检索结果-内蒙古大学图书馆

Using the base semantics given by fUML for verification

学校读者我要写书评

暂无评论

Using the base semantics given by fUML for verification

International Conference on Model-Driven Engineering and Software Development (MODELSWARD)

作者： Alessandro Gerlinger Romero Klaus Schneider Maurício Gonçalves Vieira Ferreira Satellite Tracking and Control Center Brazilian National Institute for Space Research São José dos Campos Brazil Department of Computer Science University of Kaiserslautern Kaiserslautern Germany

ISBN: (纸本)9781479941643

The lack of formal foundations of UML results in imprecise models since UML only defines graphical notations, but not their formal semantics. However, in safety-critical applications, formal semantics is a requirement for verification. Semantics for the key parts of activities and classes of UML is defined by the semantics of a foundational subset for executable UML models (fUML). Moreover, the base semantics given by fUML defines the formal semantics of UML. In this paper, we evaluate a subset of the base semantics given by fUML covering its formal definition and its use for verification. From the practical perspective, we show with a simple example how the base semantics can support formal verification through theorem proving. The initial results show that the base semantics, when mature, can play an important role in the formal verification of UML models.

关键词： Semantics Unified modeling language Syntactics Abstracts Object oriented modeling Communities Computational modeling

BPM Model of GQIMP for ISO 9001:2008 Supported by CASE Tools

学校读者我要写书评

暂无评论

BPM Model of GQIMP for ISO 9001:2008 Supported by CASE Tools

International Conference on Information Technology: New Generations (ITNG)

作者： Denis Avila Montini Gustavo Ravanhani Matuck Adilson Marques da Cunha Luiz Alberto Vieira Dias Massimo Jorge Isaac Computer Science Division Brazilian Aeronautics Institute of Technology (ITA) Sao Jose dos Campos SP Brazil Faculdade de Engenharia Mecanica FEM da Universidade de Campinas

ISBN: (纸本)9781479931897

This paper describes a methodology which combines Goals, Questions, Indicators, Measures and Procedures (GQIMP), aimed at the implementation of ISO9001, to structure the operation of a Service Center, in a context of Business Process Modeling (BPM). The methodology GQIMP was structured based on BPM approach. In this case, the BPM modeling was used to define the scope of Service Centers. The GQIMP methodology is a form of integration that uses a heuristic process of Causal Analysis and Resolution (CAR). In this context, a CAR was used to identify the necessary components to enable BPM Service Centers. The conceived model was systematized by means of a CASE tool which allowed the integration of Quality Management System (QMS) in an integrated way into a ISO 9001:2008 real case. The results through the selection of this strategy presents is lean and concise, for obtaining ISO certification. In this context, this model is driven by process indicators that support a CASE tools instrumentalization.

关键词： ISO standards computer aided software engineering Context Certification Business Measurement Software

Dynamic load balancing in GPU-based systems for a MPI program

学校读者我要写书评

暂无评论

Dynamic load balancing in GPU-based systems for a MPI progra...

International Conference on High Performance Computing & Simulation (HPCS)

作者： Alvaro Luiz Fazenda auCelso L. Mendes Laxmikant V. Kale Jairo Panetta Eduardo Rocha Rodrigues Institute of Science and Technology Federal University of Sao Paulo (UNIFESP) São José dos Campos SP Brazil National Center for Supercomputing Application University of Illinois at Urbana-Champaign Urbana IL USA Department of Computer Science University of Illinois at Urbana-Champaign Urbana IL USA Computer Science Department Aeronautics Institute of Technology (ITA) São José dos Campos SP Brazil IBM Research Brazil Rio de Janeiro RJ Brazil

The dynamic load-balancing framework Charm++/AMPI, developed at the University of Illinois, is based on processor virtualization to allow thread migration across processors. This framework has been successfully applied to many scientific applications in the past, such as BRAMS, NAMD, ChaNGa, and others. Most of these applications use only CPUs, that is, they do not use accelerators. However, the use of GPUs to improve computational performance is quickly getting massively disseminated in the high-performance computing community. This paper aims to investigate how the same Charm++/AMPI framework can be extended to balance load in a synthetic application inspired by the BRAMS numerical forecast model, running on GPUs instead of CPUs. Many major questions involving the use of GPUs with AMPI where handled in this work, including: how to measure the GPU's load, how to use and share GPUs among user-level threads, and what results are obtained when applying the required over-decomposition technique to a GPU-accelerated program.

