• The Bulletin of The Korean Astronomical Society
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• v.46 no.1
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• pp.36.4-36.4
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• 2021

블레이자는 제트가 관측자 시선방향과 나란하게 놓여있는 활동은하핵(AGN)으로 모든 파장대역에서 변광을 보이는 것이 주요 특징이다. 우리는 블레이자의 변광특성을 이해하기 위해 강한 변광을 보이는 천체인 3C 279를 연구대상으로 선정했고, 9년간의 X선 및 광학 데이터를 이용하여 이 천체의 광도와 스펙트럼 기울기 사이의 상관관계분석을 수행하였다. 이를 통하여, 시간에 따라 상관계수가 변한다는 것과 X선 변광이 광학변광보다 65일 앞선다는 것을 발견하였다. 이 발표에서는 one-zone SED 모형을 이용해 위의 현상들을 해석한 결과를 제시한다.

• The Bulletin of The Korean Astronomical Society
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• v.40 no.1
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• pp.51.4-52
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• 2015

From 2010 to 2014, CQUEAN (Camera for QUasars in EArly uNiverse) has been operated for the observation at the 82 inch Otto Struve Telescope of the McDonald Observatory, US. This camera is optimized at wavelength range of 0.7 - 1.1 um with seven (g', r', I', z', Y, Iz and Is) broad-band filters for the survey of high redshift (z > 5) quasars in the early universe. We are upgrading this system to identify more details of SED (Spectral Energy Distribution) of quasar candidates and other astronomical sources. The SQUEAN is comprised of a focal reducer, a CCD camera, a new filter wheel, new auto guiding system and new control software. The new filter wheel consists of interchangeable cartridges for various wavelength and size of filters. 50 nm medium bandwidth filters from 600 - 1050 nm, seven SDSS (Sloan Digital Sky Survey) filters and Johnson-Cousin BVRI filters are installed for now. We also have a plan to use narrow band interference filters to classify high redshift quasars or to obtain SEDs of interesting astronomical sources in details more efficiently. We also developed KAP82 (Kyung Hee University Auto guiding Package for 82 inch telescope) for auto guiding software. CQUEAN and SQUEAN have been developed by CEOU (Center for the Exploration of the Origin of the Universe).

• Publications of The Korean Astronomical Society
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• v.27 no.4
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• pp.281-284
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• 2012

We utilize AKARI's slitless spectroscopic capability to detect the $3.3{\mu}m$ polycyclic aromatic hydrocarbons (PAHs) emission and measure star formation (SF) activity for various AKARI programs. First, we obtain $2{\sim}5{\mu}m$ spectra of 20 flux-limited galaxies with mixed SED classes in order to calibrate the $3.3{\mu}m$ PAH luminosity ($L_{PAH3.3}$) as a star formation rate (SFR) indicator. We find that $L_{PAH3.3}$ correlates with $L_{IR}$ as well as with the $6.2{\mu}m$ PAH luminosity ($L_{PAH6.2}$). The correlations does not depend on SED classes. We find that ULIRGs deviate from the correlation between PAH luminosities and $L_{IR}$, while they do not for the correlation between PAH luminosities. We suggest possible effects to cause this deviation. On the other hand, how AGN activity is linked to SB activity is one of the most intriguing questions. While it is suggested that AGN luminosity of quasars correlates with starburst (SB) luminosity, it is still unclear how AGN activity is connected to SF activity based on host galaxy properties. We are measuring SFRs for the LQSONG sample consisting of reverberation mapped AGNs and PG-QSOs. This is an extension of the ASCSG program by which we investigated the connection between SB and AGN activities for Seyferts type 1s at z ~ 0.36. While we found no strong correlation between $L_{PAH3.3}$ and AGN luminosity for these Seyferts 1s, $L_{PAH3.3}$ measured from the central part of galaxies correlates with AGN luminosity, implying that SB and AGN activities are directly connected in the nuclear region.

