• 전자공학회논문지D
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• 제36D2호
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• pp.20-30
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• 1999

85-115GHz 주파수 범위의 100GHz 대역과 125-175GHz 주파수 범위를 갖는 150GHz 대역을 동시에 관측하기 위한 헤테로다인 방식의 이중채널 수신기에 사용될 단측파대 여파기의 이론을 제시하고 이를 근거로 설계, 제작한 후 성능을 측정하였다. 여파기의 이론은 편파 회전 특성을 갖는 Martin-Puplett 간섭계의 원리를 도입하여 전개하였다. 설계와 제작은 빔의 전송손실을 최소화하고 중간주파수와 관련된 경로차를 고려하여 두 빔의 결합 손실을 최소화하는데 주안점을 두었다. 두 주파수 대역을 동시에 관측하기 위해서는 우주전파가 각각 다른 빔의 경로로 전송되어야 하므로 두 개의 단측파대 여파기가 각각 제작되었다. 주파수에 따른 여파기의 이론적인 최적 경로차와 중간주파수 및 대역폭을 계산하였다. 네트웍 분석기와 자체에서 제작한 빔 측정장치를 이용하여 여파기의 성능을 측정하고 이론치와 비교하였다. 주파수에 따른 최적 경로차에 대한 이론치와 측정치를 비교해 본 결과 거의 일치하는 특성을 보여 제시된 설계 이론의 타당성과 정밀한 제작이 검증되었고, 두 대역 여파기의 이미지 제거비는 약 22dB이상을 갖는 우수한 성능을 보였다. 제작된 여파기는 이중채널 수신기에 설치되어 우주전파를 성공적으로 관측함으로서 그 성능이 입증되었다.

• 대한전기학회:학술대회논문집
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• 대한전기학회 2005년도 학술대회 논문집 정보 및 제어부문
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• pp.116-119
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• 2005

In this paper, we propose the PLL system of the local oscillator system for the millimeter wave band's radio astronomy receiving system. The development of the proposed local oscillator system based on the YIG oscillator VCO with 26.5 ${\sim}$ 40GHz specification. This system consists of the oscillator part including the YIG VCO, the harmonic mixer, and the isolator, the RF processing part including the triplexer, limiter, and RF discrimination processor. and the PLL system including YIG modulator and controller. Based on this configuration. we verify the frequency and power stability of the developed local oscillator system according to some temperature variation. From this test results we confirm the stable output frequency and power characteristic performance of the developed La system at constant temperature.

• 전자공학회논문지D
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• 제36D권8호
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• pp.7-18
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• 1999

100GHz와 150GHz 대역의 우주전파를 동시에 관측하기 위한 준광학계가 설계, 제작되었다. 밀리미터파 및 서브밀리미터파 대역의 전송수단으로 널리 이용되고 있는 준광학계는 가우시안 빔으로 해석된다. 따라서 가우시안 빔 이론을 이용하여, 광대역 주파수 범위에서 주로 사용되는 영상 빔 방법으로 준광학계를 해설한다. 이중채널 준광학계는 두 대역의 전파를 동시에 관측하기 위해서, 두 개의 빔을 유도하는 시스템이다. 따라서 두 빔을 유도하기 위한 준광학계와 준광학계를 구성하는 각 부품은 영상 빔 방법을 이용하여 설계하였다. 이러한 설계를 바탕으로 준광학계의 각 소자들이 제작되었고, 전체 시스템이 구현되었다. 제작된 준광학계는 자체에서 제작한 빔 측정장치를 이용하여 측정함으로써, 설계에 대한 검증과 정확한 제작여부를 확인하였다. 그리고 제작된 시스템은 이중채널 수신기에 설치되어, 우주전파를 동시에 성공적으로 관측함으로써 그 성능이 입증되었다.

• 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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• 제28권3호
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• pp.95-100
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• 2013

A fiber-optic reference signal transmission system, which transmits the 1.4 GHz reference signal from H-maser to receiver cabin in radio telescopes, was adopted for compensating the phase changes due to temperature variation and antenna movement. At the first experiment, the remote signal's phase changed more than 15 degrees at 1.4 GHz. We found unstable components in sub-system experiments and replaced them. The main cause of unstable phase stability was the unaligned polarization axis between Laser Diode and Mach-Zehnder Modulator (MZM). The improved system stability showed $1{\times}10^{-16}$ allan standard deviation at 1,000 sec integration time with the antenna fixed. When the antenna moves in the azimuth axis, the 1.4 GHz remote signal showed the phase change smaller than 0.2 degrees.

