• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.71.2-71.2
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• 2011

한국천문연구원은 한일상관센터(Korea-Japan Correlation Center)에 2009년부터 한일공동 VLBI상관기(Korea-Japan Joint VLBI Correlator, KJJVC)를 설치하여 운영하고 있다. 한일공동VLBI상관기는 한국우주전파관측망(Korean VLBI Network, KVN), VERA(VLBI Exploration of Radio Astrometry), JVN(Japanese VLBI Network)을 연결하여 관측을 수행하고 동아시아 지역의 VLBI 관측망의 상관처리를 담당할 예정이다. 한일공동VLBI상관기 중에서 데이터동기재생처리장치(Raw VLBI Data Buffer, RVDB)와 관측데이터를 재생할 수 있는 재생기 시스템(Mark5B)간의 데이터 전송은 1Gbps 전송속도를 가지는 VSI(VLBI Standard Interface)규격의 전송케이블을 통하여 수행된다. 고속 데이터 전송에 있어 발생하는 전자기방해(Electromagnetic Interference, EMI)는 관측 데이터의 손실을 발생시키며, 이러한 고속데이터 전송간에 발생하는 EMI는 케이블의 길이가 길어질수록 많이 발생하게 되며 향후 상관기 시스템의 확장을 고려할 때 상당한 문제점을 초래 할 수 있다. 따라서, VSI규격의 통신에서 발생하는 EMI 노이즈 정도를 측정하고, 노이즈 제거 필터를 적용하여 데이터 손실을 최소화 할 수 있는 방안을 고려하였다. 본 발표에서는 한일공동VLBI상관기(KJJVC)에서 운용되는 고속재생기(Mark5B)와 RVDB간의 VSI방식의 데이터 전송에 있어 야기되는 EMI를 제거하고 관측 데이터의 손실을 최소화할 수 있는 방안을 제안한다.

• Journal of The Korean Astronomical Society
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• v.56 no.2
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• pp.159-168
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• 2023

The main goal of the Korean VLBI Network Calibrator Survey (KVNCS) is to expand the VLBI calibrators catalog for KVN, KaVA (KVN and VERA Array), EAVN (East-Asian VLBI Network), and other extended regions. The second KVNCS (KVNCS2) aimed to detect VLBI fringes of new candidates for calibrators in the K band. Out of the 1533 sources whose single-dish flux density in the K band was measured with KVN telescopes (Lee et al. 2017), 556 sources were observed with KVN in the K band. KVNCS2 confirmed the detection of VLBI fringes of 424 calibrator candidates over a single baseline. All detected sources had a high Signal-to-Noise Ratio (SNR) of >25. Finally, KVNCS2 confirmed 347 new candidates as VLBI calibrators in the K band, resulting in a 5% increase in the sky coverage compared to previous studies. The spatial distribution was quasi-uniform across the observable region (Dec. > -32.5°). In addition, the possibility as calibrator candidates for the detected sources was checked, using an analysis of the flux-flux relationship. Ultimately, the KVNCS catalog will not only become the VLBI calibrator list but is also useful as a database of compact radio sources for astronomical studies.

• The Journal of the Korea institute of electronic communication sciences
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• v.15 no.6
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• pp.1159-1168
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• 2020

In the past, control and monitor of a large number of instruments is a specialized area, which requires an expensive dedicated module to implement. However, with the recent development of embedded technology, various products capable of performing M&C (Monitor and Control) have been released, and the scope of application is expanding. Accordingly, it is possible to more easily build a small M&C environment than before. In this paper, we discussed a method to replace the M&C of the VLBI system, which had to be implemented through a specialized hardware product, with an inexpensive general imbeded technology. Memory based data transmission, reception and storage is a technology that is already generalized not only in VLBI but also in the network field, and more effective M&C can be implemented when some items of Ethernet are optimized for the VLBI (Very Long Baseline Interferometer) system environment. In this paper, we discuss in depth the design and implementation for the multidrop based IoT architecture.

• Publications of The Korean Astronomical Society
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• v.23 no.2
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• pp.37-45
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• 2008

We present the results of image simulations of 43.1 GHz SiO maser emission toward a Mira variable using the KVN (Korean VLBI Network) and other facilities which can make joint VLBI experiments with the KVN. To test the imaging capability of the KVN we used the image of SiO masers in the simulation obtained by the VLBA, which is considered to be the optimum VLBI facility at present to study SiO masers toward evolved stars. The simulated images of SiO maser emission confirm that coordinate VLBI expriments of KVN with several more stations in Japan or in the neighborhood of Korean Peninsula are necessary to exert the functional benefit of the KVN as the first mm VLBI facility which can perform simultaneous observations at four different frequency bands.

