• 한국통신학회논문지
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• 제31권7B호
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• pp.573-582
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• 2006

본 논문에서는 기존 PON 구조와 단일 AWG 기반의 WDM-PON 구조의 문제점을 해결하고, 새로운 서비스 및 망의 증가 추세를 반영할 수 있는 혼합형 2단 AWG 기반의 WDM-PON 구조를 제안한다. 제안한 구조는 하향 전송을 위하여 2단 AWG를 사용하고, 상향 전송을 위하여 단일 AWG와 결합기를 사용함으로써 RN을 구성한다. 이러한 구조적 특징으로 인하여 제안한 구조는 확장성이 좋고, 낮은 비용과 높은 대역을 제공할 수 있다. 제안한 구조에서 하향 전송의 경우 트래픽이 별도의 하향 채널을 통하여 각 ONU에게 전송되므로 하향 트래픽에 대한 투명성 및 보안능력을 제공할 수 있다. 반면 상향 전송은 통신의 비대칭적인 특성을 고려해 다수의 ONU가 WDM/TDMA 기법을 사용함으로써 하나의 채널을 공유하는 형태이다. 본 논문에서는 제안한 구조의 성능 평가를 위하여 구성에 따른 망 구성의 전체 비용, 망 용량 , 각 ONU에게 할당 가능한 평균 상 하향 전송 대역 관점에서 비교 분석한다.

• Current Optics and Photonics
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• 제2권1호
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• pp.15-22
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• 2018

To measure atmospheric temperature, water vapor, and aerosol simultaneously, an efficient multi-function Raman lidar using an ultraviolet-wavelength laser has been developed. A high-performance spectroscopic box that utilizes multicavity interference filters, mounted sequentially at small angles of incidence, is used to separate the lidar return signals at different wavelengths, and to extract the signals with high efficiency. The external experiments are carried out for simultaneous detection of atmospheric temperature, water vapor, and aerosol extinction coefficient in Beijing, under clear and hazy weather conditions. The vertical profiles of temperature, water vapor, and aerosol extinction coefficient are analyzed. The results show that for an integration time of 5 min and laser energy of 200 mJ, the mean deviation between measurements obtained by lidar and radiosonde is small, and the overall trend is similar. The statistical temperature error for nighttime is below 1 K up to a height of 6.2 km under clear weather conditions, and up to a height of 2.5 km under slightly hazy weather conditions, with 5 min of observation time. An effective range for simultaneous detection of temperature and water vapor of up to 10 km is achieved. The temperature-inversion layer is found in the low troposphere. Continuous observations verify the reliability of Raman lidar to achieve real-time measurement of atmospheric parameters in the troposphere.

• Bulletin of the Korean Chemical Society
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• 제28권7호
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• pp.1187-1194
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• 2007

The three major active isoflavonoids (calycosin-7-O-β -glucoside, isomucronulatol 7-O-β-glucoside, formononetin) and two main saponins (astragaloside I, astragaloside IV) in an extract of Radix Astragali were determined using rapid, sensitive, reliable HPLC/UV and LC-ESI-MS/MS methods. The separation conditions employed for HPLC/UV were optimized using a phenyl-hexyl column (4.6 × 150 mm, 5 μm) with the gradient elution of acetonitrile and water as the mobile phase at a flow rate of 1.0 mL/min and a detection wavelength of 230 nm. The specificity of the peaks was determined using a triple quadrupole tandem mass spectrometer equipped with an electrospray ionization (ESI) source that was operated in multiple reaction monitoring (MRM) in the positive mode. These methods were fully validated with respect to the linearity, accuracy, precision, recovery and robustness. The HPLC/UV method was applied successfully to the quantification of three major isoflavonoids in the extract of Radix Astragali. The results indicate that the established HPLC/UV and LC-ESI-MS/MS methods are suitable for the quantitative analysis and quality control of multi-components in Radix Astragali.

• 천문학회보
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• 제39권2호
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• pp.78.2-78.2
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• 2014

MIRIS (Multi-purpose Infrared Imaging System) is the primary payload on the Korean science and technology satellite, STSAT-3, which was launched on 2013 November 21. It is designed to observe the near-infrared sky with a $3.67^{\circ}{\times}3.67^{\circ}$ field of view and a $51.6^{{\prime}{\prime}}{\times}51.6^{{\prime}{\prime}}$ pixel resolution. Using two narrow-band filters at $1.88{\mu}m$ (Pa ${\alpha}$ line) and $1.84+1.92{\mu}m$ (Pa ${\alpha}$ dual continuum), the Paschen ${\alpha}$ Galactic plane survey has been carrying out, and the area for the Galactic longitude from $+280^{\circ}$ to $+100^{\circ}$ (with the width of $-3^{\circ}$ < b < $+3^{\circ}$) has been covered by 2014 August 31. In this contribution, we present the preliminary results of the MIRIS Paschen ${\alpha}$ emission maps and compare them with other wavelength maps such as $H{\alpha}$ and dust maps. Many of the Paschen ${\alpha}$ features have been detected along the plane, and some of them are weak or invisible in the $H{\alpha}$ map and coincide well with dense cloud regions.

