• Journal of The Korean Astronomical Society
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• v.55 no.6
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• pp.207-213
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• 2022

The Seoul Radio Astronomy Observatory (SRAO) operates a 6.1-meter radio telescope on the Gwanak campus of Seoul National University. We present the efforts to reform SRAO to a Very Long Baseline Interferometry (VLBI) station, motivated by recent achievements by millimeter interferometer networks such as Event Horizon Telescope, East Asia VLBI Network, and Korean VLBI Network (KVN). For this goal, we installed a receiver that had been used in the Combined Array for Research in Millimeter-wave Astronomy and a digital backend, including an H-maser clock. The existing hardware and software were also revised, which had been dedicated only to single-dish operations. After several years of preparations and test observations in 1 and 3-millimeter bands, a fringe was successfully detected toward 3C 84 in 86 GHz in June 2022 for a baseline between SRAO and KVN Ulsan station separated by 300 km. Thanks to the dual frequency operation of the receiver, the VLBI observations will soon be extended to the 1 mm band and verify the frequency phase referencing technique between 1 and 3-millimeter bands.

• Publications of The Korean Astronomical Society
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• v.32 no.1
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• pp.231-233
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• 2017

We have imaged the AKARI Deep Field with the GMRT radio telescope at 610 MHz, detecting 1224 radio components, which are optically identified with 455 optical galaxies having a mean r' magnitude brighter of 22.5 (to a completeness limit of 25.4 mag), and an average redshift ~ 0.8.

• Journal of The Korean Astronomical Society
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• v.29 no.spc1
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• pp.261-262
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• 1996

Nearly simultaneous observations for $^{28}SiO$ v=0, 1, 2, J =3-2 transitions in 39 late-type stars have been carried out in February 1995 and 1996 with the 14 m radio telescope at Taeduk Radio Astronomy Observatory (TRAO). Observations for $^{28}SiO$ v=0, 1, 2, J=2-1 lines in the same objects have been also carried out in March 1995 and March-April 1996. The detection rate of $^{28}SiO$ v=l, J=3-2 line for the $^{28}SiO$ v=l, J=2-1 sources was $59\%$. Seventeen new detections in the $^{28}SiO$ v=l, J=3-2 transition and 4 new detections in the $^{28}SiO$ v=2, J=3-2 transition have been reported including the intensity ratios within the vibrational ladders and rotational states.

• Journal of The Korean Astronomical Society
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• v.29 no.spc1
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• pp.173-174
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• 1996

We have mapped $17 deg^2$ region toward Galactic anticenter in $^{12}CO$ J = 1 - 0 using the 3 mm SIS receiver on the 14 m telescope at Taeduk Radio Astronomy Observatory (TRAO). The region mapped in this paper is the first target of the Galactic AntiCenter CO Survey Project (GACCOS) and was selected comparing with IRAS Sky Survey Atlas (ISSA) images at 100${\mu}m$. Molecular emission of the target area is found to be very extended and is well matching with the FIR emission boundary. There are several pieces of clouds, and as some of spectra show several peaks, there seem to be several clouds overlapped in some directions. The Velocity of Local Standard of Rest ($V_{LSR}$) of the CO emission of the mapped region ranges from -20 to +10 km/s. It is also found that the two cloudlets located around I = $180^{\circ}$ have $V_{LSR}$ = -20 km/s, which is very abnormal. The peak antenna temperature of 13 K arises near the H II Region S241.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.1
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• pp.33.4-34
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• 2017

전파망원경 레이돔은 14미터 우주전파망원경을 외부 환경(눈, 비, 바람, 햇빛)으로 부터 보호하여 효율적인 우주전파 관측연구를 수행하는데 필수적인 연구시설이다. 현재 사용 중인 대덕전파천문대 레이돔은 1985년에 설치되어 30년째 사용 중이다. 노후화로 인해 누수가 있으며, 겨울철에는 내부에 빙결이 발생하며, 유지보수가 어려운 상황이다. 본 발표에서는 2016년 12월말부터 2017년 2월 초까지 이루어진 레이돔의 교체과정과 기존 레이돔과 교체된 레이돔의 성능 등을 발표한다.

