• 천문학회보
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• 제40권1호
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• pp.41.2-41.2
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• 2015

Steward Observatory has a rich and diverse program of investigations, with significant groups working on star and planet formation and astrobiology, galaxy and quasar formation and evolution, technology for adaptive optics and interferometry, computational astrophysics, and effectiveness of educational practice. To support this work, Steward operates and offers a range of observational and other facilities, including the Large Binocular Telescope, the MMT, the Magellan Telescopes, the Arizona Radio Observatory, and a suite of 1- and 2-m class telescopes. A special opportunity for IR astronomy exists with Arizona now running UKIRT. Steward Observatory astronomers would welcome the opportunity to form genuine scientific collaborations that are mutually beneficial for high-impact projects and improving the observing facilities.

• 대한전자공학회:학술대회논문집
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• 대한전자공학회 2003년도 하계종합학술대회 논문집 V
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• pp.2681-2684
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• 2003

본 연구에서는 전파천문학에 있어서 스펙트로그램을 얻기 위한 장치인 필터뱅크의 고속 데이터 취득에 관한것이다. 여기서는 FPGA를 기반으로 데이터 취득시스템을 설계하였는데, 기존의 모노리틱 IC 를 기반으로 설계된 데이터 I/O 를 FPGA 로 대체함으로써 부피를 적게하고 데이터의 고속처리를 가능하게 하였다. 우주현상을 관측함에 있어 고속으로 데이터를 처리함은 대기중의 불안정한 상태나 시스템의 불안정에 의한 좋지 않은 데이터를 정확히 선택하여 제거할 수 있는 데이터 시간 분활이 가능하게 한다. 본 논문에서 개발된 시스템을 적용하여 기존 시스템에 비하여 약 15 배 정도의 고속 데이터 처리가 가능하게 되었다.

• 천문학회보
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• 제42권1호
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• pp.58.2-58.2
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• 2017

2013년 청소년 교육목적으로 개발된 고흥전파간섭계시스템을 활용하여 청소년으로 하여금 전파관측을 체험케하고, 전파천문학 연구 기회를 제공하고자 한다. 안정된 단일경 전파관측과 간섭계모드 전파관측을 위해 현 시스템이 갖추어야 할 기능을 개선하고 있다. 보다 정밀하게 관측대상을 추적하고, 전파 점광원을 관측할 수 있도록 새로운 전파관측시스템을 개발한다. 정밀한 관측대상 추적과 함께 데이터 취득 시간을 확장하여 점광원 관측이 가능하게 되면, 청소년에게 전파관측 및 전파간섭원리와 관측방법을 실험체험 프로그램으로 전해 줄 수 있다.

• 천문학회지
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• 제27권1호
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• pp.55-60
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• 1994

The 3mm transitions to CO, $^{13}CO,\;CS,\;HCO^+$, and HCN have been observed toward the compact HII regions in W58 using the 14m Daeduk Radio Telescope (DRT). Some of the observed lines show high-velocity wings resulted from outflowing materials of the compact HII regions. We derive the beam averaged column densities of the observed species and compare their relative abundances. The $HCO^+$ abundance appears to be smaller by about an order of magnitude than those of 'typical' quiet molecular clouds. CS may be a good reference molecule in comparing relative abundances in different physical conditions.

• 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.

• 천문학논총
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• 제13권1호
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• pp.129-134
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• 1998

Observations of the J=1-0 transition line of HCN were made at the center of Comet C/1995 O1 (Hale-Bopp) from November, 1996 to April, 1997 with the 14-m radio telescope at the TRAO (Taeduk Radio Astronomical Observatory). From the obtained data, an HCN production rate at each observed date was derived. The rapid variation of the HCN production rate near the perihelion was detected, and it is thought to be caused by jet(s) from the nucleus. The correlation between the visual magnitude and the HCN production rate is found to be $Q_{HCN}=27.03-0.11(m_v-5log{\Delta})$.

• 천문학회지
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• 제23권2호
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• pp.85-96
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• 1990

High resolution $^{12}CO$ observations of the region containing the planetary nebula Hb12 were made with the Nobeyama Radio Telescope. These observations reveal that there is no significant CO emission from Hb 12 itself. Near Hb 12, however, the observed regions show a structure of clustered dark clouds whose physical parameters suggest that these clumps would be further fragmented or collapesed. Also found with the high resolution observations is that a few isolated clumps are located away from the main CO feature extended possibly from the galactic plane. For more detail morphologies and velocity structures of the clumps, especially in relation to the large CO complex to which these are likely to be associated, more observations are substantiated.

• 천문학논총
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• 제7권1호
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• pp.155-166
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• 1992

We observed a total of 14 Mira variables as well as 4 late type variable stars for their SiO ${\nu}= 1$, J = 2 - 1 maser lines from April 1989 to November 1990 with the 13.7 m radio telescope at Daeduk Radio Astronomy Observatory. The maser intensity variations were the prime objective of the observations which well covered the periods of the variations. The origion of the variations were studied by comparing wi th those previousely measured in optical and infrared(IR) wavelengths and we confirmed that the intensity variations were in good correlation with those in V magnitude and IR intensity as previousely found in former investigators in general. However, for a few sources, we could find the missing maxima. The intensities themselves also were in good correlation with SiO ${\nu}\;=\;1$, J = 1 - 0 maser intensities observed in Yebes as expected. The good correlations indicate that the pumping source of the SiO maser is likely to be the IR emission in the masing regions and the "missing maxima" that are apparent in two particular sources are considered to relate wi th the strength of shocks arising from the eruptive mass-loss from central stars.

• 천문학회지
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• 제26권1호
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• pp.65-72
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• 1993

Using the Daeduk Radio Telescope, we have observed $J=1\rightarrow0$ transitions of 1$^{12}CO,\;^{13}CO\;and\;C^{18}O$ toward OMC-l. The column densities of $1\~5\times10^{17}\;cm^{-2}\;and\;1\~3\times10^{16}\;cm^{-2}$ have been derived, for $^{13}CO$ and $C^{18}O$, respectively, in the $11'\times11'$ region centered at Orion - KL. The double isotope ratio $[^{13}CO]/[C^{18}O]$ was found to be larger than the cosmic abundance ratio by factors of $2\~10$ which may result from the chemical fractionation effect.

• 천문학회지
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• 제4권1호
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• pp.9-16
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• 1971

The asymmetry of received intensity pattern within the bandwidth is derived from the analogy of the intensity distribution of two-slit interference. This suggests that the length of $\frac{1}{2}{\lambda}$ delay line should be adjusted to the slightly upper frequency than the central frequency of the radio telescope with a wide bandwith. Some strange communication signals and man-made noises prevented us from obtaining the discernible information from the observed data for the sun. To overcome this difficulties, it is necessary to alter the operating frequency and site. It will be fo1lowed to measure the angular dimensions of the superposed radio sources by changing the distance between two antennas.