• 한국통신학회논문지
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• 제30권7A호
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• pp.535-541
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• 2005

본 논문은 채널을 파장별로 할당하는 방식인 WDM-PON을 각각의 채널당 단일광원을 사용하는 방식을 이용하여 기가비트 전송이 가능한 GPON 표준에 맞춰 단일 모드 광섬유와 다중 모드 광섬유로 혼합 구성된 망을 제안하고, 제안된 시스템의 전송 특성을 실험을 통해 고찰하였다. 본 시스템은 고속의 하향전송을 위해 직접변조가 가능한 DFB-LD를 사용하였고, 상향전송을 위해서는 저가의 ONU구성을 위해 SFP 타입의 Transceiver모듈을 사용하였다. 광 선로구간에서의 파장다중화를 위해서 채널 결합 및 분기기능을 갖는 MUX/DEMUX를 이용하였으며, SMF로 이루어진 WDM-PON망의 ONU단에 추가로 1km이내의 MMF를 연결시켜 두 라인을 혼합시킨 시스템을 구성하였다. 시스템의 타당성을 입증하기 위해 ITU-T G.984.2에서 권고하는 하향 2.5 Gbit/s, 1.25 Gbit/s, 상향 1.25 Gbit/s, 622 Mbit/s 속도의 전송실험을 하였으며, 표준안을 근거로 비교분석하여 상$\cdot$하향 전송에서 적합성과 여유도를 확인하였다.

• 대한전자공학회논문지SD
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• 제37권6호
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• pp.57-63
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• 2000

다분기 열광학 스위치는 수위칭 상태에 딸 요구되는 소비전력의 차이가 큰 단점이 있다. 이를 개선하는 방법으로 전극형태에서 외측전극폭을 내측전극폭에 비해 크게 설계하고 굴절률차이가 큰 코아와 클래드 물질을 사용하여 상부클래드의 두께를 얇게 하는 방법을 제안한다. 제안된 형태의 4분기 열광학스위치는 테플론과 폴리이미드계 폴리머 물질을 사용하여 제작되었고 1550 nm 파장대에서 그 특성을 측정하였다. 제작되어진 4분기 열광학스위치는 310~390 mW 정도의 소비전력에서 -16 dB 이하의 누호 특성을 나타 내어 스위칭 상태에 따른 소비전력의 차가 줄었을 뿐만 아니라 스위칭에 필요한 소비전력도 상당히 줄었다. 그리고 4.7 dB 정도의 삽입손실과 1 ms 이하의 스위칭 속도를 얻었다.

• 천문학회보
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• 제35권1호
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• pp.39.2-39.2
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• 2010

In this paper, I present the domestic development of near infrared camera systems for the ground telescope and the space satellite. These systems are the first infrared instruments made for astronomical observation in Korea. KASINICS (KASI Near Infrared Camera System) was developed to be installed on the 1.8m telescope of the Bohyunsan Optical Astronomy Observatory (BOAO) in Korea. KASINICS is equipped with a $512{\times}512$ InSb array enable L band observations as well as J, H, and Ks bands. The field-of-view of the array is $3.3'{\times}3.3'$ with a resolution of 0.39"/pixel. It employs an Offner relay optical system providing a cold stop to eliminate thermal background emission from the telescope structures. From the test observation, limiting magnitudes are J=17.6, H=17.5, Ks=16.1 and L(narrow)=10.0 mag at a signal-to-noise ratio of 10 in an integration time of 100 s. MIRIS (Multi-purpose InfraRed Imaging System) is the main payload of the STSAT-3 in Korea. MIRIS Space Observation Camera (SOC) covers the observation wavelength from $0.9{\mu}m$ to $2.0{\mu}m$ with a wide field of view $3.67^{\circ}{\times}3.67^{\circ}$. The PICNIC HgCdTe detector in a cold box is cooled down below 100K by a micro Stirling cooler of which cooling capacity is 220mW at 77K. MIRIS SOC adopts passive cooling technique to chill the telescope below 200K by pointing to the deep space (3K). The cooling mechanism employs a radiator, a Winston cone baffle, a thermal shield, MLI of 30 layers, and GFRP pipe support in the system. Opto-mechanical analysis was made in order to estimate and compensate possible stresses from the thermal contraction of mounting parts at cryogenic temperatures. Finite Element Analysis (FEA) of mechanical structure was also conducted to ensure safety and stability in launching environments and in orbit. MIRIS SOC will mainly perform the Galactic plane survey with narrow band filters (Pa $\alpha$ and Pa $\alpha$ continuum) and CIB (Cosmic Infrared Background) observation with wide band filters (I and H) driven by a cryogenic stepping motor.

