• 천문학논총
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• 제29권3호
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• pp.45-52
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• 2014

This paper describes the development of algorithm for direct data transmission between Raw VLBI Data Buffer (RVDB) and Huge Capacity Data Server (HCDS) operated in Korea-Japan Correlation Center (KJCC). The transmitted data is the VLBI observation data, which is recorded at each radio telescope site, and the data transmitting rate is varying from 1 Gbps, in usual case, upto 8 Gbps. The developed algorithm for data transmission enables the direct data transmission between RVDB and HCDS through 10 Gbps optical network using VLBI Data Interchange Format (VDIF). Proposed method adopts the conventional UDP/IP protocol, but in order to prevent the loss of data during data transmission, the packet error monitoring and data re-transmission functions are newly designed. The VDIF specification and VDIFCP (VDIF Control Protocol) are used for the direct data transmission between RVDB and HCDS. To validate the developed algorithm for data transmission, we conducted the data transmission from RVDB to HCDS, and compared to the transmitted data with the original data bit by bit. We confirmed that the transmitted data is identical to the original data without any loss and it has been recovered well even if there were some packet losses.

• 한국정보통신학회논문지
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• 제15권3호
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• pp.719-724
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• 2011

최근 대부분의 가정에서 자식을 하나만 나아서 기르는 저출산 시대가 왔다. 이에 따라 부모들은 태어나면서부터 아이에게 지대한 관심을 가지게 되고, 헬스케어(Healthcare) 분야가 새로운 성장산업으로 부상하면서 (베이비 케어)Baby Care에 대한 관심 또한 높아졌다. 지금까지의 Baby Care 제품은 식품, 목욕용품 그리고 의복 등에서 발전을 해 왔지만 유비쿼터스 컴퓨팅 환경의 발달과 헬스케어산업의 발달과 함께 Baby Care 전자 제품 개발이 이루어지고 있다. 유럽이나 미국 등에서는 유아를 다른 방에서 키운다. 이때 유아가 돌연사하는 현상이 종종 일어나는데 이를 예방하기 위해서 유아의 상태를 측정하고, 부모가 유아에게 떨어져 있어도 유아의 상태를 확인할 수 있는 Platform를 구현하였다. 본 논문에서는 기존의 라디오 주파수를 이용하여 데이터 저장 없이 부모의 실시간 관찰에 의해서만 판단했던 시스템을 고속의 ARM11 기반의 S3C6410 CPU를 이용하고, 무선 WI-FI(IEEE8.2.11)기술을 활용한 유아 돌연사 방지 Platform구현에 대한 연구를 진행하였다.

• 천문학논총
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• 제27권3호
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• pp.71-80
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• 2012

We have developed superconducting mixer receivers for 129 GHz VLBI observation in Korean VLBI Network (KVN). The developed mixer has a radial waveguide probe with simple transmission line L-C transformer as a tuning circuit to its 5 series-connected junctions, which can have 125 - 165 GHz as the operation radio frequency (RF). For intermediate frequency (IF) signal path a high impedance quarter-wavelength line connects the probe to one end of symmetric RF chokes. The double side band (DSB) receiver noise of the mixer was about 40 K over 4 - 6 GHz IF band, whereas we achieved the uncorrected single side band (SSB) noise temperature of about 70 K and better than 10 dB image rejection ratio in 2SB configuration with 8 - 10 GHz IF band. Insert-type receiver cartridges employing the mixers have been under commission for KVN stations.

• 천문학논총
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• 제30권2호
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• pp.61-64
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• 2015

