• 천문학회보
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• 제32권1호
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• pp.75.1-75.1
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• 2007

• 한국주거학회논문집
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• 제16권4호
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• pp.91-100
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• 2005

This study aims to find the architectural concepts of Song-Sun and the spatial structure of the Myonangjong through kasa, sijo, and Chinese poems. He considered his place as a ideal place to dwell a secluded life which is surrounded by mountains, and opened to a field in front. That places is connected with geomancy or Feng Sui, and he attached great importance to placeness of the Myonangjong as a pavilion. As his place was called 'tyoro samgan', his place should be simple, and that was harmonized with nature. He regarded his place as a part of the outside space and its surrounding nature. As the pen name of Myonangjong shows that his way of life is very pure so he need not disgrace against the earth and the sky, he considered his building as a place of embodying the Confucian great law of heaven and earth. Myonangjong has a concentric circle structure of the scenery which is viewed panoramically along with the visual direction.

• 천문학회지
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• 제35권2호
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• pp.67-73
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• 2002

We have made a topological study of cosmic microwave background (CMB) polarization maps by simulating the AMiBA experiment results. A ACDM CMB sky is adopted to make mock interferometric observations designed for the AMiBA experiment. CMB polarization fields are reconstructed from the AMiBA mock visibility data using the maximum entropy method. We have also considered effects of Galactic foregrounds on the CMB polarization fields. The genus statistic is calculated from the simulated Q and U polarization maps, where Q and U are Stokes parameters. Our study shows that the Galactic foreground emission, even at low Galactic latitude, is expected to have small effects on the CMB polarization field. Increasing survey area and integration time is essential to detect non-Gaussian signals of cosmological origin through genus measurement.

• 천문학논총
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• 제32권1호
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• pp.127-129
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• 2017

We have observed ~60 Weak-line T Tauri stars (WTTSs) toward the Chamaeleon star forming region using the AKARI Far-Infrared Surveyor (FIS) All-Sky maps. We could not detect any significant emission from each source even at the most sensitive WIDE-S band. Then, we have performed stacking analysis of these WTTSs using the WIDE-S band images to improve the sensitivity. However, we could not detect any significant emission in the resultant image with a noise level of $0.05MJy\;sr^{-1}$, or 3 mJy for a point source. The three-sigma upper limit of 9 mJy leads to the disk dust mass of $0.01M_{\oplus}$. This result suggests that the disks around Chamaeleon WTTSs are already evolved to debris disks.

• 대기
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• 제15권4호
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• pp.203-211
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• 2005

One algorithm has been developed for retrieving aerosol optical thickness from GMS-5 visible channel measurements, and then the algorithm was applied for obtaining the geographical distribution of aerosol optical thickness over East Asia during April 2002. Algorithm employs a look-up table based upon radiative transfer calculations with solar geometry, aerosol optical thickness, and surface albedo as inputs. Validation was conducted by comparing retrieved aerosol optical thickness with measured values from ground-based sky radiation measurements at Anmyon Do, Korea. It was found that the correlation coefficient is 0.71 with -0.03 of bias and 0.34 of root mean square error, suggesting that the algorithm developed in this study can be used for estimating aerosol optical thickness in a quantitative sense.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 1998년도 Proceedings of International Symposium on Remote Sensing
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• pp.404-408
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• 1998

Yellow sand event has been studied using SeaWiFS data in order to examine the aerosol optical characteristics in the Yellow Sea and their influences on the atmospheric correction for the ocean color remote sensing. Two SeaWiFS images of April 18 and April 25, 1998, representing Yellow Sand event and clear-sky case respectively, are selected for emphasizing the impact of high aerosol concentration on the ocean color remote sensing. It was shown that NASA's standard atmospheric correction algorithm treats yellow sand area as either too high radiance or cloud area, in which ocean color information is not generated. SeaWiFS aerosol optical thickness is compared with nearby ground-based sun photometer measurements and also is compared with radiative transfer simulation in conjunction with yellow sand model, examining the performance of NASA's atmospheric correction algorithm in case of the heavy dust event.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 1998년도 Proceedings of International Symposium on Remote Sensing
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• pp.14-19
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• 1998

