• KSII Transactions on Internet and Information Systems (TIIS)
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• v.11 no.2
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• pp.628-649
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• 2017

Security and resource-saving are both demands of the fifth generation (5G) wireless networks. In this paper, we study the secrecy spectrum efficiency (SSE) and secrecy energy efficiency (SEE) of a K-tier massive multiple-input multiple-output (MIMO) enabled heterogeneous cellular network (HetNet), in which artificial noise (AN) are employed for secrecy enhancement. Assuming (i) independent Poisson point process model for the locations of base stations (BSs) of each tier as well as that of eavesdroppers, (ii) zero-forcing precoding at the macrocell BSs (MBSs), and (iii) maximum average received power-based cell selection, the tractable lower bound expressions for SSE and SEE of massive MIMO enabled HetNets are derived. Then, the influences on secrecy oriented spectrum and energy efficiency performance caused by the power allocation for AN, transmit antenna number, number of users served by each MBS, and eavesdropper density are analyzed respectively. Moreover, the analysis accuracy is verified by Monte Carlo simulations.

• KSII Transactions on Internet and Information Systems (TIIS)
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• v.14 no.10
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• pp.4214-4230
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• 2020

This paper introduces a pilot allocation scheme for massive MIMO systems based on deep convolutional neural network (CNN) learning. This work is an extension of a prior work on the basic deep learning framework of the pilot assignment problem, the application of which to a high-user density nature is difficult owing to the factorial increase in both input features and output layers. To solve this problem, by adopting the advantages of CNN in learning image data, we design input features that represent users' locations in all the cells as image data with a two-dimensional fixed-size matrix. Furthermore, using a sorting mechanism for applying proper rule, we construct output layers with a linear space complexity according to the number of users. We also develop a theoretical framework for the network capacity model of the massive MIMO systems and apply it to the training process. Finally, we implement the proposed deep CNN-based pilot assignment scheme using a commercial vanilla CNN, which takes into account shift invariant characteristics. Through extensive simulation, we demonstrate that the proposed work realizes about a 98% theoretical upper-bound performance and an elapsed time of 0.842 ms with low complexity in the case of a high-user-density condition.

• Clinics in Shoulder and Elbow
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• v.19 no.2
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• pp.84-89
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• 2016

Background: The purpose of this study was to assess the results of arthroscopic bridging repair using a human dermis allograft in the treatment of massive irreparable rotator cuff tears. Methods: From November 2009 to April 2011, 12 patients underwent arthroscopic bridging repair using a human dermis allograft in the treatment of massive irreparable rotator cuff tears. Patients were followed for an average of 33.9 months. Clinical outcome was evaluated preoperatively and postoperatively using the mean University of California, Los Angeles (UCLA) score and the Korean Shoulder Scoring System (KSS). Magnetic resonance imaging (MRI) was performed postoperatively at an average of 6.5 months. Results: At a mean follow-up of 33.9 months (range, 25 to 42 months), 11 out of 12 patients were satisfied with their procedure. Patients showed significant improvement in their mean modified UCLA score from 15.9 preoperatively to 29.4 postoperatively (p=0.001). The mean KSS score improved from 45.6 preoperatively to 80.5 postoperatively (p=0.002). In MRI studies, 9 out of 12 patients had full incorporation of the graft into the native rotator cuff remnant. To date, there has been no intraoperative or postoperative complication from the graft procedure, such as infection or allograft rejection, in any patient. Conclusions: Arthroscopic bridging repair using a human dermis allograft can be considered as an option in treatment of select cases of massive irreparable rotator cuff tears, resulting in high patient satisfaction.

• Tuberculosis and Respiratory Diseases
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• v.76 no.3
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• pp.127-130
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• 2014

The risk of dying from a pulmonary embolism (PE) is estimated to be about 30% if inotropic support is required and no cardiopulmonary arrest occurs. Fibrinolysis in massive PE is regarded as a life-saving intervention, unless there is a high risk of bleeding following the use of the fibrinolytic therapy. Rivaroxaban is an oral factor Xa inhibitor, however its anticoagulation effects before or after administration of fibrinolytics in massive PE are still unknown. Two patents were admitted: 61-year-old woman with repeated syncope, and a 73-year-old woman was admitted with dyspnea and poor oral intake. Systemic arterial hypotension with radiologic confirmation led to a diagnosis of massive PE in both patients. Rivaroxaban was administered before in one, and after firbrinolytic therapy in the other. One showed similar efficacy of rivaroxaban with currently used anticoagulants after successful fibrinolysis, and the other one without antecedent administration of the fibrinolytic agent showed unfavorable efficacy of rivaroxaban.