• Publications of The Korean Astronomical Society
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• v.32 no.1
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• pp.109-111
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• 2017

We detected bright mid- to far-infrared emission from the helium nova V445 Puppis in the AKARI all-sky survey data taken in 2006. Assuming an optically thin condition, we decomposed the spectral energy distribution (SED) of V445 Puppis in October 2006 by model fitting and found that the SED can be explained by a combination of cold amorphous carbon (125 K and the mass of $4.5^{+6.6}_{-2.7}{\times}10^{-4}M_{\odot}$) and warm amorphous carbon (250 K and the mass of $1.8^{+1.0}_{-0.5}{\times}10^{-5}M_{\odot}$). Assuming that the former is pre-existing dust formed in the past nova outbursts and the latter is newly formed dust in December 2000's nova wind, this result suggests that the amount of dust formed around V445 Puppis in a single outburst is larger than $10^{-5}M_{\odot}$, which is larger than those in any other classical novae ever reported.

• Publications of The Korean Astronomical Society
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• v.32 no.1
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• pp.239-244
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• 2017

How does the presence of an AGN influence the total SFR estimates of galaxies and change their distribution with respect to the Galaxy Main Sequence? To contribute to solving this question, we study a sample of 1133 sources detected in the North Ecliptic Pole field (NEP) by AKARI and Herschel. We create a multi-wavelength dataset for these galaxies and we fit their multi-wavelength Spectral Energy Distribution (SED) using the whole spectral regime (from 0.1 to $500{\mu}m$). We perform the fit using three procedures: LePhare and two optimised codes for identifying AGN tracers from the SED analysis. In this work we present an overview of the comparison between the estimates of the Infrared bolometric luminosities (between 8 and $1000{\mu}m$) and the AGN fractions obtained exploiting these different procedures. In particular, by estimating the AGN contribution in four different wavelength ranges ($5-40{\mu}m$, $10-20{\mu}m$, $20-40{\mu}m$ and $8-1000{\mu}m$) we show how the presence of an AGN affects the PAH emission by suppressing the ratio $\frac{L_{8{\mu}m}}{L_{4.5{\mu}m}}$ as a function of the considered wavelength range.

• Radiation Oncology Journal
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• v.6 no.2
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• pp.151-154
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• 1988

To answer the question whether last clonogenic cell should be eradicated for the tumor to be controlled, radiation tumor control study was performed using microscopic tumors of variable sizes ranging from 101 to 10s tumor cells. $TCD_{50}'s$ estimated from experimental data were 14.8, 27. 1, 42.4, 49.9 and 65.5 Gy for $10^1,\;10^2,\;10^3,\;10^4\;and\;10^4$ tumor cells, respectively. Theoretical calculations, assuming that all the clonogenic cells should be inactivated, were 15.65, 8.50, 40.97, 53.41 and 65.85 Gy. From this well matched data, it can be concluded that all the clonogenic cells should be eradicated for tumor control, at least in this tumor model.

• Proceedings of the Korea Contents Association Conference
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• 2009.05a
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• pp.437-441
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• 2009

The modern times is as special as from the river, the river is very important of our life. The importance to preserve the river environment has been issued and the river developing method is being changed to use potential function of nature as well as flood control. Essential element of the river restoration is a vegetation. The flow resistance by vegetation along the river banks is greatly increase the flood stage. Therefore, the flow resistance due to vegetation in the river and roughness coefficient changes to understand the hydraulic characteristics is an important elements in the river restoration. The purpose of this study is to analyze the flood stage and the aspects of riverbed changes due to the corridor restoration with river vegetation. In order to simulate the flood stage and riverbed changes, HEC-RAS, RMA-2, and SED-2D model were applied for the upstream and downstream in study reaches, respectively.

