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우측 테리온을 통한 양측성 대칭성 내경동맥류의 결찰 : 증례 보고
여만수,조봉수,김대능,박화성,박상남,김상용,이동열 대한신경외과학회 1992 Journal of Korean neurosurgical society Vol.21 No.11
The known incidence of multiple aneurysm is about 5~30% in the literatures and bilateral symmetrical aneurysms are more than bilateral asymmetrical aneurysms. The microsurgical technique is so much developed to control the bilateral multiple aneurysm at one stage operation in recent The author report on case of bilateral carotid aneurysms clipped by right side pterional appraoch at one time, successfully.
SMA OBSERVATIONS OF THE HOT CORES OF DR21(OH)
Minh, Young Chol,Chen, Huei-Ru,Su, Yu-Nung,Liu, Sheng-Yuan The Korean Astronomical Society 2012 Journal of The Korean Astronomical Society Vol.45 No.6
Using the Submillimeter Array (SMA), we identified two bright hot subcores, MM1a and MM1b (size ~ 1" and mass ~ 0.5 $M_{\odot}$) separated by about 1.600, in the 230 GHz continuum emission toward the massive star-forming region DR21(OH). Both display typical hot core characteristics but have slightly different chemical properties. For example, highly saturated species show stronger emission toward MM1a and seem to be evaporating directly from the grain mantles. In contrast, simple sulfur-bearing species have brighter emission at MM1b. These features indicate that MM1a is at an earlier stage than MM1b, and the small-scale chemical differences between these two cores may result from the age difference of the order of $10^4$ years.
Data Hiding Using Sequential Hamming + k with m Overlapped Pixels
( Cheonshik Kim ),( Dongkyoo Shin ),( Ching-nung Yang ),( Yi-cheng Chen ),( Song-yu Wu ) 한국인터넷정보학회 2019 KSII Transactions on Internet and Information Syst Vol.13 No.12
Recently, Kim et al. introduced the Hamming + k with m overlapped pixels data hiding (Hk_ mDH) based on matrix encoding. The embedding rate (ER) of this method is 0.54, which is better than Hamming code HC (n, n- k) and HC (n, n- k) +1 DH (H1DH), but not enough. Hamming code data hiding (HDH) is using a covering function COV(1, n=2<sup>k</sup>-1, k) and H1DH has a better embedding efficiency, when compared with HDH. The demerit of this method is that they do not exploit their space of pixels enough to increase ER. In this paper, we increase ER using sequential Hk_mDH (SHk_mDH ) through fully exploiting every pixel in a cover image. In SHk_mDH, a collision maybe happens when the position of two pixels within overlapped two blocks is the same. To solve the collision problem, in this paper, we have devised that the number of modification does not exceed 2 bits even if a collision occurs by using OPAP and LSB. Theoretical estimations of the average mean square error (AMSE) for these schemes demonstrate the advantage of our SHk_mDH scheme. Experimental results show that the proposed method is superior to previous schemes.
INTERSTELLAR MEDIUM PROCESSING IN THE INNER 20 pc IN GALACTIC CENTER
Liu, Hauyu Baobab,Ho, Paul T. P.,Wright, Melvyn C. H.,Su, Yu-Nung,Hsieh, Pei-Ying,Sun, Ai-Lei,Kim, Sungsoo S.,Minh, Young Chol IOP Publishing 2013 The Astrophysical journal Vol.770 No.1
<P>We present the Submillimeter Array 157 pointing mosaic in 0.86 mm dust continuum emission with 5 ''.1 x 4 ''.2 angular resolution, and the National Radio Astronomy Observatory Green Bank 100 m Telescope (GBT) observations of the CS/(CS)-S-34/(CS)-C-13 1-0 and SiO 1-0 emission with <= 20 '' x 18 '' angular resolution. The dust continuum image marginally resolves at least several tens of 10-10(2) M-circle dot dense clumps in the 5' field including the circumnuclear disk (CND) and the exterior gas streamers. There is very good agreement between the high resolution dust continuum map of the CND and all previous molecular line observations. As the dust emission is the most reliable optically thin tracer of the mass, free from most chemical and excitation effects, we demonstrate the reality of the abundant localized structures within the CND, and their connection to external gas structures. From the spectral line data, the velocity dispersions of the dense clumps and their parent molecular clouds are similar to 10-20 times higher than their virial velocity dispersions. This supports the idea that the CND and its immediate environment may not be stationary or stable structures. Some of the dense gas clumps are associated with 22 GHz water masers and 36.2 GHz and 44.1 GHz CH3OH masers. However, we do not find clumps that are bound by the gravity of the enclosed molecular gas. Hence, the CH3OH or H2O maser emission may be due to strong (proto) stellar feedback, which may be dispersing some of the gas clumps.</P>
MILLIMETER OBSERVATIONS OF THE TRANSITION DISK AROUND HD 135344B (SAO 206462)
Lyo, A-Ran,Ohashi, Nagayoshi,Qi, Chunhua,Wilner, David J.,Su, Yu-Nung American Institute of Physics 2011 The Astronomical journal Vol.142 No.5
<P>We present ~1'' resolution 1.3 mm dust continuum and spectral line (<SUP>12</SUP>CO and <SUP>13</SUP>CO J = 2-1) observations of the transitional disk system HD 135344B obtained with the Submillimeter Array. The disk shows a Keplerian rotation pattern with an inclination of ~11°, based on the spatially and spectrally resolved <SUP>12</SUP>CO and <SUP>13</SUP>CO emission. The data show clear evidence for both dust and gas surface density reductions in the inner region of the disk (radius <img entity='lsim' SRC='http://ej.iop.org/icons/Entities/lsim.gif' ALT='lsim' ALIGN='BASELINE' /> 50 AU) from the continuum and <SUP>13</SUP>CO J = 2-1 data, respectively. The presence of this inner cavity in both the dust and gas is more consistent with clearing by giant planet formation than by photoevaporation or by grain growth. There is also an indication of global CO gas depletion in the disk, as the mass estimated from <SUP>13</SUP>CO emission (~3.8 × 10<SUP>–4</SUP> M<SUB>☉</SUB>) is about two orders of magnitude lower than that derived from the 1.3 mm continuum (~2.8 × 10<SUP>–2</SUP> M<SUB>☉</SUB>).</P>
MILKY WAY SUPERMASSIVE BLACK HOLE: DYNAMICAL FEEDING FROM THE CIRCUMNUCLEAR ENVIRONMENT
Liu, Hauyu Baobab,Hsieh, Pei-Ying,Ho, Paul T. P.,Su, Yu-Nung,Wright, Melvyn,Sun, Ai-Lei,Minh, Young Chol IOP Publishing 2012 The Astrophysical journal Vol.756 No.2
<P>The supermassive black hole (SMBH), Sgr A*, at the Galactic center is surrounded by a molecular circumnuclear disk (CND) lying between 1.5 and 4 pc radii. The irregular and clumpy structures of the CND suggest dynamical evolution and episodic feeding of gas toward the central SMBH. New sensitive data from the Submillimeter Array and Green Bank Telescope reveal several >5-10 pc scale molecular arms, which either directly connect to the CND or may penetrate inside the CND. The CND appears to be the convergence of the innermost parts of large-scale gas streamers, which are responding to the central gravitational potential well. Rather than being a quasi-stationary structure, the CND may be dynamically evolving, incorporating inflow via streamers, and feeding gas toward the center.</P>