• Solar Energy
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• v.11 no.2
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• pp.3-8
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• 1991

This paper reports the application of the PSTAR(Primary and Secondary Terms Analysis and Henormalization) method to a thermally massive passive solar house located in Daejeon, Korea. The house has approximately $156m^2$ of living area with 3 bedrooms and a living room, which embodies many passive solar features for energy conservation. The primary concern of this work was to properly evaluate the thermal behavior of a thermally massive building structure using the PSTAR method. Results show close agreements between the measured and renormalized values in most cases in which the simulation results from the audit description of the house deviate somewhat considerably.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.1
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• pp.42.1-42.1
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• 2013

In the LCDM paradigm, hierarchical merging is thought to play a key role in the formation and evolution of massive galaxies. Theoretical and observational studies suggest that massive galaxies started forming at high redshifts and were assembled via numerous mergers. Galaxy clusters are the sites where the most massive galaxies are found and the most dramatic merger histories are embedded. The previous work of Sheen et al. (2012) identified via visual inspection many massive galaxies with merger features in clusters, which surprised the community. In this study we aim to quantify peculiarity of galaxies to pin down the merger frequency in cluster environments more objectively. We have performed optical deep imaging of 4 Abell clusters by using IMACS f/2 on a Magellan Badde 6.5-m telescope. For the galaxies in our data, we applied GALFIT algorithm, which fits analytic models to galaxy data, and we analyzed their residuals. We present the preliminary results of our sample galaxies.

• The Bulletin of The Korean Astronomical Society
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• v.38 no.1
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• pp.50.2-50.2
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• 2013

In the process of star formation, the density and temperature of associated material, which are the physical conditions for the molecular chemistry, vary dramatically. As a result, the connection between physical and chemical conditions has been used to trace the evolutionary stages in star formation. One chemical tracer for the physical conditions in star forming material is the [HCN]/[HNC] abundance ratio since the ratio strongly depends on the kinetic temperature in molecular clouds. Here we investigate the [HCN]/[HNC] abundance ratios in objects related to the massive star formation. For the investigation, we carried out $H^{13}CN$ and $HN^{13}C$ line observation toward objects in three different evolutionary stages of massive star formation: Infrared dark clouds (IRDCs), High-mass protostellar object (HMPOs), and Ultra-compact HII regions (UCHIIs). According to our observational results, both $H^{13}CN$ and $HN^{13}C$ lines have been detected toward 19 IRDCs, 25 HMPOs, and 31 UCHIIs. We will discuss about the [HCN]/[HNC] abundance ratios in different evolutionary stages of massive star formation and associate the results with the physical conditions of the targets.

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.93-97
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• 2015

How high-mass stars form is currently unclear. Calculations suggest that the radiation pressure of a forming star can halt spherical infall, preventing further growth when it reaches $10M_{\odot}$. Two major theoretical models on the further growth of stellar mass have been proposed. One model suggests the merging of less massive stellar objects, and the other is through accretion, but with the help of a disk. Inflow motions are key evidence for how forming stars gain further mass to build up massive stars. Recent developments in technology have boosted the search for inflow motion. A number of high-mass collapse candidates were obtained with single dish observations, and mostly showed blue profiles. Infalling signatures seem to be more common in regions which have developed radiation pressure than in younger cores, which is the opposite of the theoretical prediction and is also very different from observations of low mass star formation. Interferometer studies so far confirm this tendency with more obvious blue profiles or inverse P Cygni profiles. Results seem to favor the accretion model. However, the evolution of the infall motion in massive star forming cores needs to be further explored. Direct evidence for monolithic or competitive collapse processes is still lacking. ALMA will enable us to probe more detail of the gravitional processes.

• Tuberculosis and Respiratory Diseases
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• v.78 no.2
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• pp.106-111
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• 2015

Tracheal hemangioma is a rare benign vascular tumor in adults. We reported a case of massive hemoptysis caused by a cavernous hemangioma in a 75-year-old man. This is the first report, to our knowledge, of a tracheal cavernous hemangioma that presented with massive hemoptysis. The lesion was removed with a $CO_2$ laser under rigid laryngoscopy. Endovascular tumors, such as tracheobronchial hemangiomas, should be considered a diagnostic option in cases of massive hemoptysis without a significant underlying lung lesion.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.2
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• pp.59.4-60
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• 2018

Ultra-diffuse galaxies (UDGs) are an unusual galaxy population. They are ghostlike galaxies with fainter surface brightness than normal dwarf galaxies, but they are as large as MW-like galaxies. The key question on UDGs is whether they are 'failed' giant galaxies or 'extended' dwarf galaxies. To answer this question, we study UDGs in massive galaxy clusters. We find an amount of UDGs in deep HST images of three Hubble Frontier Fields clusters, Abell 2744 (z=0.308), Abell S1063 (z=0.347), and Abell 370 (z=0.374). These clusters are the farthest and most massive galaxy clusters in which UDGs have been discovered until now. The color-magnitude relations show that most UDGs have old stellar population with red colors, while a few of them show bluer colors implying the existence of young stars. The stellar masses of UDGs show that they have less massive stellar components than the bright red sequence galaxies. The radial number density profiles of UDGs exhibit a drop in the central region of clusters, suggesting some of them were disrupted by strong gravitational potential. Their spatial distributions are not homogeneous, which implies UDGs are not virialized enough in the clusters. With virial masses of UDGs estimated from the fundamental manifold, most UDGs have M_200 = 10^10 - 10^11 M_Sun indicating that they are dwarf galaxies. However, a few of UDGs more massive than 10^11 M_Sun indicate that they are close to failed giant galaxies.