• 천문학회보
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• 제45권1호
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• pp.46.1-46.1
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• 2020

DEEP-South (DEep Ecliptic Patrol of the Southern Sky) team will start the 2nd phase of KMTNet observation in Oct 2020. The DEEP-South observation mainly consists of three survey modes: (1) Activity survey (AS) that aims at finding active phenomena of small Solar System bodies. (2) Light curve survey (LS) targets to discover and characterize light variations of asteroids. And (3) Deep drilling survey (DS) focuses on the objects beyond the orbit of Jupiter (Centaurus and trans-Neptunian objects) as well as near Earth asteroids. For asteroid family (AF) studies and target of opportunity (TO) observations for urgent photometric follow-up, targeted mode will also be used. DEEP-South team is awarded 7.0% of the telescope time at each site every year from Oct 2020 to Sep 2023 in the 2nd phase of KMTNet operation which corresponds to about 75 full nights a year for the network. In this presentation, we will introduce our survey strategy and observation plan.

• Journal of Chest Surgery
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• 제30권7호
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• pp.733-738
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• 1997

순차적 양측 폐이식수술은 수술시 및 수술후 합병증이 매우 다양하며 수술후 결과가 매우 불량하다. 저자 등은 양측 폐 이식수술후의 혈역학적 변화를 연구관찰하고자 하였으며 수술후 발생할 수 있는 거부반 응을 예방하기 위하여 양측 폐재식수술을 선택,시행하였으며 폐동맥의 뒤틀림이나 협착, 좌심방내의 혈전발 생 등을 예방하기 위하여 폐동맥 및 좌심방 부위를 혈관감자로 폐쇄시킨 후 폐측 폐동맥의 전면을 절단하였고, 폐측 상하 폐정맥부위 좌심방 전면을 절단한 후 1시간동안 폐동맥 절단부위를 통해 PGEI이 함유된 I-C 용액을 주입하였고 1시간동안 I-C용액이 함유된 거즈를 이용하여 냉각을 유지하였다. 다시 5-0 prolene을 이 용하여 봉합하였다. 좌심방을 봉합할 때 내면이 외 전되게끔 everted suture 방법으로 봉합하였다. 주기관지는 완전 절단후 telescope방법으코 단단문합하였으며 폐재식 수술전후의 동맥혈 산소가스치, 대퇴동맥 및 폐동맥 압을 측정하여 비교하였으며 수술전후의 뚜렷한 혈역학적 변화는 없었다. 절단 결찰된 폐는 PcEl이 함유된 I-c용액을 폐동맥으로 4o cmHlo 압력으로 Is ~h입분의 속도로 총량이 70 mfg되도록 주입하\ulcorner으며 그후 1시간동안 냉각된 I-C용액이 함유된 거즈를 이용하여 절단된 폐를 감싸서 냉각저류보관하여 허혈성 손상을 예방함으로써 수술수기에 대한 합병증이 없는한 양측 폐 이식수술후 성 적은 양호할 것으로 생각된다.

• 대한기관식도과학회지
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• 제8권2호
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• pp.36-42
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• 2002

Aspirated and ingested foreign bodies continue to present challenges to otolaryngologists. The major discussions were the accurate diagnosis and speedy, safe removal of foreign body. Many diagnostic tools have been tried and removal of foreign bodies has been facilitated by technical improvements with rod lens telescope, video endoscope, flexible fiberoendoscope and safer anesthesia. In spite of these advances, more than 3000 children's death occur per year in the world because of foreign bodies and untold number of parients survive with variable sequelae. In these study, 59 consecutive cases of children and adults with tracheobronchial foreign bodies were reviewed from 1992 to 2001. We studied the history, symptoms, ausculatory radiologic, bronchoscopic finding and post operative complications. 71% (42 cases in 59 cases) of patients had foreign body aspiration history or choking crisis. In 64% (38cases) cough was observed. 81% (48cases) had abnormal finding in chest auscultation and 78% in chest X-ray. Computed tomography was done in 12 cases, all were founded foreign body shadow. Main site of foreign body was right main bronchus (41%, 24cases) and most frequent foreign body was peanut (36% , 21cases) . 4 experienced ICU(intensive care unit) care. 2 cases were failed to remove foreign. In these cases 1 cases was improved by steroid therapy and physical therapy and the other was treated with thoracotomy. We concluded the morbidity and motality were much correlated with speedy decision making and experienced skill of operator.