• 천문학논총
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• 제20권1호
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• pp.125-134
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• 2005

In this paper, we propose a small-scale Gigabit VLBI observing system for the Korean VLBI Network (KVN) under construction. The system consists of high-speed sampler, IP-VLBI board, PC-VSI board, and software correlator. Radio signal received by receiver is sampled by high-speed sample. at 1 Gsps (Gigabit sample per second) rate with 2 bits quantization. The digitized signal is recorded in PC and the software correlator does the cross correlation. IP-VLBI board will be used for the geodesy VLBI observation, while PC-VSI board is for the astronomical VLBI observation. The PC-VSI board adopts the VSI-H (VLBI Standard Interface Hardware). The proposed system is based on commercial PCs and therefore can be built inexpensively.

• Journal of Astronomy and Space Sciences
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• 제40권4호
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• pp.237-245
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• 2023

Laser communication has been considered as a novel method for earth observation satellites with generation of high data volume. It offers faster data transmission speeds compared to conventional radio frequency (RF) communication due to the short wavelength and narrow beam divergence. However, laser beams are refracted due to atmospheric turbulence between the ground and the satellite. Refracted laser beams, upon reaching the receiver, result in angle-of-arrival (AoA) fluctuation, inducing image dancing and wavefront distortion. These phenomena hinder signal acquisition and lead to signal loss in the course of laser communication. So, precise alignment between the transmitter and receiver is essential to guarantee effective and reliable laser communication, which is achieved by pointing, acquisition, and tracking (PAT) system. In this study, we simulate the effectiveness of tip/tilt compensation for more efficient laser communication in the satellite-ground downlink. By compensating for low-order terms using tip/tilt mirror, we verify the alleviation of AoA fluctuations under both weak and strong atmospheric turbulence conditions. And the performance of tip/tilt correction is analyzed in terms of the AoA fluctuation and collected power on the detector.

• Journal of Astronomy and Space Sciences
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• 제30권4호
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• pp.345-353
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• 2013

A W-band Orthomode Transducer (OMT) has been developed for Korean VLBI Network (KVN) polarization observation. The OMT design was based on E-plane split-block technique using septum structure. 3-dimensional electromagnetic simulation was fully employed to optimize the performance of the OMT. Measurements of the fabricated OMT show that the return losses for the vertically and horizontally polarized modes are better than -20 dB across 80 ~ 108 GHz and the insertion losses for the both modes are less than 0.47 dB. The cross-polarization level of the OMT is less than -30 dB. The bandwidth of the developed OMT is estimated as around 30%.

• 천문학논총
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• 제15권spc2호
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• pp.21-25
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• 2000

The ionosphere, the atmosphere of the earth ionized by solar radiations, has been strongly varied with solar activity. The ionosphere varies with the solar cycle, the seasons, the latitudes and during any given day. Radio wave propagation through or in the ionosphere is affected by ionospheric condition so that one needs to consider its effects on operating communication systems normally. For examples, sporadic E may form at any time. It occurs at altitudes between 90 to 140 km (in the E region), and may be spread over a large area or be confined to a small region. Sometimes the sporadic E layer works as a mirror so that the communication signal does not reach the receiver. And radiation from the Sun during large solar flares causes increased ionization in the D region which results in greater absorption of HF radio waves. This phenomenon is called short wave fade-outs. If the flare is large enough, the whole of the HF spectrum can be rendered unusable for a period of time. Due to events on the Sun, sometimes the Earth's magnetic field becomes disturbed. The geomagnetic field and the ionosphere are linked in complex ways and a disturbance in the geomagnetic field can often cause a disturbance in the F region of the ionosphere. An enhancement will not usually concern the HF communicator, but the depression may cause frequencies normally used for communication to be too high with the result that the wave penetrates the ionosphere. Ionospheric storms can occur throughout the solar cycle and are related to coronal mass ejections (CMEs) and coronal holes on the Sun. Except the above mentioned phenomena, there are a lot of things to affect the radio communication. Nowadays, radio technique for probing the terrestrial ionosphere has a tendency to use satellite system such as GPS. To get more accurate information about the variation of the ionospheric electron density, a TEC measurement system is necessary so RRL will operate the system in the near future.

• 천문학회지
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• 제39권2호
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• pp.51-56
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• 2006

We report the development of a semi-VLBI observation system operating at 21 cm and present the measurement of visibility function toward the sun using this system. The system consists of two 2.3 meter antennas with a maximum separation of 35 meter, a conventional high speed data acquisition system, and a set of programs for software correlation. Since two local oscillators of receiver modules are independent, data had to be fringe-fitted to yield the visibility amplitude. It is found that the visibility amplitude decreases and then bounces back as baseline increases. We confirm that solar disk with brighter limb best explains the measured visibility amplitude.