• 천문학논총
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• 제25권1호
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• pp.23-28
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• 2010

We present results of a test-study of the large-scale survey using the multi-beam receiver system recently installed on the 14 m telescope at Taeduk Radio Astronomy Observatory (TRAO). We have tested several modes of mapping, and found suitable (time-saving) mapping parameters of 'ON-SOURCE' = 8, 'OFF-SOURCE' = 1 when using 'RPT' = 3 as a position-switching mode. We observed 504 spectra towards the NGC 7538, a star forming molecular cloud in the transition of J = 1 - 0 of $^{12}CO$. From the Outer Galaxy Survey database (Heyer et al., 1998) we obtained 504 spectra for the same region. We compared integrated intensities, line profiles of two databases, and found that they are consistent to each other. From the intensity ratio of these two databases we also found that the value of forward spillover scattering of the TRAO telescope system is 0.58.

• 천문학논총
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• 제28권1호
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• pp.7-13
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• 2013

We present a multi-dimensional reduction method of the surveyed cube database obtained using a single- dish radio telescope in Taeduk Radio Astronomy Observatory (TRAO). The multibeam receiver system installed at the 14 m telescope in TRAO was not optimized at the initial stage, though it became more stabilized in the following season. We conducted a Galactic Plane survey using the multibeam receiver system. We show that the noise level of the first part of the survey was higher than expected, and a special reduction process seemed to be definitely required. Along with a brief review of classical methods, a multi-dimensional method of reduction is introduced; It is found that the 'background' task within IRAF (Image Reduction and Analysis Facility) can be applied to all three directions of the cube database. Various statistics of reduction results is tested using several IRAF tasks. The rms value of raw survey data is 0.241 K, and after primitive baseline subtraction and elimination of bad channel sections, the rms value turned out to be 0.210 K. After the one-dimensional reduction using 'background' task, the rms value is estimated to be 0.176 K. The average rms of the final reduced image is 0.137 K. Thus, the image quality is found to be improved about 43% using the new reduction method.

• 한국광학회지
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• 제35권4호
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• pp.143-149
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• 2024

대기 중을 진행하는 레이저 빔에 대기 요동이 미치는 영향을 단일 위상판 모델 및 다수 위상판 모델로 분석하고 비교하였다. 파장이 1064 nm 이고 반지름이 10 mm인 레이저 빔을 1인치 광학계로 시준하여 3 km를 진행하는 경우에 대해 대기 요동 강도를 나타내는 구조 상수 C_n²를 10^-17부터 10^-14까지 변화시켜가며 단노출 빔 형상을 단일 및 다수 위상판 모델로 확인하였다. 구조 상수에 따른 레이저 빔의 변화를 정량화하기 위해 장노출에 대한 유효 수광 출력과 빔 크기 값을 사용하였으며, 구조 상수가 증가함에 따라 이 값들은 단일 및 다수 위상판 모델에서 공통적으로 증가하는 경향을 보였다. 구조 상수인 C_n²가 2×10^-15보다 작은 경우 하나의 위상판 사용 대비 다수의 위상판 사용 사이에 1.5% 이내의 장노출 유효 수광 출력과 빔 크기 차이만 발생하였지만, 그 이상인 경우 결과값의 차이가 지속적으로 증가하였다. 즉 3 km 진행하는 레이저빔은 구조 상수 2×10^-15 이상에서 다수 위상판 모델을 사용해야 함을 확인하였다.

• International Journal of Aeronautical and Space Sciences
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• 제12권2호
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• pp.175-178
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• 2011

An optical fiber-based beam width measurement technique is presented. The proposed system can be applied to the optical fiber industry in applications such as lensed fiber, optical fiber based laser beam source, and fiber optic sensor. The measurement system is composed of optical fiber, which is used as a transceiver, and a single grating panel which consists of a multi-reflection area with an even non-reflection area. The grating panel is used to vary the reflected light. When the widths of the reflection area and non-reflection area are larger than the optical beam width, the reflected light is varied at the interface between the reflection area and the non-reflection area by the movement of the grating panel. Experiments were conducted in order to verify the feasibility of the proposed technique. Multi-mode fiber combined with a collimator was selected as an emitter and a receiver, and the beam width measurement system was contrived. Subsequently, the proposed method and the system were verified by comparing the experimental results with the results of the conventional charge-coupled device technique.