• Journal of The Korean Astronomical Society
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• v.38 no.2
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• pp.97-100
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• 2005

The first Space-VLBI project, VSOP, started successfully with the launch of the dedicated space-VLBI satellite HALCA in 1997. The project has been in scientific operation in the 1.6 GHz and 5 GHz bands, and studies have been done mainly of the jet phenomena related to active galactic nuclei. A second generation space- VLBI project, VSOP-2, has been planned by the working group formed at ISAS/JAXA with many collaborators. The spacecraft is planned to observe in the 8, 22 and 43 GHz bands with cooled receivers for the two higher bands, and with a maximum angular resolution at 43 GHz (7 mm) of about 40 micro-arcseconds. The VSOP-2 satellite will also have the capability of the phase-reference and full polarization observations, which will produce more powerful results than those of the VSOP project. Far-future space-VLBI projects following VSOP and VSOP-2, have a large potential to achieve enough resolution and sensitivity to satisfy astronomers in future.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.42.2-42.2
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• 2010

2009년부터 2010년에 걸쳐 22 및 43GHz 대역에서의 KVN 단일경 시험관측이 이루어졌다. KVN 관측소는 연세대학교, 울산대학교, 탐라대학교에 위치하고 있으며, 시험관측의 주된 내용은 안테나 지향모델 구축, 22/43 GHz 빔 정렬, 이득곡선 측정 및 안테나 효율측정 등이다. 구축된 지향오차의 정밀도는 세 곳의 관측소 모두 rms가 5초 이내였으며, 두 빔도 5초 이내로 정렬되어 있음이 확인되었다. 안테나 효율은 22 및 43GHz에서 모두 60%를 넘는 값을 얻을 수 있었다.

• The Bulletin of The Korean Astronomical Society
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• v.44 no.2
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• pp.50.4-50.4
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• 2019

2001년부터 총 230억원의 건설 예산을 투입한 한국우주전파관측망(KVN) 건설 프로젝트는 2008년 KVN을 구성하는 3개의 전파 망원경 건설을 마무리 하였고, 2009년 22GHz와 43GHz에서 세 기선의 프린지 검출에 성공하였다. 국내 최초 VLBI 관측망인 KVN은 2009년 프린지 검출로 VLBI의 첫 걸음을 시작한 이 후 올해로 VLBI 관측 역사의 10년에 이르렀다. 2009년부터 첫 4년간의 시험 관측을 거쳐 2013년 세계 최초로 22,43,86,129GHz 4개 주파수 동시 관측을 지원하는 본격적인 VLBI 관측 운영을 시작하였다. 지난 10년간의 KVN을 활용한 연구 성과를 통해 KVN 방식의 동시 다주파수 관측 시스템은 전 세계적으로 mm-VLBI의 국제 표준으로 인정받고 있다. 본 발표는 지난 10년간의 KVN의 운영 과정과 이를 통해 이룬 주요 연구 성과를 되돌아보고 앞으로의 전망에 대해 소개한다.

• The Journal of the Korea institute of electronic communication sciences
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• v.14 no.6
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• pp.1109-1120
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• 2019

In the field of VLBI, If the quality of the connected network between the VLBI station and the correlation center is ensured, the existing inefficiency of repeatedly storing the observation data in each station and the correlation center can be overcome. In other words, the data center can be unified with the correlation center where data analysis is performed, which can improve data processing speed and productivity. In this paper, we design a massive VLBI data system that directly transmits and stores the observation data stream obtained from the VLBI station to the correlation center via the high - speed network KREONET. Based on this system, VLBI test observations confirmed that the observation data was stored perfectly in the recording system of the correlation center without a single packet loss.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.241-241
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• 2012

MOGABA is a project monitoring of gamma-ray bright AGN(Active Galactic Nuclei). Since May 2011, we have observed total flux, degree of linear polarization, and polarization angle of about twenty AGN once a week at 22, 43 and 86GHz using KVN(Korean VLBI Network) 21m radio telescopes. We have observed variation of total flux of BLLAC and OJ287 from May 2011 to March 2012. We have observed flares of total flux at 22GHz for those sources from October 2011 to November 2011. In this paper we report the variation of total flux, degree of linear polarization and polarization angle at 22, 43, 86GHz for BLLAC and OJ287.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.239.2-239.2
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• 2012

We report preliminary results of MOGABA project for monitoring total flux density, linearly polarized flux, and polarization angle at 22, 43 and 86GHz of Gamma-ray bright AGN (Active Galactic Nuclei) with KVN (Korean VLBI Network) 21-m radio telescopes. The project has been conducted in one year since May 2011 with an effective monitoring cycle of 1 week, observing four main objects (3C 454.3, BL Lac, 3C 273, and 3C 279). More objects were included in the source list when they had flared in Gamma-ray. Especially, we included a compact radio source at the Galactic center, SgrA* since Jan. 2012. In this paper, we report the current status of the project and preliminary results for the monitoring observations.