• 천문학회지
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• 제42권6호
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• pp.161-174
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• 2009

Observation of standard stars is of crucial importance in stellar photometry. We have studied the standard transformation relations of the UBV RI CCD photometric system at the Maidanak Astronomical Observatory in Uzbekistan. All observations were made with the AZT-22 1.5m telescope, SITe 2k CCD or Fairchild 486 CCD, and standard Bessell UBV RI filters from 2003 August to 2007 September. We observed many standard stars around the celestial equator observed by SAAO astronomers. The atmospheric extinction coefficients, photometric zero points, and time variation of photometric zero points of each night were determined. Secondary extinction coefficients and photometric zero points were very stable, while primary extinction coefficients showed a distinct seasonal variation. We also determined the transformation coefficients for each filter. For B, V, R, and I filters, the transformation to the SAAO standard system could be achieved with a straight line or a combination of two straight lines. However, in the case of the U filter and Fairchild 486 CCD combination, a significant non-linear correction term - related to the size of Balmer jump or the strength of the Balmer lines - of up to 0:08 mags was required. We found that our data matched well the SAAO photometry in V, B - V, V - I, and R - I. But in U - B, the difference in zero point was about 3.6 mmag and the scatter was about 0.02 mag. We attribute the relatively large scatter in U -B to the larger error in U of the SAAO photometry. We confirm the mostly small differences between the SAAO standard UBV RI system and the Landolt standard system. We also attempted to interpret the seasonal variation of the atmospheric extinction coefficients in the context of scattering sources in the earth's atmosphere.

• International Union of Geodesy and Geophysics Korean Journal of Geophysical Research
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• 제26권1호
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• pp.43-58
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• 1998

The Kwinana Shoreline Fumigation Experiment (KSFE) took place at Fremantle, WA, Australia between January 23 and February 8, 1995. The CSIRO DAR LIDAR measured plume sections from near the Kwinana Power Station (KPS) stacks to up to about 5 km downstream. It also measured boundary layer aerosols and the structure of the boundary layer on some occasions. Both stages A and C of KPS were used as tracers at different times. The heart of the LIDAR system is a Neodymium-doped Yttrium-aluminum-garnet (Nd:YAG) laser operating at a fundamental wavelength of 1064 nm, with harmonics of 532 nm and 355 nm. For these experiments the third harmonic was used because the UV wavelength at 355 nm is eye safe beyond about 50 m. The laser fires a pulse of light 6 ns in duration (about 1.8 m long) and with an energy (at the third harmonic) of about 70 mJ. This pulse subsequently scattered and absorbed by both air molecules and particles in the atmosphere. A small fraction of the laser beam is scattered back to the LIDAR, collected by a telescope and detected by a photo-multiplier tube. The intensity of the signal as a function of time is a measure of the particle concentration as a function of distance along the line of the laser shot. The smoke plume was clearly identifiable in the scans both before and after fumigation in the thermal internal boundary layer (TIBL). Both power station plumes were detected. Over the 9 days of operation, 1,568 plumes scans (214 series) were performed. Essentially all of these will provide instantaneous plume heights and widths, and there are many periods of continuous operation over several hours when it should be possible to compile hourly average plume statistics as well. The results of four days LIDAR observations of the dispersion of smoke plume in the TIBL at a coastal site are presented for the case of stages A and C.

• Journal of Astronomy and Space Sciences
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• 제32권3호
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• pp.237-245
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• 2015

A strategy is needed for a regional survey of geosynchronous orbits (GSOs) to monitor known space objects and detect uncataloged space objects. On the basis of the Inter-Agency Debris Committee's recommendation regarding the protected region of geosynchronous Earth orbit (GEO), target satellites with perigee and apogee of $GEO{\pm}200km$ and various inclinations are selected for analysis. The status of the GSO region was analyzed using the satellite distribution based on the orbital characteristics in publicly available two-line element data. Natural perturbation effects cause inactive satellites to drift to two stable longitudinal points. Active satellites usually maintain the designed positions as a result of regular or irregular maneuver operations against their natural drift. To analyze the detection rate of a single optical telescope, 152 out of 412 active satellites and 135 out of 288 inactive satellites in the GSO region were selected on the basis of their visibility at the observation site in Daejeon, Korea. By using various vertical view ranges and various numbers of observations of the GSO region, the detection efficiencies were analyzed for a single night, and the numbers of follow-up observations were determined. The orbital estimation accuracies were also checked using the arc length and number of observed data points to maintain the GSO satellite catalog.

