• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.43.2-43.2
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• 2010

Following the success of detecting fringes on KVN (Korean VLBI Network), a phase referencing observation is currently planned in order to achieve a better sensitivity in mm-VLBI. The high frequency observation ($\geq$ 22 GHz), wide bandwidths (~512 MHz) and high speed data recording (~1 Gbps, Mark5B) will result in resolution and sensitivity improvement on KVN. In particular, two powerful techniques of VLBI phase correction by fast-antenna switching and multi-frequency phase referencing are also introduced in KVN, hoping to resolve the problem of atmospheric delay errors which degrade the coherence significantly. In this study, we have compared the expected performance of phase referencing between fast antenna switching and multi-frequency phase referencing and discussed the essential condition and postulates of phase referencing for KVN.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.216.2-216.2
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• 2012

22/43/86/129GHz로 구성되는 KVN 4채널 수신기시스템의 제어 및 모니터링에 있어 데이터의 신속 정확한 전송 및 효율적인 시스템 관리는 매우 중요하다. 수신기 등의 프런트 엔드 시스템을 통해 입력되는 천체신호를 실시간 처리하기 위해서는 그를 구성하는 각 디바이스에 대한 제어 및 모니터링 구현은 물론 아날로그/디지털/시리얼 인터페스 간 적절한 조합이 구현되어야 한다. 이러한 사항을 고려하여 KVN은 프로피버스를 KVN수신기의 제어 및 모니터링을 위한 기반 인터페이스로 선택하였다. 프로피버스의 이점으로는 여러가지가 있으나 그 중 물리적으로 분산되어 있는 여러 시스템에 대한 제어 및 모니터링을 효과적으로 구현할 수 있다는 점을 가장 큰 장점으로 들 수 있다. 우리의 경우 KVN 수신기의 제어 인터페이스 구성에 있어 이러한 장점을 십분 활용하였다. 본 포스터에서는 프로피버스의 개요 및 특성에 대한 소개를 기반으로 분산 환경의 시스템 항목을 제어 및 모니터링하기 위한 방안에 대해 논의할 것이다. 나아가 이를 기반으로 구현된 KVN수신기의 제어 인터페이스 현황에 대해 살펴보고자 한다.

• Journal of the Institute of Convergence Signal Processing
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• v.17 no.2
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• pp.83-92
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• 2016

In this paper, we introduce the results of the testing and observation systems for performance wideband expansion in the Korean VLBI Network(KVN). The KVN performs VLBI observations to 1024 Mbps data rate, and 8192 Mbps observing for four simultaneous observation is now evaluating for normal operation. The VLBI stations in several world countries developed their own wideband observing systems to observe the celestial objects with high precision and high resolution or are working with several countries. The KVN is planning to introduce a high-speed sampler, OCTAD, for sampling directly up to 2048 MHz bandwidth for RF signal of K/Q/W/D band in the frequency band without conversion. Therefore, as a preliminary study for the performance scalability of the KVN then through the close cooperation with National Astronomical Observatory of Japan (NAOJ), the OCTAD high-speed sampler and OCTADISK2 high-speed recorder were installed in the KVN Yonsei station, and verify the performance through a wideband.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.133.2-133.2
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• 2011

KVN phase Calibrator Survey(KVNCS)는 VLBI 관측 시 대기의 불규칙한 수증기 분포로 인한 visibility 위상의 불규칙한 변화를 보정하기 위해 도입되는 phase-referencing 기법 등에서 필수요소인 위상보정 calibrator를 얻기 위한 연구이다. Phase-referencing 기법을 이용하여 위상을 보정하기 위해서는 대상 천체의 근접한 곳에 비교적 compact한 calibrator가 존재해야 한다. 또한 Asaki et al.(1996)에 의하면 대기의 coherence structure가 유지되기 위해서는 두 천체가 적어도 $5^{\circ}$ 이내의 분리각을 가져야 한다. 위상보정 calibrator에 대한 연구는 주로 2, 8GHz 대역에서 진행되어 왔고 최근에는 22GHz에서 VLBI 관측이 진행되고 있지만 천구상의 특정 영역에 국한되거나 calibrator들 간의 분리각이 여전히 크다. KVNCS는 천구상에서 calibrator의 분포를 좀 더 고르게 하고 더 많은 calibrator를 얻어 적어도 $5^{\circ}$ 이내의 분리각을 구현하고자 한다. 먼저, 단일경을 이용하여 KVNCS의 대상을 확보하기위하여 이들의 플럭스를 정확히 측정하였다. 2, 8GHz 대역에서 관측된 VLBA(Very Long Baseline Array) Calibrator Survey(VCS) 목록을 기초로 power-law를 가정하여 22GHz에서 100mJy 이상일 것으로 예상되는 천체 2503개를 KVNCS 단일경 연구의 후보로 선정하였다. KVN 연세와 울산 전파망원경경을 이용하여 2009년 12월부터 2011년 3월까지 2298개의 플럭스 측정 관측을 진행하여 22GHz에서 약 77%, 43GHz에서 약 23%의 검출률을 얻었다. 또한 이 천체들의 공간분포도 $5^{\circ}$의 분리각을 만족하는 것을 확인하였다. 앞으로 KVNCS 단일경 결과를 활용하여 KVN 각 사이트의 위치 정보를 비롯하여 22GHz KVN VLBI 관측을 통해 KVN 위상보정 calibrator를 확보 할 계획이다.