• Proceedings of the Korea Water Resources Association Conference
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• 2008.05a
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• pp.963-966
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• 2008

본 연구에서는 최근까지 유사관측을 수행하고 있는 금강본류 하도구간의 금남$\sim$공주 지점을 대상으로 하였다. 분석을 위하여 이 지점의 총유사량 산정에 영향을 미치는 부유사량 관측 및 수위, 유량과 같은 하천 흐름 등에 관한 과거의 자료를 수집 정리 하였다. 본 연구에서 적용하고자 하는 교량의 교각에 대한 기하학적 형상은 원형, 정사각형, 정팔각형, 장방형으로 하였으며 분석 모형은 SED2D-WES 모형을 이용하여 유역에 대한 교각의 형상이 미치는 영향에 대하여 연구 하였다. 그 결과 지름이 6m, 경간장 57m인 원형교각의 경우 교각에서 약 14.3m 떨어진 곳에서 최고 유속 0.75m/s가 발생되었으며, $6{\sim}6m$의 정사각형교각의 경우 교각으로부터 약 15.8m떨어진 곳에서 0.68m/s의 최대 유속이 발생하고 $6{\sim}6m$ 정팔각형교각의 경우 교각으로부터 약 16.2m떨어진 곳에서 0.65m/s의 최대유속이 발생하고, 마지막으로 $3{\sim}6m$ 장방형교각의 경우 교각으로부터 약 21m 떨어진 구간에서 0.63m/s의 최고 유속이 발생하는 것으로 나타났다. 대상유역의 길이가 길고, 유속이 낮으므로 유출지점까지 흘러내려가는 유사량보다 하천내에 유입된 유사가 그대로 퇴적되는 경우가 많아 24시간 분석결과 하상변동량은 퇴적량과 침식량을 합하여 약 0.22%정도 변동되는 것으로 나타났으며, 교각형상에 따른 하상변동특성으로 원형교각의 경우 세굴이 일어나는 지점은 교각에서 약 16.88m떨어진 지점까지 하상변동이 일어났으며, 정사각형 교각의 경우 교각에서 약 10.96m떨어진 지점까지, 정팔각형 교각의 경우 교각에서 약 6.32m떨어진 지점까지, 장방형 교각의 경우 교각에서 약 18.23m떨어진 지점까지 하상변동이 나타남을 알 수 있었다.

• Proceedings of the Korean Society of Propulsion Engineers Conference
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• 2008.05a
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• pp.321-327
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• 2008

Performance characteristics of the axi-symmetric supersonic exhaust diffuser (SED) with a second throat are numerically investigated. Computational strategy repeats those for a straight exhaust diffuser with zero-secondary flows. Renolds-Average Navier-Stokes equations with a standard ${\kappa}-{\varepsilon}$ turbulence model incorporated with standard wall function are solved to simulate the diffusing evolutions of the nozzle plume. The methodology is validated with accuracy. To predict the improvement of starting performance by second throat diffuser, diffuser characteristic curve due to the SED equipped with the second throat is speculated with respect to that of a straight area type as a function of nozzle stagnation pressure. Principal physics caused by the of the second throst is also addressed in terms of a second throat area ratio.

• Journal of Environmental Science International
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• v.18 no.2
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• pp.221-230
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• 2009

In this study, a river basin with a lot of measured data such as water level, flow rate, current speed, and sediment rate from the past to now was selected and geometrical shape of a pier was re-analyzed, in order to study the effects of the flow around the pier area as well as the riverbed alternation characteristics. A finite element mesh of the entire river was prepared, and via parameter revision, the section that the pier has influence on was decided, to analyze the shape of the pier using RMA-2 and SED2D-WES models. With regards to the section that the pier has influence on, analysis was done on the four pier shapes, namely circle, square, rectangle, and octagon. The results showed that the shape with the least influence around the pier around is the octagon, followed by circle, rectangle, and square, showing the different geometrical effects that the shapes have on the pier. Furthermore, it was shown that the distribution of sediment concentration had effect from about (+) 110 m of the upstream to about (-) 130 m of the downstream, from the pier installation point. Also, it was shown after analyzing drag forces for different sediment particle distributions that the shape with the greatest drag is the octagon, followed by circle, square, and rectangle.