• 천문학회보
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• 제46권1호
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• pp.32.3-33
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• 2021

We present H I gas kinematics and star formation activities of NGC 6822, a dwarf galaxy located in the Local Volume at a distance of ~ 490 kpc. We perform profile decomposition of the line-of-sight velocity profiles of the high-resolution (42.4" × 12" spatial; 1.6 km/s spectral) H I data cube taken with the Australia Telescope Compact Array (ATCA). For this, we use a new tool, the so-called BAYGAUD (BAYesian GAUssian Decompositor) which is based on Bayesian Markov Chain Monte Carlo (MCMC) techniques, allowing us to decompose a line-of-sight velocity profile into an optimal number of Gaussian components in a quantitative manner. We classify the decomposed H I gas components of NGC 6822 into bulk-narrow, bulk-broad, and non_bulk with respect to their velocity and velocity dispersion. We correlate their gas surface densities with the surface star formation rates derived using both GALEX far-ultraviolet and WISE 22 micron data to examine the impact of gas turbulence caused by stellar feedback on the Kennicutt-Schmidt (K-S) law. The bulk-narrow component that resides within r25 is likely to follow the linear extension of the Kennicutt-Schmidt (K-S) law for molecular hydrogen (H2) at the low gas surface density regime where H I is not saturated.

• 천문학회보
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• 제45권1호
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• pp.60.3-61
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• 2020

We perform disk-halo decomposition of the Large Magellanic Cloud (LMC) using a novel HI velocity field extraction method, aimed at better deriving its HI kinematics and thus the dark matter density profile. For this, we use two newly developed galaxy kinematic analysis tools, BAYGAUD and 2DBAT which have been used for the kinematic analysis of resolved galaxies from Australian Square Kilometre Array (ASKAP) observations like WALLABY which is an all-sky HI galaxy survey in southern sky. By applying BAYGAUD to the combined HI data cube of the LMC taken with the Australia Telescope Compact Array (ATCA) and Parkes radio telescopes, we decompose all the line-of-sight velocity profiles into an optimal number of Gaussian components based on Bayesian MCMC techniques. From this, we disentangle turbulent non-circular gas motions from the overall rotation of the galaxy. We then derive the rotation curve of the LMC by applying 2DBAT to the separated circular motions. The rotation curve reflecting the total kinematics of the LMC, dark and baryonic matters is then be combined with the mass models of baryons, mainly stellar and gaseous components in order to examine the dark matter distribution. Here, we present the analysis of the extracted HI gas maps, rotation curve, and J, H and K-band surface photometry of the LMC.

• 천문학논총
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• 제32권1호
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• pp.157-161
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• 2017

The dusty torus of Active Galactic Nuclei (AGNs) is one of the important components for the unification theory of AGNs. The geometry and properties of the dusty torus are key factors in understanding the nature of AGNs as well as the formation and evolution of AGNs. However, they are still under discussion. Infrared observation is useful for understanding the dusty torus as thermal emission from hot dust with the dust sublimation temperature (~ 1500 K) has been observed in the infrared. We have analyzed infrared spectroscopic data of low-redshift and high-redshift quasars, which are luminous AGNs. For the low-redshift quasars, we constructed the spectral energy distributions (SEDs) with AKARI near-infrared and Spitzer mid-infrared spectra and decomposed the SEDs into a power-law component from the nuclei, silicate features, and blackbody components with different temperatures from the dusty torus. From the decomposition, the temperature of the innermost dusty torus shows the range between 900-2000 K. For the high-redshift quasars, AKARI traced rest-frame optical and near-infrared spectra of AGNs. Combining with WISE data, we have found that the temperature of the innermost dusty torus in high redshift quasars is lower than that in typical quasars. The hydrogen $H{\alpha}$ emission line from the braod emission line region in the quasars also shows narrow full width at half maximum of $3000-4000km\;s^{-1}$. These results indicate that the dusty torus and the broad emission line region are more extended than those of typical quasars.

• 천문학회보
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• 제42권2호
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• pp.49.1-49.1
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• 2017

Comets are one of the most primordial solar system objects that hold the information of the early days of solar system formation inside their nuclei. Orbiting the Sun, they spew such ancient materials that have been buried for many years, creating dust and gas comae. Cometary dust grains absorb and scatter sunlight radiating the continuous light, while gas molecules form the line emissions. Eachof the comets has its own light patterns, which depends on the physical and chemical properties of the dust and gas components. In this regard, spectropolarimetrycan be a powerful tool to study the properties of cometary constituents free from contamination of each other. This methodology offers a series of information on the polarization degrees of the dust and gas components as well as on wavelength dependence of the polarization degree and polarization angle of cometary dust simultaneously. Herein, we will report the results of the spectropolarimetric study of comet 2P/Encke, which is one of the well-known objects for its shortest orbital period and its prominent aging signals. We performed a spectropolarimetric observation of comet 2P/Encke in its inbound orbit using the Higashi-Hiroshima Optical and Near-Infrared Camera (HONIR) at the Higashi-Hiroshima Observatory, Japan, on UT 2017 February 21 at high phase angle of =75.7 deg. Ourstudy of this interesting comet is the first and only one done through spectropolarimetry in a referred publication. We will discuss the most recent polarimetric results of our study in terms of 2P/Encke' scurrent evolutionary status.