• 천문학회지
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• 제31권2호
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• pp.161-171
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• 1998

We have mapped about 1.5 square degree regions of Lynds 1299, a well isolated dark cloud in the Outer Galaxy (l = $122^{\circ}$, b = $-7^{\circ}$), in the J = 1- 0 transition of $^{12}CO$ and $^{13}CO$ with the 13.7 m radio telescope at Taeduk Radio Astronomy Observatory (TRAO). We found that there are two velocity components in the molecular emission, at $V_{LSR} = -52 km S^{-1}$ (Cloud A) and -8.8 km $s^{-1}$ (Cloud B), respectively. We have derived physical parameters of two molecular clouds and discussed three different mass estimate techniques. We found that there are large discrepancies between the virial and LTE mass estimates for both clouds. The large virial mass estimate reflects the fact that both are not gravitationally bound. We adopt the mass of $5.6 {\times}10^3 \;M{\bigodot}$ for Cloud A and $1.2{\times}10^3 \;M{\bigodot}$) for Cloud B using conversion factor. Cloud A is found to be associated with a localized star forming site, and its morphology is well matching with that of far-infrared (FIR) dust emission. It shows a clear ring structure with an obvious velocity gradient. We suggest that it may be a remnant cloud from a past episode of massive star formation. Cloud B is found to be unrelated to Cloud A (d = 800 pc) and has no specific velocity structure. The average dust color temperature of the uncontaminated portion of Cloud A is estimated to be 24$\~$27.4 K. The low dust temperature may imply that there is no additional internal heating source within the cloud. The heating of the cloud is probably dominated by the interstellar radiation field except the region directly associated with the new-born B5 star. Overall, the dust properties of Cloud A are similar to those of normal dark cloud even though it does have star forming activity.

• 한국환경과학회:학술대회논문집
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• 한국환경과학회 1996년도 봄 학술발표회 초록집
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• pp.22-22
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• 1996

;The Kwinana Shoreline Fumigation Experiment(KSFE) took place in Fremantle, WA, Australia between 23 January and 8 February, 1995. All measurement systems performed to expectation. The CSIRO DAR(Division of Atmospheric Research) LIDAR measured plume sections from near the Kwinana Power Station(KPS) stacks to up to about 5 km downstream. It also measured boundary layer aerosols and the structure of the boundary layer on some occasions. Both stages A and C of KPS were used as tracers at different times. Radiosonde and double theodolite sounding systems measured temperature, humidity, air pressure and wind structure at the coast(Woodman Point) and at the inland(ALCOA residue dump) site at intervals of roughly two hours. These were supplemented by mid afternoon soundings(radiosonde and single theodolite) by Department of Environmental Protection(DEP) at Swanbourne. The Flinders aircraft measured wind, turbulence and temperature structure of the atmospheric boundary layer, concentrations of $C0_2,\;0_3,\;S0_2\;and\;NO_x$ in the smoke plumes and surface radiation over both land and sea. CSIRO DCET(Division of Coal and Energy Technology) vehicle successfully interceptde many smoke plumes and using a range of tracers will be able to identify the various sources much of the time. Routine data from the DEP and Kwinana Industrial Council(KIC) air quality monitoring networks were also automatically logged. Murdoch University measured surface heat flux at Hope Valldy monitoring station and also at Wattleup monitoring station for the last five days. The heart of the LIDAR system is a Neodymium-doped Yttrium-aluminumgarnet(Nd:Y AG) laser operating at a fundamental wavelength of 1064 nm, with harmonics fo 532 nm and 355 nm. A small fraction of the laser beam is scattered back to the LIDAR, collected by a telescope and detedted by a photomultiplier tube. The intensity of the signal as a function of time is a measure of the particle concentration as a function of distance along the line of the laser shot. The results of nine days special field observations are summarized in detail.etail.

• 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.

• 한국지구과학회지
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• 제40권5호
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• pp.464-475
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• 2019

대부분의 중 고등학교가 도심지에 위치하며 사용할 수 있는 천문 관측 장비에 제한이 있다는 점을 고려하여 DSLR 카메라와 교육용 소형 망원경을 결합하여 도심지 밤하늘 밝기를 측정하였다. DSLR 카메라의 다양한 설정은 ISO 설정 외에는 원본 파일에 영향을 주지 않았으며, 필터 변환까지 고려한 일반적인 측광 정밀도는 대략 0.1 등급이다. 밤하늘 밝기는 천정 부근의 경우 B, V, r 필터에서 각각 약 17.5, 17.1, $16.9mag\;arcsec^{-2}$으로 측정되었다. 이를 통해 도심지의 대략적인 한계등급은 B 필터에서 17.5 등급, V와 r 필터에서 17등급으로 추정할 수 있다. 관측지점과 가까운 대규모 인공 조명은 고도와 필터에 무관하게 밤하늘 밝기를 약 $0.6mag\;arcsec^{-2}$ 증가시킴으로써 관측 환경을 악화시키는 주요인으로 나타났다.