• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.68.1-68.1
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• 2018

KaVA(KVN and VERA Array)는 KVN 3기, 일본 VERA 4기로 구성되어 있다. 더 나아가 일본의 JVN, 중국의 CVN으로 확장한다면 동아시아에 더 많은 기선들이 존재한다. 각 전파망원경은 천문학자의 연구수요, 디지털 백엔드(Back-end) 시스템 기술수준에 의해 각기 다른 다양한 자료구조를 이용한다. 이와 함께, 현재 전파천문관측은 디지털 백엔드 시스템의 발달로 2Gbps 관측이 주를 이루고 있으며 32Gbps 시험 관측이 이루어지고 있다. 이에 한일상관센터는 이런 다양한 자료구조와 관측 대역폭을 지원하기 위해 KaVA용 디지털필터를 개발하고 있다. 기존에 개발된 CPU기반의 디지털필터를 연산속도와 자료 입출력 대역폭을 상당히 높인 GPU 기반 디지털필터로 업그레이드하고 있다. 본 발표는 GPU를 활용한 KaVA용 디지털 필터 개발에 관하여 소개하고자 한다.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.60.2-60.2
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• 2011

We introduce the preliminary results of flux monitoring of BL Lac object 0716+714 with the KVN Ulsan 21m radio telescope. This radio source is well known as the intraday variable (IDV) source which is characterized by the rapid flux variation on the time scale of a day or less. In general, the IDV phenomenon is interpreted as the effect of refractive scintillation in the interstellar medium or the evidence of intrinsic flux variation. In previous observations that took a few days, however, it had not been detected the flux variation of short time scale but the monotonic increase and decrease. Therefore, to investigate the longer time scale of 0716+714, we had the flux variation monitoring at 22GHz and 43GHz simultaneously for 9 months from October 2010 to June 2011. We present here the structure functions and the cross correlation functions between different frequencies as well as the light curves.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.1
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• pp.68.4-69
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• 2016

We report preliminary results of KaVA observations of central galaxies in cool-core and non cool-core clusters. The main goal is to study how cooling environments of galaxy clusters affect the central AGN activities especially at its innermost region. For KaVA observations, 7 radio bright AGNs have been selected from the extended Highest Flux Galaxy Cluster Sample (eHIFLUGCS; the X-ray flux limited & all sky galaxy cluster catalog) with various cooling timescales. In our previous KVN study, we have found that most AGNs in the cool-core clusters show the hint of pc-scale jet-like features while the ones in the non cool-core clusters do not. Using the KaVA 22/43 GHz data of a much higher resolution than the KVN resolution, we have investigated detailed pc-scale jet properties such as physical size, morphology, and radiative age. Based on the KaVA data, we discuss the effect of cluster cooling environment on the evolution of AGNs in the cluster center.

• Publications of The Korean Astronomical Society
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• v.21 no.2
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• pp.95-100
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• 2006

In this paper, we describe the radio astronomical data processing system implementation using Mark5B and its development. KASI(Korea Astronomy and Space Science Institute) is constructing the KVN (Korean VLBI Network) until the end of 2007, which is the first VLBI(Very Long Baseline Interferometery) facility in Korea and dedicated for the mm-wave VLBI observation. KVN will adopt the DAS (Data Acquisition System) consisting of digital filter with various function and 1Gsps high-speed sampler to digitize the radio astronomical data for analyzing on the digital filter system. And the analyzed data will be recorded to recorder up to 1Gbps data rates. To test this, we have implemented the system which is able to process 1Gbps data rates and carried out the data recording experiment.

