• 천문학회보
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• 제42권2호
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• pp.56.3-56.3
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• 2017

The Breakthrough Starshot initiative aims to launch gram-scale spacecraft to a speed of v~0.2c, capable of reaching Alpha Centauri and seeing the Earth-like exoplanet, Proxima b, from close distance, in about 20 years. However, a critical challenge for the initiative is the effects of interstellar matter and magnetic field to the relativistic spacecraft during the journey. In this talk, I will first present our evaluation for the damage to the spacecraft by interstellar gas and dust based on a detailed analysis of the interaction of a relativistic spacecraft with the ISM. Second, I will discuss the deflection and oscillation of spacecraft by interstellar magnetic fields. Third, I will discuss the gas drag fore at high energy regime and quantify its effect on the slowing down of the relativistic lightsails. Finally, we will discuss practical strategies to mitigate the damage by interstellar dust and to maintain the spacecraft aiming at the intended target.

• 천문학회보
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• 제36권2호
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• pp.62.1-62.1
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• 2011

We investigate various physical parameters of the narrow-line region (NLR) of two type I QSOs, PG1012+008 and PG1307+085. Using the spectra obtained with the FORS1 at the VLT with an excellent seeing condition (<0.7"), we can extract spectra with varying distances from the center out to the galactic scales. From these spectra we derive physical quantities such as reddening, temperature, electron density, and ionization parameter as a function of distance from the center. We also explore the possibility of defining the size of the NLR with line ratio diagnostics regardless of starbursts, shock-ionized gas, or tidal tails.

• 천문학회보
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• 제36권1호
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• pp.53.1-53.1
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• 2011

We investigate the radial properties of the narrow-line region (NLR) in two radio-quiet quasars, PG1012+008 and PG1307+085, using the spectra obtained with the FORS1 at the Very Large Telescope. These high quality spectra with seeing < 0.6" enable us to extract seven two-pixel (0.4") spectra as a function of the radial distance from the accretion disk. In contrast to [OIII] narrow-band imaging, which can be contaminated by starbursts, shock-ionized gas, and tidal tails, we use emission-line diagnostic to determine the true size of the AGN-excited NLR. In this poster, we present the results based on the radial variance of $H{\beta}$ to [OIII] ${\lambda}5007$ ratio. For both targets, the [OIII] emission line exhibits a blue wing, suggesting an outflow of gas. In the case of PG1307+085, the blue wing disappears at the distance of 1". We will discuss the properties of the NLR in detail.

• 천문학회보
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• 제44권2호
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• pp.35.1-35.1
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• 2019

One day, a galaxy study suddenly came to me and became a friend of 40 years. The study of galaxies, which began with surface photometry of nearby galaxies, ended up in galaxy morphology through chemical and dynamical evolution of galaxies. All that deviated from the study of galaxies was the study of the open clusters. So it seems to me that I devoted my entire life to the study of galaxies. The most memorable one is the observation at Sobaeksan Observatory. Even though the heavy snow fell, I climbed Sobaeksan to meet galaxies. Galaxies observed at Kiso Observatory, DAO, and BOAO are now beyond memory, but I still enjoy seeing them. There are many memories, but the biggest pleasure I've had in my galaxy studies is when I've encountered the galactic conformity between host and its satellite galaxies. Eureka! Now the night sky is changing from the object of study to the object of awe. I will share this joy.

• 천문학회보
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• 제45권1호
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• pp.67.1-67.1
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• 2020

Adaptive Optics (AO) is the technology for ground-based telescopes to overcome the interference caused by atmospheric turbulence. We are developing an AO system for the 1-m telescope at Seoul National University Observatory (SNUO). The seeing size of the SNUO is 2 arcseconds on average, and 0.85 arcseconds at best condition. Our system is based on MEMS deformable mirror and Shack-Hartmann wavefront sensor. We developed the wavefront sensor using a cheap CMOS camera, and measured phase disturbance at SNUO. To verify the performance of the AO system, we designed an artificial phase disturber that produces similar scale phase error, measured at SNUO. We carried out laboratory tests in which the AO system measures and corrects the wavefront using the phase disturber and an F/6 light source, the same as that of SNUO telescope. The control system was developed in C++. The system performs closed-loop PI correction up to 100 Hz at a consumer-grade PC.