• 한국지구과학회지
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• 제40권1호
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• pp.86-106
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• 2019

이 연구의 목적은 천문학적 사고를 반영한 과학관 천문교육 프로그램을 개발하고, 그 프로그램이 고등학생들의 천문학적 사고 능력의 향상에 미치는 효과를 확인하는 것이다. 문헌 연구를 통해 천문학적 사고의 구성 요소를 선정한 후 사고력 학습 발달 모형을 응용하여 시연과 관찰, 문제 제시와 사고 활동, 지원과 모둠 토의, 시연과 평가의 네 단계로 구성된 천문교육 프로그램을 개발하였다. 이 프로그램의 효과를 검증하기 위하여 실험군과 대조군의 사전, 사후 검사에 대해 공변량 분석을 실시하였고, 프로그램을 이용한 교수 학습 활동의 사전과 사후에 학생들의 수준 변화를 살펴 보았다. 연구 결과, 천문학적 사고를 반영한 과학관 천문교육 프로그램은 학생들의 천문학적 사고를 증진시키는 데 효과가 있는 것으로 확인되었다. 특히 이 프로그램은 천문 영역의 공간적 사고와 관련하여 관측된 천문 현상을 우주에서 보는 관점에서 재구성하여 모델링하는 능력을 신장시키는 데 효과가 있었고, 시스템 사고와 관련하여 천문 시스템을 구성하는 요소들 간의 관계를 파악하여 시스템을 조직할 수 있는 능력을 향상시키는 데 효과가 있었다. 이 연구는 학생들의 천문학적 사고를 발달시키기 위한 구체적인 교수 학습 프로그램을 제시하였다는 데 그 의의가 있다.

• 천문학회지
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• 제38권2호
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• pp.249-252
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• 2005

We present results of the velocity-resolved spectroscopy of the [Fe II] $\lambda$1.644${\mu}m$ emission toward outflow sources with the Subaru Telescope at the angular resolution of 0.apos;16 ${\~}$ 0.apos;5 arcseconds. The observed sources are L1551 IRS 5, DG Tau, HL Tau and RW Aur, which are located in the Taurus-Aurigae Molecular Cloud, one of the closest star forming regions (0.apos;1 = 14 AU). We were able to resolve outflow structure in the vicinity of the sources at a scale of a few tens of AU. The position-velocity diagram of each object shows two velocity components: the high velocity component (HVC: 200 - 400 km $s^{-l}$) and the low velocity component (LVC: 50 - 150 km $s^{-l}$), which are clearly distinct in space and velocity. The HVC may be a highly collimated jet presumed from its narrow velocity width and high velocity. The LVC, on the other hand, may be a widely opened disk wind inferred from its broad velocity width and low velocity. The spectrum taken perpendicular to the L1551 IRS 5 outflow at its base shows that the LVC has a spatially wide subcomponent, supporting the above interpretation. We demonstrated that the [Fe II] 1.644 $\mu$ spectroscopy is a very powerful tool for the studies of fast jets and winds that directly emanate from star-disk systems.

• 한국과학교육학회지
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• 제26권1호
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• pp.68-87
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• 2006

본 연구에서는 예비 초등 교사들을 대상으로 천문현상(계절 변화와 달의 위상변화)에 대한 정신모형과 그 모형에 영향을 주는 요소들을 조사하였다. 본 연구에 참여한 예비교사는 교육대학교에 재학 중인 학생이다. 자료 수집은 지필 검사와 개별 면담을 통해 이루어졌다. 연구 결과, 예비 초등 교사들은 천문현상의 설명들이 과학적 모형과는 다른 합성 정신모형들을 가지고 있었으며, '거리 이론' 과 '가리기 이론'이 그들의 정신 모형에 가장 큰 영향을 미치는 것으로 나타났다. 또한 예비 초등 교사들이 갖는 천문현상의 합성 정신모형의 구조와 근원을 알아보기 위하여 그들의 정신 모형들을 형성하는 틀 이론과 특정 이론을 집중적으로 탐색하였다. 끝으로 연구 결과와 관련된 예비 교사교육에의 시사점을 논하였다.