• Publications of The Korean Astronomical Society
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• v.25 no.1
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• pp.15-21
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• 2010

We report results of image simulations of the KVN and VLBI experiments of the KVN with several other East Asia VLBI facilities. To investigate their imaging capability a model-generated image of 7 mm SiO maser emission in Mira variables is used. The resulting simulations show that the joint VLBI experiments of the KVN with East Asia VLBI facilities can produce reasonably good images at 7 mm spectral line experiments. However, there are no apparent differences in peak flux densities and images themselves in the simulations among different combinations of these facilities. In addition, the simulated images of observations which include bigger antennas do not show any expected improvement to the image sensitivity. The small variations in the peak flux density and similar image sensitivity, irrespective of different antenna sizes or numbers of baselines used in the simulations, turn out due to a specific characteristic of the adopted model image. Test simulations using another SiO maser image from R Cas observations prove that the participation of bigger antennas in the VLBI experiments does improve image sensitivity. We confirm the need of additional longer baselines in the experiments of the East Asia VLBI facilities to study very compact maser clumps on sub-milliarcsecond scales.

• Journal of The Korean Astronomical Society
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• v.49 no.4
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• pp.137-144
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• 2016

The calibration of Very Long Baseline Interferometry (VLBI) data has long been a time consuming process. The Korean VLBI Network (KVN) is a simple array consisting of three identical antennas. Because four frequencies are observed simultaneously, phase solutions can be transferred from lower frequencies to higher frequencies in order to improve phase coherence and hence sensitivity at higher frequencies. Due to the homogeneous nature of the array, the KVN is also well suited for automatic calibration. In this paper we describe the automatic calibration of single-polarisation KVN data using the KVN Pipeline and comparing the results against VLBI data that has been manually reduced. We find that the pipelined data using phase transfer produces better results than a manually reduced dataset not using the phase transfer. Additionally we compared the pipeline results with a manually reduced phase-transferred dataset and found the results to be identical.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.43.1-43.1
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• 2010

We have carried out 43-GHz VLBI test observations of the Korean VLBI Network (KVN), which has obtained the first fringes at 22/43-GHz in 2009 (a talk by Sohn, Bong Won). In collaboration with VERA (VLBI Exploration of Radio Astrometry) in Japan, we have observed Active Galactic Nuclei (AGNs) and Orion-KL at 43GHz on 22nd and 23rd December, 2009, in order to evaluate the baseline- and image-sensitivity of KVN and KVN+VERA. In this talk we report the preliminary results of the VLBI test observations of the Korean VLBI Network at 43GHz.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.238.1-238.1
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• 2012

We present the results of simultaneous observations of SiO v=1 and 2, J=1-0 maser lines which were carried out with the combined network of the KVN and VERA in 2012 April. The observations were performed toward a long period OH/IR star, WX Psc in order to test the technical and scientific feasibilities of the KVN+VERA combination. The resultant (u, v) coverage of the KVN+VERA combined array enhances the image quality. We confirmed that the distribution and intensity of individual maser spots using the combined network are more reliable compared with the images using the KVN or VERA only. This observation also provides a chance to find a high sensitivity and imaging quality which are comparable to those of VLBA. In addition, the simultaneous observations of two SiO v=1 and 2, J=1-0 maser lines enable us to trace the detail physical environments close to the central star due to different high excitation conditions between two lines at a time.

• The Bulletin of The Korean Astronomical Society
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• v.44 no.1
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• pp.76.1-76.1
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• 2019

CTA 102, one of gamma-ray bright active galactic nuclei (AGN) has been observed with Korean very long baseline interferometry (VLBI) network (KVN) during the period of 2012 December-2018 May as part of interferometric Monitoring Of Gamma-ray Bright AGN (iMOGABA). Multi-frequency VLBI observations enable us to compare the milliarcsecond(mas)-scale iMOGABA images of relativistic jets with those from the Monitoring Of Jets in AGN with Very long baseline array (VLBA) Experiments (MOJAVE) and the VLBA-Boston University(BU)-BLAZAR programs which use VLBA with its angular resolutions of 0.2-1.3 mas. In spite of the relative larger beam sizes of KVN (1-10 mas), we are able to identify jet components of CTA 102 using the KVN multi-frequency VLBI observations with those resolved with VLBA. Considering an instrumental beam blending effect on the jet component identification, we were able to obtain a blending shift of the core position based on a convolution analysis using the VLBA data. When we apply the core position shift to the KVN images of CTA 102, we find that the identified jet components of CTA 102 from the KVN observations are well matched with those from the VLBA observations. Based on the results of the analysis, we may be able to study the jet kinematics and its correlation with gamma-ray flare activity.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.127.2-127.2
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• 2011

KVN 21미터 전파 망원경의 수신시스템은 동시에 좌우 원형편파를 수신할 수 있다. 또한 단일경 전파 분광 관측에 사용되고 있는 전파분광기는 자기상관자료와 함께 교차상관자료도 동시에 처리할 수 있다. 이 전파분광기의 교차상관자료 처리 기능을 이용하여 편광관측을 할 수 있도록 관측 소프트웨어를 개선하였으며 현재 연속파 편광관측을 진행 중이다. 본 발표는 KVN 21미터 망원경을 이용한 단일경 편광 관측에 대해 소개하고 편광 관측 성능 측정 결과를 소개한다.