• 천문학회보
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• 제35권1호
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• pp.27.2-27.2
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• 2010

We have studied the formation of coronal holes (CHs) associated with halo CMEs. For this study, we used multi-wavelength data from Yohkoh Soft X-ray Telescope (SXT), GOES Soft X-ray Imager (SXI), SOHO EIT 195 ${\AA}$, SOHO MDI magnetogram, MLSO He I 10830 ${\AA}$, and BBSO H-alpha. The CHs are characterized by open magentic field regions with low emission, density, and temperature and their open fields drive high speed solar winds which cause geomagnetic storms. So far, the formation and the evolution of CHs are not well understood. The formation of the dark region associated with the eruption of a CME is well known as "coronal dimming" which may be caused by the mass depletion near the CME footpoint. It is different from a typical CH since it persists for only one or two days. In this study, we present three cases that show the formation of coronal holes which are associated with three halo CMEs: 1) 2000 Jul 14, 2) 2003 Oct 28, 3) 2005 May 13. In the first case, hot plasma was ejected during a weak eruption and then filled out the pre-existing CH. After the halo CME occurred, the hot plasma region becomes a CH again. In the second and the third cases, we found newly formed CHs just after their associated CMEs. All three coronal holes are associated with strong flares and persist over 3 days until they disappeared by the solar rotation. Examining the MDI magnetograms, we found that the magnetic polarity of each CH region has one polarity. Based on these results, we suggest that the coronal holes can be formed by the CMEs and they should be distinguished from the coronal dimming.

• 천문학회보
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• 제42권1호
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• pp.45.1-45.1
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• 2017

Optical variability is one way to probe the nature of the central engine of AGN at smaller linear scales, and previous studies have shown that optical variability of AGN is more prevalent at longer timescales and at shorter wavelengths. To understand the properties and physical mechanism of variability, we are performing the KMTNet Active Nuclei Variability Survey (KANVaS). Especially, we investigated intra-night variability of AGN with KMTNet data which observed COSMOS field during 3 separate nights from 2015 to 2016 in B, V, R, and I bands. Each night was composed of 5, 9, and 11 epochs with 20-30 min cadence. To find AGN in the COSMOS field, we applied multi-wavelength selection methods. Using X-ray, mid-infrared, and radio selection methods, 50-60, 130-220, 20-40 number of AGN are detected, respectively. Achieving photometric uncertainty ~0.01mag by differential photometry, we employed a standard time-series analysis tool to identify variable AGN, chi-square test. Preliminary results indicate that there is no evidence of intra-night optical variability of AGN. It is possible that previous studies discovered intra-night variability used inappropriate photometric error. However, main reason seems that our targets have fainter magnitude (higher photometric error) than that of previous studies. To discover variability of AGN, we will investigate longer timescale variability of AGN.

• 천문학회보
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• 제43권1호
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• pp.44.1-44.1
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• 2018

We present a spectroscopic study of the Galactic supernova remnant (SNR) Cygnus Loop using the fifth Data Release (DR5) of LAMOST. The LAMOST (Large Sky Area Multi-Object Fiber Spectroscopic Telescope) features both a large field-of-view (about 20 deg2) and a large aperture (~4 m in diameter), which allow us to obtain 4000 spectra simultaneously. Its wavelength coverage ranges from ${\sim}3700{\AA}$ to $9000{\AA}$ with a spectral resolution of $R{\approx}1800$. The Cygnus Loop is a prototype of middle-aged SNRs, which has advantages of being bright, large in angular size (${\sim}3.8^{\circ}{\times}3^{\circ}$), and relatively unobscured by dust. Along the line of sight of the Cygnus Loop, 2747 LAMOST DR5 spectra are found in total, which are spatially distributed over the entire remnant. Among them, 778 spectra are selected based on the presence of emission lines (i.e., [O III]${\lambda}5007$, Ha, and [S II]${\lambda}{\lambda}$ 6717, 6731) for further visual inspection. About half of them (336 spectra) show clear spectral features to confirm their association with the remnant, 370 spectra show stellar features only, and 72 spectra are ambiguous and need further investigation. For those associated with the remnant, we identify emission lines and measure their intensities. Spectral properties considerably vary within the remnant, and we compare them with theoretical models to derive physical properties of the SNR such as electron density and temperature, and shock velocity. While some line ratios are in good agreement with model prediction, others cannot be explained by simple shock models with a range of shock velocities. We discuss these discrepancies between model predictions and the observations and finally highlight the powerfulness of the LAMOST data to investigate spatial variations of physical properties of the Cygnus Loop.