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.637-639
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• 2015

The Korean very-long-baseline interferometry (VLBI) network (KVN) and VLBI Exploration of Radio Astrometry (VERA) Array (KaVA) is the first international VLBI array dedicated to high-frequency (23 GHz (K-band) and 43 GHz (Q-band)) observations in East Asia. To evaluate the imagine capability of KaVA, we performed imaging observations of three bright active galactic nuclei (AGNs) known for their complex morphologies: 4C 39.25, 3C 273, and M87 by KaVA at K-/Q-band. Our KaVA images reveal extended outflows with complex substructure such as knots and limb brightening, in agreement with previous observations by other VLBI facilities. Angular resolutions are better than 1.4 and 0.8 milliarcsecond (max) at K-/Q-band, respectively. KaVA achieves a high dynamic range of ~1000, more than three times the value achieved by VERA. We conclude that KaVA is a powerful array with a great potential for the study of AGN outflows, at least comparable to the best existing radio interferometric arrays.

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.633-636
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• 2015

KaVA (KVN and VERA Array) is a new combined VLBI array composed of KVN (Korean VLBI Network) and VERA (VLBI Exploration of Radio Astrometry). Here, we report the following two issues. (1) We review the initial results of imaging observations of M87 at 23 GHz following Niinuma et al. (2014). The KaVA images reveal extended outflows including complex substructures such as knots and limb-brightening, in agreement with previous VLBI observations. KaVA achieves a high dynamic range of ~1000, more than three times better than that achieved by VERA alone. (2) Based on subsequent observations and discussions led by the KaVA AGN SubWorking Group, we set monitoring observations of Sgr $A^{\ast}$ and M87 as our Key Science Project (hereafter KSP) because of the closeness and largeness of their central super-massive black holes. The main science goals of the KSP are (i) testing the magnetically-driven-jet paradigm by mapping velocity fields of the M87 jet, and (ii) obtaining tight constraints on physical properties of the radio emitting region in Sgr $A^{\ast}$. Towards KSP, we show the first preliminary images of M87 at 23 GHz and Sgr $A^{\ast}$ at 43 GHz with the bandwidth of 256 MHz.

• 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.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.103.2-103.2
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• 2012

NGC 2024 FIR 6 is a star formation site in Orion and may contain a hypercompact H II region, FIR 6c, and a low-mass protostar, FIR 6n. The FIR 6 region was observed in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz, using KVN in the single-dish telescope mode. The water maser spectra displayed several velocity components and month-scale time variabilities. Most of the velocity components may be associated with FIR 6n while one component was associated with FIR 4, another young stellar object in the 22 GHz beam. A typical life time of the water-maser velocity-components is about 8 months. The components showed velocity fluctuations with a typical drift rate of about 0.01 km/s/day. The methanol class I masers were detected toward FIR 6. The methanol emission is confined within a narrow range around the systemic velocity of the FIR 6 cloud core. The methanol masers did not show a detectable time-variability. The methanol masers suggest the existence of shocks driven by either the expanding H II region of FIR 6c or the outflow of FIR 6n.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.68.2-68.2
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• 2011

KVN은 2008년말에 3 대의 망원경 구축을 완료하고, 2009년에는 22/43 GHz 수신기를 각 망원경에 설치하였으며, 2009년말부터는 이 망원경들을 이용한 단일안테나 연구관측 및 VLBI 시험관측에 착수하였다. 2010년에는 86 Hz 수신기 1 대를 도입하였고, 129 GHz 수신기의 경우 믹스 개발을 완료한 후 현재 수신기 1대를 조립하고 있다. 적어도 1 set의 86/129 Hz 수신기가 금년 내에 연세망원경에 설치되어 시험관측이 수행될 예정이다. 2010년에는 또한 안테나의 크래딩 작업을 완료하여 지향성을 개선하였으며, 단일 안테나 연구관측 결과를 논문으로 생성하기도 하였다. 2011년말부터는 VLBI 연구관측에 착수할 예정이며, 관측시간의 50 %를 일본의 VERA와 공동관측에 활용할 예정이다. 2010년말에는 동아시아VLBI센터 건물의 건설이 착수되었으며, 2012년 6월경에 완공될 예정이다.