• Journal of The Korean Astronomical Society
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• v.29 no.spc1
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• pp.197-198
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• 1996

We have carried out $^{13}CO$ J = 1 $\to$ 0 line observations with spatial resolution of 2' toward 17 small globules selected from the catalogue of Clemens & Barvainis (1988) with a selection criterion of [b] $\ge$ 15 degrees using the Nagoya 4-m radio telescope. Overall characteristics and physical parameters are presented and discussed by examining the $^{13}CO$ integrated intensity map for each of the globules.

• Publications of The Korean Astronomical Society
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• v.7 no.1
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• pp.149-153
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• 1992

We determined the efficiencies of the aperture. beam and forward spillover and scattering of 13.7 m radio telescope at Daeduk Radio Astronomy Observatory through the observations of the planets and Moon. The main panels adjustments were carried out on September 1991 and the improvements in the efficiencies were checked by comparing the observations made before and after the panel adjustments. The efficiencies were turned out to be 0.35, 0,47 and 0.83 at 115.27 GHz for the aperture, beam and forward scattering and spillover. respectively. These marked nearly a factor of two upgrade of the efficiencies previously measured.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.49.2-49.2
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• 2011

To investigate whether radio galaxies have systematically different accretion disk compared to radio-quiet AGN, we obtained high quality optical spectra for a sample of 22 young radio galaxies, using the KAST Double Spectrograph at the Lick 3-m telescope. Young radio galaxies are particularly useful since the age of the radio phenomena is comparable to that of accretion disk. Based on the optical emission-line diagnostics of narrow line region, which is thought to be photoionized by the nuclear radiation, we constrain the states of the accretion disk. In addition to strong emission lines, i.e., [O I], [O II], [O III], and [Ne III], we use the [Ar III] line to break the degeneracy between the ionization parameter and the SED shape. We find that young radio galaxies show systematically different emission line ratios compared to radio-quiet Type II AGN, suggesting that young radio galaxies probably have the power-law SED without a strong big blue bump. We will present the main results of the emission-line diagnostics.

• Publications of The Korean Astronomical Society
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• v.14 no.2
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• pp.123-128
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• 1999

The beam size and the antenna efficiency of TRAO 14m radio telescope were measured at 86.2, 98.0 and 115.2 GHz. The beam size was determined by deconvolving the azimuthal scanning data of the Venus. To test the accuracy of our deconvolution method, the beam size at 86.2 GHz was compared with that determined from the mapping data of SiO maser line and we found no difference between them. With above beam sizes, antenna efficiencies were calculated from the continuum measurements of Venus, Jupiter and Moon. The beam efficiencies at these frequencies are appeared to be 0.49, 0.45 and 0.41, respectively. On the other hand, we also suggest that an automatic focus setting can be adopted for TRAO radio telescope based on the gradual change of best focus with elevation.

• Journal of The Korean Astronomical Society
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• v.38 no.2
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• pp.253-256
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• 2005

We have constructed the Mount Fuji submillimeter-wave telescope at Nishiyasugawara (alt. 3725 m) near the summit of Mt. Fuji (alt. 3774 m). Thanks to the excellent condition of Mt. Fuji, we have successfully carried out the [CI] survey toward more than 40 square degrees of sky, including qrion MC, Taurus MC, Rosetta MC, DR 15, DR 21, NGC 1333, NGC 2264, W 3, W 44, W 51, L 134, p-Oph. Our [CI] survey have revealed that the [CI] 492 GHz emission widely extends to the molecular clouds. The spatial and velocity structures of the [CI] 492 GHz emission resemble those of 13CO J=l-0 in many molecular clouds, implying that [CI] 492 GHz and $^{13}CO$ J=1-0 are emitted from the same gas. The column density of $C^o$ linearly correlates with that of CO up to high Av, suggesting that $C^o$ exist in the deep interior of molecular clouds. In several regions, we have found that the distributions of $C^o$ and CO are different from each other. The $C^o$-rich area is found in the Hieles' cloud 2. The C+/CO/$C^o$ configuration is found in DR 15, p-Oph, M 17, Orion KL, and NGC 1333. These results indicate that an origin of $C^o$ is unrelated with the photodissociation process. We discuss the observed $C^o$ distributions in relation to the non-equilibrium chemistry.