关键词： Graphics processing units Kernel Load modeling Physics Instruction sets Scalability Jacobian matrices

Astrometric calibration and performance of the Dark Energy Camera

学校读者我要写书评

暂无评论

arXiv 2017年

作者： Bernstein, G.M. Armstrong, R. Plazas, A.A. Walker, A.R. Abbott, T.M.C. Allam, S. Bechtol, K. Benoit-Lévy, A. Brooks, D. Burke, D.L. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Cunha, C.E. da Costa, L.N. DePoy, D.L. Desai, S. Diehl, H.T. Eifler, T.F. Fernandez, E. Fosalba, P. Frieman, J. García-Bellido, J. Gerdes, D.W. Gruen, D. Gruendl, R.A. Gschwend, J. Gutierrez, G. Honscheid, K. James, D.J. Kent, S. Krause, E. Kuehn, K. Kuropatkin, N. Li, T.S. Maia, M.A.G. March, M. Marshall, J.L. Menanteau, F. Miquel, R. Ogando, R.L.C. Reil, K. Roodman, A. Rykoff, E.S. Sanchez, E. Scarpine, V. Schindler, R. Schubnell, M. Sevilla-Noarbe, I. Smith, M. Smith, R.C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M.E.C. Tarle, G. Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Astrophysical Sciences Princeton University Peyton Hall PrincetonNJ08544 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Dr. PasadenaCA91109 United States Cerro Tololo Inter-American Observatory National Optical Astronomy Observatory Casilla 603 La Serena Chile Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States LSST 933 North Cherry Avenue TucsonAZ85721 United States CNRS UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Observatório Nacional Rua Gal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Department of Astronomy University of Illinois 1002 W. Green Street UrbanaIL61801 United States National Center for Supercomputing Applications 1205 West Clark St. UrbanaIL61801 United States Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Department of Physics and Astronomy Texas A&M University College StationTX77843 United States Department of Physics IIT Hyderabad KandiTelangana502285 India Institut de Ciències de l’Espai IEEC-CSIC Campus UAB Carrer de Can Magrans s/n Bellaterra Barcelona08193 Spain Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States I

We characterize the ability of the Dark Energy Camera (DECam) to perform relative astrometry across its 500 Mpix, 3-deg2 science field of view, and across 4 years of operation. This is done using internal comparisons of ∼ 4 × 107 measurements of highS/N stellar images obtained in repeat visits to fields of moderate stellar density, with the telescope dithered to move the sources around the array. An empirical astrometric model includes terms for: optical distortions;stray electric fields in the CCD detectors;chromatic terms in the instrumental and atmospheric optics;shifts in CCD relative positions of up to ≈ 10 µm when the DECam temperature cycles;and low-order distortions to each exposure from changes in atmospheric refraction and telescope alignment. Errors in this astrometric model are dominated by stochastic variations with typical amplitudes of 10–30 mas (in a 30 s exposure) and 50–100 coherence length, plausibly attributed to Kolmogorov-spectrum atmospheric turbulence. The size of these atmospheric distortions is not closely related to the seeing. Given an astrometric reference catalog at density ≈ 0.7 arcmin−2, e.g. from Gaia, the typical atmospheric distortions can be interpolated to ≈ 7 mas RMS accuracy (for 30 s exposures) with 10 coherence length in for residual errors. Remaining detectable error contributors are 2–4 mas RMS from unmodelled stray electric fields in the devices, and another 2–4 mas RMS from focal plane shifts between camera thermal cycles. Thus the astrometric solution for a single DECam exposure is accurate to 3–6 mas (≈ 0.02 pixels, or ≈ 300 nm) on the focal plane, plus the stochastic atmospheric distortion. Copyright © 2017, The Authors. All rights reserved.

