• 한국지형학회지
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• 제20권4호
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• pp.15-28
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• 2013

본고는 2012년 11월 14일부터 25일까지 10일간 남미대륙의 파타고니아와 아타카마 지역을 중심으로 한 안데스 산지를 답사한 후 그곳에서 관찰된 지형경관에 대해 지오투어리즘 관점에서 고찰한 것이다. 파타고니아 지형경관은 칠레의 토레스델파이네 국립공원과 아르헨티나의 로스 빙하국립공원에서, 그리고 아타카마 지형경관은 칠레의 산페드로데아타카마를 중심으로 한 지역에서 주로 관찰되었다. 파타고니아는 세계에서 가장 빠른 융기율을 나타내고 있는 곳 중의 한 곳으로 위의 두 개 국립공원에는 반건조지형과 융기지형 그리고 빙식지형이 매우 잘 발달되어 있다. 특히, 파이네와 피츠로이 암봉군은 관입에 의한 화강암 빙식지형의 백미를 보여주고 있어 두 곳 모두 유네스코 세계자연유산으로 등록된 곳이기도 하다. 한편, 아타카마 사막은 악지와 염호, 간헐천 등 사막과 화산경관이 공존해 있는 독특한 지형경관이 발달된 곳이다. 그 이유는 아타카마 사막이 산페드로데아타카마 동쪽의 화산호(弧)와 해성층의 융기로 형성된 대륙붕단 사이의 전호분지에 위치하고 있기 때문이다. 또한 응결응회암 완사면, 선상지면 등으로 형성된 페디플레인이 곳곳의 페디멘트와 어우러져 건조지형의 전형을 잘 나타내 주고 있기도 하다. 파타고니아와 아타카마는 남미판과 태평양판의 충돌로 인해 형성된 안데스 산지가 만든 매우 다양한 지형경관이 발달된 최적의 지리여행지이다.

• 천문학회보
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• 제40권2호
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• pp.44.1-44.1
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• 2015

We set up a project to make spectrometers for single dish observations of the Korean VLBI Network (KVN), a new future multi-beam receiver of the ASTE (Atacama Submillimeter Telescope Experiment), and the total power (TP) antennas of the Atacama Large Millimeter/submillimeter Array (ALMA). Traditionally, spectrometers based on ASIC (Application-Specific Integrated circuit) and FPGA (Field-Programmable Gate Array) have been used in radio astronomy. It is, however, that a Graphics Processing Unit (GPU) technology is now viable for spectrometers due to the rapid improvement of its performance. A high-resolution spectrometer should have the following functions: poly-phase filter, data-bit conversion, fast Fourier transform, and complex multiplication. We wrote a program based on CUDA (Compute Unified Device Architecture) for a GPU spectrometer. We measured its performance using two GPU cards, Titan X and K40m, from NVIDIA. A non-optimized GPU code can process a data stream of around 2 GHz bandwidth, which is enough for the KVN spectrometer and promising for the ASTE and ALMA TP spectrometers.

• 천문학회보
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• 제39권2호
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• pp.116.1-116.1
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• 2014

Korea officially joined the ALMA (Atacama Large Millimeter/submillimeter Array) project on August 17, 2014. Korea was allowed to apply for the Cycle 2 call-for-proposal before joining the project. Korea submitted 17 proposals, and 4 of them were selected as high-priority. The fund of an 11-year Korean ALMA project in the KASI (Korea Astronomy and Space Science Institute) was approved. The project team formulated an ARC (ALMA Regional Center) node at the KASI and already started its supporting activities for the Korean Astronomical Society. The team also set up a future development plan for ASTE (Atacama Submillimeter Telescope Experiment) and ALMA. A couple of engineers are now doing concept design of a multi-beam receiver system for the ASTE, Because of the ALMA participation, Korea could also access open-use time of ASTE and Mopra telescopes organized by Japan. As of this writing, EACOA (East Asia Core Observatories Association) is now under discussion on making an organization called "East Asian Observatory" and the possible operation of JCMT (James Clerk Maxwell Telescope). I will briefly mention the future prospect of these activities.

• 천문학논총
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• 제30권2호
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• pp.617-620
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• 2015

This paper presents an overview of the large international projects in which the National Astronomical Observatory of Japan is involved, namely, the Subaru Telescope, Atacama Large Millimeter/submillimeter Array, and the Thirty Meter Telescope. The last section provides a brief historical view of the international collaboration in East Asia regions over the last 20 years.

• 천문학회보
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• 제42권1호
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• pp.39.1-39.1
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• 2017

Protoplanetary disks (PPDs) are a natural consequence of star formation and play crucial roles in planet formation. Atacama Large Millimeter/submillimeter Array (ALMA) has provided sub-mm data for the PPDs with a high angular resolution and sensitivity, and it makes us enable to study PPDs in detail. We have developed Packages of Unified modeling for Radiative transfer, gas Energetics, and Chemistry (PUREC), which consists of a self-consistent thermo-chemical model and line and continuum radiative transfer models, in order to interpret and predict the ALMA observations for PPDs. In this talk, we introduce capabilities of PUREC.

