• Journal of Astronomy and Space Sciences
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• v.23 no.4
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• pp.337-344
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• 2006

KVN simulation, which is focused on evaluating the impacts of KVN to geodetic VLBI network, was performed. The KVN is under construction with three radio telescopes VLBI system for radio astronomy and space geodesy. To distinguish the impacts of KVN on global and local scale networks, we designed two different sizes of VLBI networks, namely, KVN-Asia and KVN-Pacific. While the former consisted of Far East Asia region VLBI stations, the latter consisted of pacific region VLBT stations. The primary purpose of our simulation is quantitative evaluation of KVN impacts before and after the participation of KVN in the previous two virtual networks. We selected two different sets of parameters to be estimated in the simulation as indices of evaluating estimation precision: station coordinates and EOPs. The station coordinates are evaluating index for KVN-Asia and the EOPs are another evaluating index for KVN-Pacific. From the simulation results of comparisons between evaluating indexes, 50% and 20% of maximum improvements for KVN-Asia and KVN-Pacific were anticipated respectively. We expect that the space geodetic use of KVN will be focused on the several promising research fields which are proposed through the simulation results.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.42.1-42.1
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• 2010

한국천문연구원 한국우주전파관측망(KVN)은 2008년 KVN연세-VERA 간의 프린지 검출에 이어, 2009년 10월 KVN 모든 기선 간의 22GHz와 43GHz 프린지 검출에 성공하였다. 본 발표에서는 KVN 프린지 검출 시험의 과정과 결과를 요약하고, 또한 현재 수행 중인 KVN의 두 주파수 동시 VLBI 시험관측의 진행과정을 보고 하고자 한다.

• The Journal of the Korea institute of electronic communication sciences
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• v.14 no.6
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• pp.1097-1108
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• 2019

In VLBI(Very Long Baseline Interferometry), the observed data created in many observatories which are far away from each other should be collected in correlation center for data analysis. Traditionally, observed data is moved by transportation such as car or airplane. But it is replaced with data transfer over the network rapidly as the advancement of information technology, and therefore, international cooperative research is also now more widely expanding. e-KVN(electronic Korean VLBI Network) has been upgraded two times so the network interface of KVN has been evolved to the highest specification of 100GbE. During this time period, the portion of network usage for VLBI observations and experiments in KVN has been increased exponentially. In this paper, we describe KVN VLBI system and network technology for the performance upgrade and advanced status monitoring between three radio astronomy observatories and Daejeon correlation center with KREONET(Korea Research Environment Open NETwork). Furthermore, future plan of e-KVN for the implementation of wide band VLBI observation will be also briefly discussed.

• 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.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.115-115
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• 2014

First, We will briefly introduce early science results of AGN observations with KVN and KaVA. KaVA is the combined array of the Korean VLBI network (KVN) and VLBI Exploration of Radio Astronomy (VERA). These include KaVA monitoring of M87, Sgr A* and a few bright blazars and KVN Search for circular polarized Blazars. Furthermore, we will present our future plan of monitoring observation of Sgr A* and M87 with KaVA and Low Radio Power AGN multi frequency polarization survey with KVN. Because of the largeness of their centralsuper-massive black holes, we select them as top-priority sources of our key science program (KSP). The main science goals of the KaVA KSP are (1) mapping the velocity field of the M87 jet and testing magnetically-driven-jet paradigm, and (2) obtaining tightest constraints on physical properties of radio emitting region in Sgr A. High sensitivity achieved through simultaneous multifrequency phase referencing technique of KVN will allow us to explore Low Radio Power AGN cores which build majority of AGNs and therefore are important for undestanding the evolution of AGNs and of their hosts.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.112.1-112.1
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• 2014

KVN은 현재 연간 3000시간 이상의 VLBI 관측 시간을 운영하는 안정적인 운영단계에 들어섰다. 또한 일본의 VLBI 관측망인 VERA와 연결한 KaVA (KVN and VERA Array)도 한일상관센터의 운영시작과 더불어 연간 1000 시간의 관측 운영을 하고 있으며 KaVA를 이용한 연구 성과가 나오기 시작하였다. KVN은 다파장 Astrometry를 위해 다파장 P-Cal 시스템을 개발하고 있으며 관측 감도를 높이기 위해 8Gbps 운영을 준비하고 있다. KVN의 운영 및 시스템 개선 계획, 국제 협력 내용 등을 소개한다.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.58.2-58.2
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• 2010

