• 천문학회지
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• 제38권2호
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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.

• 천문학회지
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• 제38권2호
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• pp.257-260
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• 2005

We have mapped the W 3 giant molecular cloud in the $C^o\;^3P_1-^3 P_o$ ([CI]) line with the Mount Fuji Submillimeter-wave Telescope. The [CI] emission is extended over the molecular cloud, having peaks at three star forming clouds; W 3(Main), W 3(OH), and AFGL 333. The [CI] emission is found to be strong in the AFGL 333 cloud. We have also observed the $C^{18}O,\;CCS,\;N_2H^+$, and $H^{13}CO^+$ lines by using the Nobeyama Radio Observatory 45 m telescope. In the AFGL 333 cloud, we find two massive cores, which are highly gravitationally bound and have no sign of active star formation. The high [$C^o$]/[CO] and [CCS]/[$N_2H^+$] abundance ratios suggest that the AFGL 333 cloud is younger than the W 3(Main) and W 3(OH) clouds.

• 천문학논총
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• 제32권1호
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• pp.251-255
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• 2017

Submillimetre and millimetre-wave surveys with Herschel and the South Pole Telescope have revolutionised the discovery of strong gravitational lenses. Their follow-ups have been greatly facilitated by the multi-wavelength supplementary data in the survey fields. The forthcoming Euclid optical/near-infrared space telescope will also detect strong gravitational lenses in large numbers, and orbital constraints are likely to require placing its deep survey at the North Ecliptic Pole (the natural deep field for a wide class of ground-based and space-based observatories including AKARI, JWST and SPICA). In this paper I review the current status of the multi-wavelength survey coverage in the NEP, and discuss the prospects for the detection of strong gravitational lenses in forthcoming or proposed facilities such as Euclid, FIRSPEX and SPICA.

• 한국전자파학회논문지
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• 제26권10호
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• pp.851-868
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• 2015

밀리미터파 및 서브 밀리미터파 전파천문학용 전파망원경은 주로 카세그레인 형태의 안테나를 사용한다. 다양한 전파 천문학 연구를 위해서 한 개의 카세그레인 안테나에 여러 개의 수신대역을 갖는 수신기가 설치된다. 한 개 이상의 수신 대역을 관측하기 위해서는 여러 개의 수신기가 우주전파를 관측할 수 있는 빔 가이딩 시스템이 반드시 필요하게 된다. 이러한 빔 가이딩 시스템은 가우시안 빔 전송이론을 기반으로 준광학 회로로 구성된다. 본 논문에서는 가우시안 빔의 간략한 전송이론을 기반으로 한 가우시안 빔의 변환 방법과 가우시안 빔을 전송하기 위한 빔 전송회로 설계 기법을 제시한다. 이 설계기법을 이용하여 카세그레인 안테나에 적용되는 가우시안 빔 회로 설계와 설계 결과를 기술한다. 마지막으로 준광학 회로 구성부품인 타원면경, 유전체 렌즈 및 혼의 제원 결정에 대하여 기술한다. 제안된 방법을 이용하면 카세그레인 안테나 빔 가이딩 시스템을 간단히 설계할 수 있을 것으로 기대된다.