• 한국해안·해양공학회논문집
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• 제27권3호
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• pp.149-158
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• 2015

경기만 한강하구에서 주요 수로의 조석 전파 특성을 이용하여, 천문조, 배조 및 복합조의 분포를 파악하고, 조석 형태수의 특징에 따라 구역별 조석체계 (tidal regime)를 분류하였다. 주요 수로에서 보이는 조석 전파 특성은 외해는 천문조로 대표되는 5대분조 (e.g., $M_2$, $S_2$, $N_2$, $K_1$ 및 $O_1$)가 지배적이지만, 상류로 진입할수록 천해 분조 (e.g., $M_4$)와 장주기 분조 (e.g., $MS_f$)의 뚜렷한 증가가 보인다. 반일주조 성분이 우세한 경기만 및 한강하구에서 천문조, 배조 및 복합조를 이용하여 제시된 조석 형태수 (tidal form number)의 특성에 따라 크게 3구역으로 분류하였다. 1구역은 천문조가 우세한 지역으로 외해에서 인천항 전면까지 (염하수로), 외해에서 석모수로의 북쪽 입구로 제시된다. 2구역은 염하수로 남쪽 입구에서 북쪽 입구까지와 강화 북수로 지역으로 단주기 천해 분조 (e.g., $M_4$와 $MS_4$)가 강하게 나타나는 지역이다. 마지막으로 3구역은 신곡 수중보 이후부터 한강 상류지역으로 장주기 복합조 (e.g., $MS_f$)가 제일 우세한 지역이다. 일반적인 하구와 마찬가지로 한강하구의 조석 비선형성은 지형적 특성에 기인한 천해 분조가 증가를 하며, 1/4일주기 (fourth-diurnal) 및 장주기 (long-term period) 분조의 확연한 분포 차이를 보인다. 특히, 수중보의 영향은 구조물의 상류와 하류지점의 조석체계에 지대한 변화를 일으킨다.

• 천문학회지
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• 제48권5호
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• pp.299-311
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• 2015

We report first results from KVN and VERA Array (KaVA) VLBI observations obtained in the frame of our Plasma-physics of Active Galactic Nuclei (PAGaN) project. We observed eight selected AGN at 22 and 43 GHz in single polarization (LCP) between March 2014 and April 2015. Each source was observed for 6 to 8 hours per observing run to maximize the uv coverage. We obtained a total of 15 deep high-resolution images permitting the identification of individual circular Gaussian jet components and three spectral index maps of BL Lac, 3C 111 and 3C 345 from simultaneous dual-frequency observations. The spectral index maps show trends in agreement with general expectations – flat core and steep jets – while the actual value of the spectral index for jets shows indications for a dependence on AGN type. We analyzed the kinematics of jet components of BL Lac and 3C 111, detecting superluminal proper motions with maximum apparent speeds of about 5c. This constrains the lower limits of the intrinsic component velocities to ~ 0.98c and the upper limits of the angle between jet and line of sight to ~20°. In agreement with global jet expansion, jet components show systematically larger diameters d at larger core distances r, following the global relation d ≈ 0.2r, albeit within substantial scatter.

• 천문학회보
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• 제42권1호
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• pp.28.1-28.1
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• 2017

To investigate AGN outflows as a tracer of AGN feedback on the host galaxies, we perform integral-field spectroscopy of 20 type 2 AGNs at z<0.1 using the Magellan/IMACS and the VLT/VIMOS. The observed objects are luminous AGNs with the [O III] luminosity >$10^{41.5}erg/s$, and exhibit strong outflow signatures in the [O III] kinematics. We obtain the maps of the narrow and broad components of [O III] and $H{\alpha}$ lines by decomposing the emission-line profile. The broad components in both [O III] and $H{\alpha}$ represent the non-gravitational kinematics, (i.e., gas outflows), while the narrow components represent the gravitational kinematics (i.e., rotational disks), especially in $H{\alpha}$. By using the spatially integrated spectra within the flux-weighted size of the narrow-line region, we estimate the outflow energetics. The ionized gas mass is $(1.0-38.5){\times}10^5M_{\odot}$, and the mean mass outflow rate is $4.6{\pm}4.3M_{\odot}/yr$, which is a factor of ~260 higher than the mean mass accretion rate $0.02{\pm}0.01M_{\odot}/yr$. The mean energy injection rate is $0.8{\pm}0.6%$ of the AGN bolometric luminosity Lbol, while the mean momentum flux is $(5.4{\pm}3.6){\times}L_{bol}/c$, except for two most kinematically energetic AGNs. The estimated energetics are consistent with the expectations for energy-conserving outflows from AGNs, yet we do not find any supporting evidence of instantaneous star-formation quenching due to the outflows.