• 응용통계연구
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• 제29권6호
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• pp.1107-1116
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• 2016

최근의 탐사 천문학 관측으로부터 대용량 관측 자료가 획득되면서, 기존의 일상적인 자료 분석 방법에 큰 변화가 있었다. 고전적인 통계적인 추론과 더불어 기계학습 방법들이, 자료의 표준화로부터 물리적인 모델을 추론하는 단계까지 자료 분석의 전 과정에서 활용되어 왔다. 적은 비용으로 대형 검출 기기들을 이용할 수 있게 되고, 더불어서 고속의 컴퓨터 네트워크를 통해서 대용량의 자료들을 쉽게 공유할 수 있게 되면서, 기존의 다양한 천문학 자료 분석의 문제들에 대해서 기계학습을 활용하는 것이 보편화되고 있다. 일반적으로 대용량 천문학 자료의 분석은, 자료의 시간과 공간 분포가 가지는 비 균질성 때문에 야기되는 효과를 고려해야 하는 문제를 가진다. 오늘날 증가하는 자료의 규모는 자연스럽게 기계학습의 활용과 더불어 병렬 분산 컴퓨팅을 필요로 하고 있다. 그러나 이러한 병렬 분산 분석 환경의 일반적인 자료 분석에서의 활용은 아직 활발하지 않은 상황이다. 천문학에서 기계학습을 사용하는데 있어서, 충분한 학습 자료를 관측을 통해 획득하는 것이 어렵고, 그래서 다양한 출처의 자료를 모아서 학습 자료를 수집해야 는 것이 일반적이다. 따라서 앞으로 준 지도학습이나 앙상블 학습과 같은 방법의 역할이 중요해 질 것으로 예상된다.

• Current Optics and Photonics
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• 제2권3호
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• pp.269-279
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• 2018

We are currently investigating the feasibility of a 1.6 m telescope with a laser-guide star adaptive optics (AO) system. The telescope, if successfully commissioned, would be the first dedicated adaptive optics observatory in South Korea. The 1.6 m telescope is an f/13.6 Cassegrain telescope with a focal length of 21.7 m. This paper first reviews atmospheric seeing conditions measured over a year in 2014~2015 at the Bohyun Observatory, South Korea, which corresponds to an area from 11.6 to 21.6 cm within 95% probability with regard to the Fried parameter of 880 nm at a telescope pupil plane. We then derive principal seeing conditions such as the Fried parameter and Greenwood frequency for eight astronomical spectral bands (V/R/I/J/H/K/L/M centered at 0.55, 0.64, 0.79, 1.22, 1.65, 2.20, 3.55, and $4.77{\mu}m$). Then we propose an AO system with a laser guide star for the 1.6 m telescope based on the seeing conditions. The proposed AO system consists of a fast tip/tilt secondary mirror, a $17{\times}17$ deformable mirror, a $16{\times}16$ Shack-Hartmann sensor, and a sodium laser guide star (589.2 nm). The high order AO system is close-looped with 2 KHz sampling frequency while the tip/tilt mirror is independently close-looped with 63 Hz sampling frequency. The AO system has three operational concepts: 1) bright target observation with its own wavefront sensing, 2) less bright star observation with wavefront sensing from another bright natural guide star (NGS), and 3) faint target observation with tip/tilt sensing from a bright natural guide star and wavefront sensing from a laser guide star. We name these three concepts 'None', 'NGS only', and 'LGS + NGS', respectively. Following a thorough investigation into the error sources of the AO system, we predict the root mean square (RMS) wavefront error of the system and its corresponding Strehl ratio over nine analysis cases over the worst ($2{\sigma}$) seeing conditions. From the analysis, we expect Strehl ratio >0.3 in most seeing conditions with guide stars.