한국우주전파관측망(KVN : Korean VLBI Network)) 시스템이 구축되어 시험관측 중에 있다. 그 동안 KVN 시스템의 성능 측정 시험과 조정을 통해 시스템을 업그레이드 하고, 안테나, 수신기, 컴퓨터 주변장치의 안정화를 위한 노력이 행해졌다. 시스템 안정화 및 시험관측을 통해 단일 망원경 관측이 수행되었고 본격적인 VLBI 관측을 위한 준비가 진행되고 있다. 지난 1년간 KVN 지역전파천문대인 울산, 탐라전파천문대의 운영에 대해 논의한다. KVN울산_탐라 지역전파천문대 운영과 기반 구축을 위한 노력, 주요업무 현황, 시스템 유지 보수 및 관측소 운영, 지역천문대 현안에 대해 돌이켜보고, 앞으로 효율적인 운영에 대해 논의한다.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.2
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• pp.57.2-57.2
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• 2017

KVN is a millimeter VLBI array composed of three 21m-diameter radio telescopes at Seoul, Ulsan and Jeju island in Korea. KVN has unique simultaneous multi-frequency receiving systems, which enable us to correct phase fluctuation of troposphere by transferring phase solution of low frequency data to higher frequency data. Although KVN can achieve very high performance up to 130 GHz through multi-frequency technique, imaging capability is highly limited because of lack of the number of baselines. In order to enhance imaging capability and maximizing multi-frequency capability, we plan to extend KVN baselines from 3 to 10 (or more) by constructing new KVN stations. This talk introduce expected performances, science cases, required budgets and periods of the Extended-KVN.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.2
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• pp.88.2-88.2
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• 2017

한국우주전파관측망(KVN: Korean VLBI Network)은 서울, 울산, 제주에 직경 21m 전파망원경 3기로 이루어진 우리나라 최초의 초장기선 전파간섭계(VLBI: Very Long Baseline Interferometry)이다. KVN은 밀리미터 파장의 22, 43, 86, 129 GHz 대역을 동시에 관측할 수 있는 수신시스템을 이용하여 독보적인 다파장 관측연구를 진행해오고 있으며, 뛰어난 위상보정 성능을 바탕으로 기존의 밀리미터 대역에서 검출되지 않았던 많은 천체들을 검출하고 있다. 하지만, KVN 3기 VLBI 관측으로부터 얻어지는 천체의 합성영상(synthesized image)은 초미세구조에서 발생하는 물리 기작을 연구하기에는 큰 한계를 지닌다. KVN을 활용한 연구 성과를 극대화하기 위한 최적의 방안을 도출하기 위하여, KVN 확장 기획연구를 진행하고 있다. 본 연구는 KVN 확장시 예상되는 성능을 분석하고, 영상 성능을 극대화하기 위한 최적의 사이트 조건을 알아본다.

• The Bulletin of The Korean Astronomical Society
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• v.40 no.1
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• pp.54.1-54.1
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• 2015

We report results of investigation of amplitude calibration for very long baseline interferometry (VLBI) observations with Korean VLBI Network (KVN). Amplitude correction factors are estimated based on comparison of KVN observations at 22 GHz correlated by Daejeon hardware correlator and DiFX software correlator in Korea Astronomy and Space Science Institue (KASI) with Very Long Baseline Array (VLBA) observations at 22 GHz by DiFX software correlator in National Radio Astronomy Observatory (NRAO). We used the observations for compact radio sources, 3C 454.3 and NRAO 512 which are almost unresolved for baselines in a range of 350-477 km. VLBA visibility data of the sources observed with similar baselines as KVN are selected, fringe-fitted, calibrated, and compared in their amplitudes. We found that visibility amplitudes of KVN observations should be corrected by factors of 1.14 and 1.40 when correlated by DiFX and Daejeon correlators, respectively. These correction factors are attributed to the combination of two steps of 2-bit quantization in KVN observing systems and characteristics of Daejeon correlator.