The brightness of Io's magnetic footprint, an indicator of electromagnetic interaction at the satellite, appears to be strongly connected to the satellite's distance from the plasma equator. As a result, the brightest footprints were detected when Io is near the interception location between the satellite's orbital plane and the plasma equator. However, volcanic activities on Io show strong correlation with the equatorward shift of Jupiter's main auroral oval, consequently causing the disappearance of Io's footprint. The same conclusion was suggested via the observation of Jupiter's hectometric radio emission, called HOM, which closely corresponds to Jupiter's auroral activity. The plasma environment near the Jovian satellites was found to vary significantly at different observational epochs. The electron density increased by approximately a factor of three from the Voyager epoch (1979) to the Galileo epoch (1995), while the electron density was found to be significantly higher (~ 5 times) in the Cassini epoch (2001). In this current study, the magnetic footprints were clearly brighter ten years ago (from peak brightness in 1998-2001) than the footprints detected in 2007. For volcanic activities on Io in 2007, there are two clear activities in February and late May. The magnetic footprint appeared to be dimmer in March 2007, expected to be the result of volcano activities in Feb 2007. However, the magnetic footprint brightness in June appeared to be slightly brighter than the footprints observed in May. The reason could be the time delay between the brightening of the sodium nebula on approximately May 31st and, a while later, the enhancement of flux tube content peaking on approximately June 5th. On the other hand, Io's magnetic footprints were observed during June 1st - 10th when they may not yet have been affected by the increase in mass outflow due to the increase of plasma density.

• 천문학회보
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• 제37권2호
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• pp.239.1-239.1
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• 2012

This paper presents the results of one of early sciences with Korean VLBI Network (KVN): a large fringe survey of compact radio sources at 43GHz. We established the catalog of correlated flux densities in three ranges of baseline projection lengths of 637 sources from a 43 GHz (Q-band) survey observed with the Korean VLBI Network. Of them, 623 sources have not been observed before at Q-band with VLBI. The goal of this work in the early science phase of the new VLBI array is twofold: to evaluate the performance of the new instrument that operates in a frequency range of 22--129 GHz and to build a list of objects that can be used as targets and as calibrators. We have observed the list of 799 target sources with declinations down to $-40{\circ}$. Among them, 724 were observed before with VLBI at 22 GHz and had correlated flux densities greater than 200 mJy. The overall detection rate is 78%. The detection limit, defined as the minimum flux density for a source to be detected with 90% probability in a single observation, was in a range of 115--180 mJy depending on declination. However, some sources as weak as 70 mJy have been detected. Of 623 detected sources, 33 objects are detected for the first time in VLBI mode. We determined their coordinates with the median formal uncertainty 20 mas. The results of this work set the basis for future efforts to build the complete flux-limited sample of extragalactic sources at frequencies 22 GHz and higher at 3/4 of the celestial sphere.

• 천문학회보
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• 제37권2호
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• pp.84.1-84.1
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• 2012

One of the most intriguing questions regarding black hole (BH)-galaxy co-evolution picture is how the BH accretion, or active galactic nucleus (AGN) activity is linked to star formation (SF) activity. While it is suggested that AGN luminosity of quasars correlates with SF luminosity, it is still unclear how AGN activity is connected to SF activity based on host galaxy properties. Utilizing AKARI's unique slit-less spectroscopic capability and wavelength coverage, we probed star formation activity of several types of AGNs by measuring the PAH 3.3 ${\mu}m$ emission. First, we detected the PAH 3.3 ${\mu}m$ emission from seven out of 27 Seyfert type-1 galaxies at z~0.36. While these galaxies deviate significantly from the local Mbh-${\sigma}$ relation meaning their black holes proceed the host galaxies in terms of evolution, they appear to follow the correlation between nuclear SF and AGN activities of local Seyfert type-1 galaxies. This implies that SF and AGN activities are directly connected at the nuclear region for these Seyfert type-1 AGNs. We also obtained 2-5 ${\mu}m$ spectra for subsamples of Quasar Spectroscopic Observation in Near-infrared Grism (QSONG) which consists of reverberation-mapped AGNs and PG-QSOs. We detected the PAH 3.3 ${\mu}m$ emission from 16 out of 31 reverberation-mapped AGNs and 10 out of 49 PG-QSOs and measured their line strengths. We present the correlations between SF and AGN activities and discuss if there is any dependency of the correlations on properties of host galaxies, such as morphology, or the presence of radio jets.