关键词： Atmospheric turbulence

An r-process enhanced star in the dwarf galaxy Tucana III

学校读者我要写书评

暂无评论

arXiv 2017年

作者： Hansen, T.T. Simon, J.D. Marshall, J.L. Li, T.S. Carollo, D. DePoy, D.L. Nagasawa, D.Q. Bernstein, R.A. Drlica-Wagner, A. Abdalla, F.B. Allam, S. Annis, J. Bechtol, K. Benoit-Lévy, A. Brooks, D. Buckley-Geer, E. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Cunha, C.E. da Costa, L.N. Desai, S. Eifler, T.F. Fausti Neto, A. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Gerdes, D.W. Gruen, D. Gruendl, R.A. Gschwend, J. Gutierrez, G. James, D.J. Krause, E. Kuehn, K. Kuropatkin, N. Lahav, O. Miquel, R. Plazas, A.A. Romer, A.K. Sanchez, E. Santiago, B. Scarpine, V. Smith, R.C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M.E.C. Tarle, G. Walker, A.R. Observatories of the Carnegie Institution of Washington 813 Santa Barbara St. PasadenaCA91101 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Department of Physics and Astronomy Texas A&M University College StationTX77843 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States INAF- Osservatorio Astronomico di Torino - Strada Osservatorio 20 Pino Torinese10020 Italy Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Physics and Electronics Rhodes University PO Box 94 Grahamstown6140 South Africa LSST 933 North Cherry Avenue TucsonAZ85721 United States CNRS UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Observatório Nacional Rua Gal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Department of Astronomy University of Illinois 1002 W. Green Street UrbanaIL61801 United States National Center for Supercomputing Applications 1205 West Clark St. UrbanaIL61801 United States Institut de Ciències de l’Espai IEEC-CSIC Campus UAB Carrer de Can Magrans s/n Bellaterra Barcelona08193 Spain Barcelona Institute of Science and Technology Campus UAB Bellaterra [Barcelona08193 Spain Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Department of Physics IIT Hyderabad KandiTelangana502285 India Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Dr. PasadenaCA91109 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Instituto de Fisica Teorica UAM/CSIC Universidad Autonoma de Madrid Madrid28049 Sp

Chemically peculiar stars in dwarf galaxies provide a window for exploring the birth environment of stars with varying chemical enrichment. We present a chemical abundance analysis of the brightest star in the newly discovered ultra-faint dwarf galaxy candidate Tucana III. Because it is particularly bright for a star in an ultra-faint Milky Way satellite, we are able to measure the abundance of 28 elements, including 13 neutron-capture species. This star, DES J235532.66−593114.9 (DES J235532), shows a mild enhancement in neutron-capture elements associated with the r-process and can be classified as an r-I star. DES J235532 is the first r-I star to be discovered in an ultra-faint satellite, and Tuc III is the second extremely low-luminosity system found to contain r-process enriched material, after Reticulum II. Comparison of the abundance pattern of DES J235532 with r-I and r-II stars found in other dwarf galaxies and in the Milky Way halo suggests a common astrophysical origin for the neutron-capture elements seen in all r-process enhanced stars. We explore both internal and external scenarios for the r-process enrichment of Tuc III and show that with abundance patterns for additional stars it should be possible to distinguish between them. Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

Discovery and physical characterization of a large scattered disk object at 92 AU

学校读者我要写书评

暂无评论

arXiv 2017年

作者： Gerdes, D.W. Sako, M. Hamilton, S. Zhang, K. Khain, T. Becker, J.C. Annis, J. Wester, W. Bernstein, G.M. Scheibner, C. Zullo, L. Adams, F. Bergin, E. Walker, A.R. Mueller, J.H. Abbott, T.M.C. Abdalla, F.B. Allam, S. Bechtol, K. Benoit-Lévy, A. Bertin, E. Brooks, D. Burke, D.L. Carnero Rosell, A. Carrasco Kind, M. Carretero, J. Cunha, C.E. da Costa, L.N. Desai, S. Diehl, H.T. Eifler, T.F. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Goldstein, D.A. Gruen, D. Gschwend, J. Gutierrez, G. Honscheid, K. James, D.J. Kent, S. Krause, E. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T.S. Maia, M.A.G. March, M. Marshall, J.L. Martini, P. Menanteau, F. Miquel, R. Nichol, R.C. Plazas, A.A. Romer, A.K. Roodman, A. Sanchez, E. Sevilla-Noarbe, I. Smith, M. Smith, R.C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M.E.C. Tarle, G. Tucker, D.L. Zhang, Y. Department of Physics University of Michigan Ann ArborMI48109 United States Department of Astronomy University of Michigan Ann ArborMI48109 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Physics St. Olaf Collage NorthfieldMN55057 United States Cerro Tololo Inter-American Observatory National Optical Astronomy Observatory Casilla 603 La Serena Chile Illinois Mathematics and Science Academy 1500 Sullivan Rd. AuroraIL60506-1000 United States Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Physics and Electronics Rhodes University PO Box 94 Grahamstown6140 South Africa LSST 933 North Cherry Avenue TucsonAZ85721 United States CNRS UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Observatório Nacional Rua Gal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Department of Astronomy University of Illinois 1002 W. Green Street UrbanaIL61801 United States National Center for Supercomputing Applications 1205 West Clark St. UrbanaIL61801 United States Barcelona Institute of Science and Technology Campus UAB Bellaterra [Barcelona08193 Spain Department of Physics IIT Hyderabad KandiTelangana502285 India Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Dr. PasadenaCA91109 United States Kavli Institute for Cosmological Physics University of Chicago Chicago

