지 특징이 나타나는 곳이다. 이러한 명당의 특징은 태조산, 중조산, 소조산를 거쳐 주산 아래 산이 겹겹이 에워싸게 되고, 계곡물의 여러 줄기가 합수하고 물이 역류하지 않으며 잘 감아도는 곳으로 표현할 수 있다 이러한 명당의 기본적인 원리는 장풍(藏風)과 득수득파(得水得破)이다. 장풍과 득수란 '국'(局), 즉 산줄기와 수계로 이루어진 일정한 범위 속에 만물이 생태계 속에서 살아가는 모습인 '체형(體形)'의 의미가 나타나야 한다는 것이다. 그러나 이러한 의미는 시대에 따라 달라질 수 있는 것이다.

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

• Publications of The Korean Astronomical Society
• /
• v.27 no.3
• /
• pp.95-103
• /
• 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 Korea Water Resources Association
• /
• v.53 no.7
• /
• pp.545-555
• /
• 2020

A feasibility modeling for potential hydroelectric dam site selection was suggested using 1 sec ASTGTM (ASTER Global Digital Elevation Model) and Terra/Aqua MODIS (Moderate Resolution Imaging Spectroradiometer) derived land use (MCD12Q1) data. The modeling includes DEM pre-processing of peak, sink, and flat, river network generation, watershed delineation and segmentation, terrain analysis of stream cross section and reservoir storage, and estimation of submerged area for compensation. The modeling algorithms were developed using Python and as an open source GIS. When a user-defined stream point is selected, the model evaluates potential hydroelectric head, reservoir surface area and storage capacity curve, watershed time of concentration from DEM, and compensation area from land use data. The model was tested for 4 locations of already constructed Buhang, BohyunMountain, Sungdeok, and Yeongju dams. The modeling results obtained maximum possible heads of 37.0, 67.0, 73.0, 42.0 m, surface areas of 1.81, 2.4, 2.8, 8.8 ㎢, storages of 35.9, 68.0, 91.3, 168.3×10⁶ ㎥ respectively. BohyunMountain and Sungdeok show validity but in case of Buhang and Yeongju dams have maximum head errors. These errors came from the stream generation error due to ASTGTM. So, wrong dam watershed boundary limit the head. This study showed a possibility to estimate potential hydroelectric dam sites before field investigation especially for overseas project.

• Journal of the Korean earth science society
• /
• v.37 no.7
• /
• pp.389-397
• /
• 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 Astronomy and Space Sciences
• /
• v.24 no.4
• /
• pp.339-348
• /
• 2007

KASINICS (Korea Astronomy and Space Science Institute Near Infrared Camera System) is equipped with a InSb array which can observe $1-5\;{\mu}m$ bands in near-infrared. The absorption and emission by telluric water vapor becomes serious in the bands longer than $3\;{\mu}m$. We measured PWV (precipitable Water Vapor) levels above Bohyusan Optical Astronomy Observatory and Sobaeksan Optical Astronomy Observatory from July 2006 to August 2007 using the GPS PWV measurement system of KASI. We found that monthly averaged PWVs are lower than the prediction using dew-point temperature and as low as above Kitt Peak from September to February.

• Journal of Astronomy and Space Sciences
• /
• v.24 no.4
• /
• pp.327-338
• /
• 2007