• 한국정보통신학회논문지
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• 제21권3호
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• pp.491-498
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• 2017

GPS (global positioning system)는 지구 궤도를 도는 여러 GPS 위성의 신호를 수신하여 위성 별 수신 시간 차이를 이용하여 자신의 절대 위치를 알아내는 시스템으로 민간 목적뿐만 아니라 군용 목적으로도 널리 사용되고 있다. 특히 유도무기 등에 사용되기 때문에 신뢰성 있는 GPS 수신은 군에서 훨씬 더 중요하다. 하지만 GPS 는 사용 주파수 대역이 알려져 있고 수신신호 전력이 미약하기 때문에 인위적인 재밍신호를 송출하여 쉽게 GPS 시스템을 무력화 시킬 수 있는 문제가 있다. 이러한 간섭신호에 대응하기 위한 한 가지 방법은 GPS 수신기에 다중 안테나를 설치하고 디지털 빔포밍 기술을 이용하여 GPS 신호는 훼손하지 않으면서 재머만을 제거하는 기술이다. 본 논문에서는 MVDR(minimum variance distortionless response) 기술에 기반하여 새로운 적응형 빔 제어 기술을 제안한다. 제안하는 방식은 알려져 있는 위성 방향으로의 빔을 형성하고 재머 방향으로는 적응형 알고리즘에 의해 널을 형성하여 재머를 제거한다. 제안하는 방식의 성능은 컴퓨터 모의실험을 통해 검증한다.

• 전자공학회논문지
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• 제50권8호
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• pp.53-60
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• 2013

이 논문에서는 Pre-FFT 빔 형성기를 가진 MIMO(Multi-Input Multi-Out)-OFDM(Orthogonal Frequency Division Multiplexing)시스템 구조에 적합한 적응 빔 형성기법과 결합된 전력제어 기법을 제안한다. 제안된 전력제어 기법과 적응 빔 형성기법이 결합되어 송신전력을 제어하는 과정과 빔형성기 계수를 갱신하는 과정이 시간적으로 함께 iterative하게 이루어져서 수렴하게 되면 원하는 방향으로 빔이 형성되고 각 부반송파별로 원하는 SNIR 값에 수렴하게 되어 다중 사용자 환경에서 성능개선 효과를 얻을 수 있다. Pre-FFT 빔 형성기를 가진 MIMO-OFDM 시스템에 전력 제어기법을 결합할 경우 시스템의 성능 개선 효과를 모의 실험을 통하여 확인한다.

• 천문학회보
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• 제41권2호
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• pp.38.1-38.1
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• 2016

TRAO has been newly equipped with a multi-beam receiver system, 16 pixel MMIC preamplifiers in a $4{\times}4$ array, a FFT spectrometer, and new control computer systems. In our new receiver systems one can make simultaneous observations with two molecular lines maximum 15 GHz apart with a spectral band width of 60 MHz. Typical system temperatures are about 160 - 200 K at 86 ~ 100 KHz and 400 - 500 K at 115 GHz in the dry weather. The new systems using On-The-Fly mode were found to be very efficient in making quick and sensitive maps of large clouds with a high velocity resolution (~0.04 km/s at 100 GHz). TRAO now calls for proposals for 2016 and 2017 observing season for everybody. In the talk we will introduce the current status of TRAO upgrade and its scientific preliminary results.

• 천문학회지
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• 제52권6호
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• pp.227-233
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• 2019

We report the performance of the 13.7-meter Taeduk Radio Astronomy Observatory (TRAO) radio telescope. The telescope has been equipped with a new receiver, SEQUOIA-TRAO, a new backend system, FFT2G, and a new VxWorks operating system. The receiver system features a 16-pixel focal plane array using high-performance MMIC preamplifiers; it shows very low system noise levels, with system noise temperatures from 150 K to 450 K at frequencies from 86 to 115 GHz. With the new backend system, we can simultaneously obtain 32 spectra, each with a velocity coverage of 163 km s^-1 and a resolution of 0.04 km s^-1 at 115 GHz. The new operating system, VxWorks, has successfully handled the LMTMC-TRAO observing software. The main observing method is the on-the-fly (OTF) mapping mode; a position-switching mode is available for small-area observations. Remote observing is provided. The antenna surface has been newly adjusted using digital photogrammetry, achieving a rms surface accuracy better than 130 ㎛. The pointing uncertainty is found to be less than 5" over the entire sky. We tested the new receiver system with multi-frequency observations in OTF mode. The aperture efficiencies are 43±1%, 42±1%, 37±1%, and 33±1%, the beam efficiencies are 45±2%, 48±2%, 46±2%, and 41±2% at 86, 98, 110, and 115 GHz, respectively.

• 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.