• 천문학회지
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• 제37권5호
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• pp.349-353
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• 2004

Magnetic fields are an important ingredient of galaxy clusters and are indirectly observed on cluster scales as radio haloes and radio relics. One promising method to shed light on the properties of cluster wide magnetic fields is the analysis of Faraday rotation maps of extended extragalactic radio sources. We developed a Fourier analysis for such Faraday rotation maps in order to determine the magnetic power spectra of cluster fields. In an advanced step, here we apply a Bayesian maximum likelihood method to the RM map of the north lobe of Hydra A on the basis of our Fourier analysis and derive the power spectrum of the cluster magnetic field. For Hydra A, we measure a spectral index of -5/3 over at least one order of magnitude implying Kolmogorov type turbulence. We find a dominant scale of about 3 kpc on which the magnetic power is concentrated, since the magnetic autocorrelation length is ${\lambda}_B = 3 {\pm} 0.5\;kpc$. Furthermore, we investigate the influences of the assumption about the sampling volume (described by a window function) on the magnetic power spectrum. The central magnetic field strength was determined to be ${\~}7{\pm}2{\mu}G$ for the most likely geometries.

• 천문학회지
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• 제46권4호
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• pp.161-172
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• 2013

A focal reducer is developed for CQUEAN (Camera for QUasars in EArly uNiverse), which is a CCD imaging system on the 2.1 m Otto Struve telescope at the McDonald observatory. It allows CQUEAN to secure a wider field of view by reducing the effective focal length by a factor of three. The optical point spread function without seeing effects is designed to be within one pixel ($0.283^{\prime\prime}$) over the field of view of $4.82^{\prime}{\times}4.82^{\prime}$ in optimum wavelength ranges of 0.8-1.1 ${\mu}m$. In this paper, we describe and discuss the characteristics of optical design, the lens and barrel fabrications and the alignment processes. The observation results show that the image quality of the focal reducer confirms the expectations from the design.

• 천문학회보
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• 제42권2호
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• pp.70.3-70.3
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• 2017

맑은 날에도 엷은 상층운이나 난류의 방해로 관측 품질이 저해되는 등 천문 분야는 대기환경에 민감하나, 하층 대기 상태에 비중을 두는 동네예보만으로는 천문 분야의 기상정보에 대한 수요를 충족하기에는 한계가 있다. 이에 천문 관측 환경에 보다 특화된 별밤예보를 개발하여 천체 관측 가능성과 천문 관측 자료의 품질을 좌우하는 대기상태를 UM 국지모델 생산자료를 바탕으로 예보하고자 한다. 예보 요소는 하늘상태(운량), 시상(seeing), 투명도, 암도(darkness) 및 대기청명지수, 풍속, 기온, 습도이다. 대기청명지수는 일반인이 관찰하기 좋은지 여부를 한 눈에 알 수 있게 운량과 투명도, 암도를 종합한 지수로 10~100까지 10단계로 제공할 계획이다. 하늘상태와 풍속, 기온, 습도는 $5{\times}5km$격자마다 제공되는 기상청 동네예보에서 천문대와 가장 가까운 격자의 예보치를 추출하였다. 시상은 대기의 난류 정도에 좌우된다. 그러나 충북의 고층기상 관측자료가 없어서, 시상 예보식을 만들기 위해 UM 국지모델에서 제공하는 각 등압면의 기온과 바람벡터로부터 정적 안정도(온위 경도)와 연직 바람시어를 유도한 뒤, 다중회귀분석으로 시상 예보식을 구하였다. 또한 대기청명지수는 청주기상지청에서 관측한 운량과 밤하늘 밝기 자료를 종속변수, 별의 개수를 독립변수로 하는 다중회귀예측식을 구하였다.