We estimate the momentum fluxes of short-period gravity waves which are observed in the OI 557.7 nm nightglow emission with all-sky camera at Mt. Bohyun ($36.2^{\circ}\;N,\;128.9^{\circ}\;E$) in Korea. The intrinsic phase speed ($C_{int}$), the intrinsic period (${\tau}_{int}$), and vertical wavelength (${\lambda}_z$) are also deduced from the horizontal wavelength (${\lambda}_h$), observed period (${\tau}_{ob}$), propagation direction (${\phi}_{ob}$), observe phase speed (${\upsilon}_{ob}$) of the gravity wave on the all-sky images. The neutral winds to deduce intrinsic wave parameters are measured with Fabry-Perot interferometer on Shigaraki ($34.8^{\circ}\;N,\;13.1^{\circ}\;E$) in Japan. We selected 5-nights of observations during the period between July 2002 and December 2006 considering of the weather and instrument conditions in two observation sites. The mean values of intrinsic parameter of gravity waves are $({\tau}_{int})\;=\;12.9\;{\pm}\;6.1\;m/s,\;({\lambda}_z)\;=\;12.9\;{\pm}\;6.5,\;and\;(C_{int})\;=\;40.6\;{\pm}\;11.6\;min$. The mean value of calculated momentum fluxes for four nights besides of ${\lambda}_z\;<\;6\;km$ is $12.0\;{\pm}\;15.2\;m^2/s^2$. It is needed the long-term coherent observation to obtain typical values of momentum fluxes of the mesospheric gravity waves using all-sky camera and the neutral wind measurements.

• Journal of the Korean earth science society
• /
• v.33 no.7
• /
• pp.608-617
• /
• 2012

The symbiotic nova Z Andromedae (And) was investigated, using the high dispersion spectra of spectral resolution, ${\Delta}{\lambda}{\sim}-0.1{\AA}$. The spectral observations were done with (1) the Hamilton Echelle Spectrograph (HES) and the high resolution spectra (exposures=1800s and 3600s) were obtained at Lick Observatory in 2001 August $30^{th}$ (phase ${\Phi}$=0.77), and 2002 August $12^{th}$ (phase ${\Phi}$=0.22), (2) with the Bohyunsan Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory and the high resolution spectra (exposure=1200s) were secured in 2009 October $21^{st}$ (phase ${\Phi}$=0.70). From both the HES and BOES spectral data in the $3600{\AA}-9500{\AA}$ wavelengths, we extracted the emission lines of HI, HeI, and HeII, which have been decomposed into double or triple Gaussian components for 3 consecutive phases. The emission zones responsible for these components appear to be closely related with the orbital motion of a white dwarf or a giant star. The presence of the Raman scattering $H{\alpha}$ broad wing feature and the kinematic characteristics of the line profile observed in each phase imply that the Z And emission lines are mostly from two Lagrangian points, $L_1$ and $L_2$, and the accretion disk around the white dwarf star. The Z And was most active in 2009 and 2001 during the outburst phase, while it remained quiescent in 2002 in spite of the complex line profiles.

• Journal of the Korean earth science society
• /
• v.38 no.3
• /
• pp.209-221
• /
• 2017

We investigate the star formation rate, stellar mass, and gas-phase metallicity of local starburst galaxies with different star formation time scales based on their optical spectra. The observation is made using the longslit spectrograph attached to the 4K CCD on the Bohyunsan Optical Astronomy Observatory 1.8m telescope, targeting 21 Wolf-Rayet galaxies as young starbursts and 13 UV excess galaxies as slightly older starbursts. A Baldwin-Phillips-Terlevich diagram analysis shows that 50% of the observed targets are pure star-forming galaxies while only 15% are classified as Active Galactic Nuclei. Fraction of galaxies that reside in composite region is higher in UV excess galaxies than in Wolf-Rayet galaxies, suggesting that the AGN development requires extra time after the onset of the star formation. Most of the observed starburst galaxies have stellar masses of $10^{9-11}M_{\odot}$ and stellar formation rates of $0.01-100M_{\odot}yr^{-1}$, and their star formation rates are consistent with that of the SDSS star forming main sequence galaxies of similar stellar mass. There is no significant difference between Wolf-Rayet galaxies and UV excess galaxies in terms of the stellar mass and star formation rate. We also see a mass-metallicity relation for local starbursts with slightly lower metallicity for a given stellar mass, which implies the existence of a strong feedback activity due to the star formation in these galaxies.