• 천문학회지
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• 제54권6호
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• pp.171-182
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• 2021

The lack of short baselines, referred to as the short-spacing problem (SSP), is a well-known limitation of the performance of radio interferometers, causing a reduction of the flux detected from source structure on large angular scales. The very large number of antennas operated in the Atacama Large Millimeter/sub-millimeter Array (ALMA) generates situations for which the impact of the SSP takes a complex form, not simply measurable by a single number, such as the maximal recoverable scale. In particular, extended antenna configurations, complemented by a small group of closeby antennas at the centre of the array, may result in a double-humped baseline distribution with a significant gap between the two groups. In such cases one should adopt as the effective maximal recoverable scale the one associated with the extended array and use only the central array to recover missing flux, as one would do with single dish or ACA (Atacama Compact Array) observations. The impact of the missing baselines can be very important and may easily be underestimated, or even overlooked. The present study uses ALMA archival data of the ²⁹SiO(8-7) line emission of the AGB star W Hydrae for a demonstration. A critical discussion of the reliability of the observations away from the star is presented together with comments of a broader scope. Properties of the circumstellar envelope of W Hya within ~15 au from the star, many of which are not mentioned in the published literature, are briefly described and compared with R Doradus, an AGB star having properties very similar to W Hya.

• 천문학회보
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• 제40권1호
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• pp.81.4-82
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• 2015

ALMA(Atacama Large Millimeter/submillimeter Array)의 고분해능 분광관측을 통해 천체에 존재하는 분자에 관한 다양한 정보를 얻을 수 있었고, 이러한 분자들을 형성하는 화학적 반응 메커니즘을 이해하는 것이 천체 현상을 이해하는 데 중요한 부분을 차지하게 되었다. 이러한 노력의 일환으로, 천체에서의 화학반응을 연구하기 위한 몇몇 코드가 개발되었는데 그중에 대표적인 것이 Astrochem 코드이다. 이 코드는 천체에 존재 할 수 있는 화학물질들의 분포변화를 시간에 따른 함수로 계산하는데, 이를위해 다양한 분자들을 형성하는 것으로 알려진 화학반응 데이터베이스인 KIDA, OSU를 활용한다. 이번 포스터에서는 Astrochem 코드를 이용해 얻을 수 있는 결과인 비교적 간단한 분자들의 시간에 따른 분포 변화를 발표한다. 향후 연구 방향은 유체역학 코드와 Astrochem 코드를 결합한 유체-천체화학 코드를 개발하는 것이며 이를 활용해 유체역학 현상이 다양한 분자들의 분포 변화에 어떠한 영향을 미치는지를 연구할 것이다. 이를 통해 보다 정확하게 천체 현상들을 예측 및 재현 가능할 것으로 기대된다.

• 천문학회보
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• 제40권1호
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• pp.67.2-67.2
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• 2015

We report Atacama Large Millimeter/submillimeter Array (ALMA) cycle I observations of L1527, a class 0 object with an infalling envelope and a rotating disk. HCO+ and HCN J=4-3 show strong redshifted absorption against the bright continuum emission associated with the optically thick disk or inner envelope. This redshifted absorption dip is an unambiguous evidence of infall. In addition, these lines and CS J=7-6 present the Keplerian rotation profile at their position-velocity diagrams, suggesting the formation of a Keplerian disk very early in star formation. We will present a model combining an infalling envelope and a Keplerian disk to fit the ALMA observations.

• 천문학회보
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• 제39권2호
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• pp.116.2-116.2
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• 2014

As Korean engineering contribution to ALMA enhancement, development of focal plane arrays(FPAs) for the total power array in ALMA compact array has been projected mainly to increase mapping speed in interferometric multi-pointing observation(mosaicking). To tackle engineering issues expected in order to be compatible with the existing ALMA receivers, we plan to develop a prototype 300-500 GHz heterodyne FPA system including a software spectrometer using GPU clusters for ASTE(Atacama Submillimeter Telescope Experiment) telescope by 2017.

• 천문학논총
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• 제33권2호
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• pp.21-30
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• 2018

Formation processes of high-mass stars have been long-standing issues in astronomy and astrophysics. This is mainly because of major difficulties in observational studies such as a smaller number of high-mass young stellar objects (YSOs), larger distances, and more complex structures in young high-mass clusters compared with nearby low-mass isolated star-forming regions (SFRs), and extremely large opacity of interstellar dust except for centimeter to submillimeter wavelengths. High resolution and high sensitivity observations with Atacama Large Millimeter/Submillimeter Array (ALMA) at millimeter/submillimeter wavelengths will overcome these observational difficulties even for statistical studies with increasing number of high-mass YSO samples. This review will summarize recent progresses in high-mass star-formation studies with ALMA such as clumps and filaments in giant molecular cloud complexes and infrared dark clouds (IRDCs), protostellar disks and outflows in dense cores, chemistry, masers, and accretion bursts in high-mass SFRs.