• 마이크로전자및패키징학회지
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• 제9권4호
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• pp.55-60
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• 2002

본 연구는 $580^{\circ}C$의 저온에서 ICPHFCVD(inductively coupled plasma hot filament chemical vapor deposition)를 이용하여 탄소나노튜브를 수직성장 시키는 것을 나타낸 것이다. 또한, 탄소나노튜브의 끝단에 존재하는 Ni-tip을 비성질 탄소같은 탄소질 물질등의 서로 다른 에칭특성에 기초하여 RF plasma를 이용하여 일회 공정으로 불순물을 정제하고, 고찰하였다. 정제된 이후의 탄소나노튜브는 속이 비어있는 다중벽 탄소나노튜브로 나타났으며, 성장된 탄소나노튜브는 외경과 내경은 50 nm와 25 nm였다. 또한, 탄소나노튜브의 graphite 층의 총수는 약 82개 층으로 구성되었으며, 층과 층간의 거리는 0.34nm였다. 그리고 TEM 관찰 결과, 탄소나노튜브 tip의 Ni촉매는 계속적인 에칭 공정에 의해 효과적으로 제거 되었다.

• 천문학회보
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• 제44권1호
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• pp.42.2-42.2
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• 2019

Turbulence is one of the natural phenomena in molecular clouds. It affects gas density and velocity fluctuation within the molecular clouds and controls the mode and tempo of star formation. However, despite many years of study, the properties of turbulence remain poorly understood. As part of the Taeduk Radio Astronomy Observatory (TRAO) Key Science Program (KSP), "mapping Turbulent properties In star-forming MolEcular clouds down to the Sonic scale (TIMES; PI: Jeong-Eun Lee)", we have fully mapped two star-forming molecular clouds, the Orion A and the Ophiuchus molecular clouds, in 3 sets of lines ($^{13}CO$ J=1-0, $C^{18}O$ J=1-0, HCN J=1-0, $HCO^+$ J=1-0, CS J=2-1, and $N_2H^+$ J=1-0) using the TRAO 14-m telescope. We apply a statistical analysis, Principal Component Analysis (PCA), which can recover an underlying turbulent-power spectrum from an observed P-P-V spectral map. We compare turbulence properties not only between the two clouds, but also between different parts within each cloud. We present the first result of our observation program.

• 한국전자통신학회논문지
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• 제15권6호
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• pp.1045-1054
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• 2020

본 논문에서는 불안정한 네트워크 환경에서 안정적으로 대용량 데이터 스트림을 전송할 수 있는 TCP/IP 기반 링 버퍼 시스템을 설계하였다. 우리가 제안한 방식에서 각 전파천문대의 백엔드 시스템으로부터 UDP 프레임으로 생성 및 출력되는 관측 데이터 스트림은 클라이언트 시스템 내의 소켓 버퍼를 경유해 대용량 링 버퍼에 UDP 패킷으로 저장된다. 이후 목적지에 해당하는 상관센터로의 안정적인 전송을 위해 해당 패킷은 TCP로 전송되고 상관센터 내의 서버 시스템은 소켓 버퍼에 수신된 패킷에 이상이 없으면 대용량 링 버퍼에 저장한다. 패킷 손실, 중복 및 순서 역전 등의 이상이 발생할 경우 TCP의 흐름 제어를 통해 패킷은 재전송되며 상관센터에 도착한 데이터는 신뢰성을 보장받게 된다. 또한 네트워크 성능 불안정으로 인한 혼잡 회피 발생 시 병렬 스트림 적용을 통해 성능 저하가 최소화될 수 있도록 하였다.

• 천문학논총
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• 제36권2호
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• pp.37-45
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• 2021

We have analyzed 42 research papers regarding on the solar astronomy written by North Korea scientists to investigate the current status of astronomical activities in North Korea. The papers are surveyed from the 'Bulletin of Astronomy', the 'Physics', the 'Bulletin of Academy of Science', and the 'Natural Science' in North Korea, and SCI journals. In addition, we refer to the presentation material announced in the 2015 IAU by director of Pyongyang Astronomical Observatory (PAO) and the 2013 OAD/IAU reports. We have analyzed the papers statistically according to three criteria such as research subject, research field, and research members. The main research subjects are the sunspot (28%), observation system (21%), and space environments (19%). The research fields are distributed with data analysis (50%), numerical method (29%), and instrument development (21%). There have been 25 and 9 researchers in the solar astronomy and space environment, respectively since 1995. North Korea's solar research activities were also investigated in three area: instrument, solar physics, and international research linkage. PAO has operated two of sunspot telescope and solar horizontal telescope for spectroscopy and polarimetry, but there is no specific information on solar radio telescopes. North Korea has cooperated in solar research with Europe and China. We expect that the results of this study will be used as useful resource in supporting astronomical cooperation between South and North Korea in the future.