The MUBEX (MUtsu Bay sea surface temperature validation EXperiment) campaign has been held from 1995 to 1997 in summer. During the MUBEX campaign, a thermal infrared camera (TIC) installed on a research vessel, which was also equipped with other various observation devices, was intensively used to observe microscopic structure of sea skin surface temperature (SSST) behavior. We have now a total number of 500,000 images observed by the TIC under various weather conditions, i.e., very calm or wavy sea condition, and clear, patchy or cloudy sky condition. In this paper, we show typical SSST patterns observed by the TIC, and describe the result of statistical analysis of SSST.

• 한국지리정보학회지
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• 제15권2호
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• pp.103-112
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• 2012

SAR(Synthetic Aperture Radar) 영상과 AIS(Automatic Identification System) 자료를 활용하여 선박 탐지 실험을 수행하였다. 2010년 5월, 2주간 서해안(인천 근해)의 다중시기 해외위성 SAR 영상인 TerraSAR-X, Cosmo-SkyMed(X-밴드), Radarsat-2(C-밴드)와 AIS 자료를 이용하였다. SAR 영상 분석을 위해 해양과 선박의 산란 특성과 SAR 영상과 AIS 자료의 기초 처리 방법을 기술하였다. 선박 식별을 위해서 임계값 설정 기법을 사용하였다. 선박 탐지 결과로 시계열 변화 탐지와 AIS 연동 선박 탐지 사례를 보인다. 이 결과를 통해 위성 SAR 영상과 AIS를 이용한 선박 탐지는 해양 관리에 유용하게 사용될 수 있을 것으로 사료된다.

• 천문학논총
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• 제27권4호
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• pp.201-207
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• 2012

Following the first Public Release of the AKARI Point Source catalogues, we have worked on the production of a new far-infrared All-Sky Diffuse mapping product. In this paper we report first results from the All Sky diffuse maps that will shortly be released to the community, based on analysis of data from the Far Infrared Surveyor ($65{\mu}m-160{\mu}m$) instrument. These data are likely to have a strong impact on studies of extended structures, and the diffuse ISM.

• 천문학회보
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• 제43권1호
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• pp.51.3-52
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• 2018

Since Voyager 1 passed the Heliopause in 2012, it has provided the observations of the charged particles in the local interstellar medium. However, Voyager 1 only provides the information along with its trajectory. In order to understand the global view of the interstellar plasma flow surrounding the Heliopause, we need another tool. When the interstellar plasmas approach the Heliopause, the ions are deflected around the Heliopause due to the draping of the interstellar magnetic field. The draping of the interstellar magnetic field is strongly connected with the shape of the Heliopause. A fraction of the diverted ions exchanges their charges with the undisturbed primary interstellar neutral atoms, and then the ions become neutral atoms called the secondary interstellar neutral atoms. The newly created neutral atoms carry information on the diverted flow of the interstellar ions, and a fraction of them can travel to the Sun. Therefore, the secondary component of the interstellar neutrals is an excellent diagnostic tool to provide important information to constrain the shape of the Heliopause. The secondary interstellar neutrals are observed by Interstellar Boundary Explorer (IBEX) at Earth's orbit. Since 2009, two energetic neutral atom cameras on IBEX have measured neutral atoms and it has provided sky maps of neutral atoms. In this presentation, we will discuss the directional distribution of the secondary interstellar neutrals at Earth's orbit. In the sky maps, the primary interstellar neutral gas is seen between $200^{\circ}$ and $260^{\circ}$ in ecliptic longitude and the secondary components are seen in the longitude range of $160^{\circ}-200^{\circ}$. We also present a simplified model of the outer heliosheath to help interpret the observations of interstellar neutrals by the IBEX-Lo instruments. We extract information on the large-scale shape of the Heliopause by comparing the neutral flux measured at IBEX along four different look directions with simple models of deflected plasma flow around hypothetical obstacles of different aspect ratios to the flow. Our comparisons between the model results and the observations indicate that the Heliopause is very blunt in the vicinity of the Heliospheric nose, especially compared to a Rankine half-body or cometary shape.