We report the observation and physical characterization of the possible dwarf planet 2014 UZ224 ("DeeDee"), a dynamically detached trans-Neptunian object discovered at 92 AU. This object is currently the second-most distant known trans-Neptunian object with reported orbital elements, surpassed in distance only by the dwarf planet Eris. The object was discovered with an r-band magnitude of 23.0 in data collected by the Dark Energy Survey between 2014 and 2016. Its 1140-year orbit has (a,e,i) = (109 AU,0.65,26.8◦). It will reach its perihelion distance of 38 AU in the year 2142. Integrations of its orbit show it to be dynamically stable on Gyr timescales, with only weak interactions with Neptune. We have performed followup observations with ALMA, using 3 hours of on-source integration time to measure the object’s thermal emission in the Rayleigh-Jeans tail. The signal is detected at 7σ significance, from which we determine a V-band albedo of 13.1+3.3−2.4(stat)+2.0−1.4(sys) percent and a diameter of 635+57−61(stat)+32−39(sys) km, assuming a spherical body with uniform surface properties. Copyright © 2017, The Authors. All rights reserved.

关键词： Orbits

EPC information services with No-SQL datastore for the Internet of Things

学校读者我要写书评

暂无评论

EPC information services with No-SQL datastore for the Inter...

IEEE International Conference on RFID

作者： Tuan Dinh Le Seong Hoon Kim Minh Hoang Nguyen Daeyoung Kim Seung Young Shin Kyung Eun Lee Rodrigo da Rosa Righi Deparment of Computer Science KAIST Daejeon South Korea Samsung Electronics South Korea Graduate Program in Applied Computing Universidade do Vale do Rio dos Sinos São Leopoldo Brazil

With the emergence of the Internet of Things (IoT) vision, RFID technology has attracted more and more interests from many industries. In the EPCglobal standard which standardizes RFID architectural framework and interfaces, the Electronic Product Code Information System (EPCIS) - the repository in the RFID network - plays a pivotal role in storing dynamic and historical RFID trajectory data, well-tailored to supply chain applications. However, in the IoT era, EPCIS should be capable of storing a large amount of realtime and continuous time-series RFID data in a scalable manner. Therefore, in this paper, we analyze the requirements and current design of EPCIS and report current limitations of SQL-based approaches for IoT applications. To cope with these limitations, we explore a NoSQL-based approach for EPCIS in the IoT and propose a column-family-based data model and customization for Cassandra-based EPCIS. Using real-world implementation, we also conduct a performance comparison between MySQL and Cassandra in different deployment scenarios (i.e., physical and virtual machines). As a result, we show the benefits of using Cassandra datastore for EPCIS in the IoT in terms of response time, throughput, and flexibility.

关键词： Radiofrequency identification Data models Indexes Relational databases Standards Containers

A Chi-Square Methodology Applied in Deviations Control of Project Plan to Support the RIMAM Model

学校读者我要写书评

暂无评论

A Chi-Square Methodology Applied in Deviations Control of Pr...

International Conference on Information Technology: New Generations (ITNG)

作者： Denis Avila Montini Danilo Battaglia Gustavo Ravanhani Matuck Adilson Marques da Cunha Luiz Alberto Vieira Dias Alessandra Avila Montini Basit Shahzad Computer Science Division Brazilian Aeronautics Institute of Technology (ITA) Sao Jose dos Campos SP Brazil University of Sao Paulo (USP) Sao Paulo SP Brazil King Saud Universiy Saudi Arabia

ISBN: (纸本)9781479931897

This paper describes a Hybrid Chi-Squared methodology of Project Plan deviations identification, including those for multiple deviations in a Project Plan system. The sampling methodology was used to analyze similarity, together with a statistical optimization methodology for Chi-Squared, to improve the existing methodology used to forecast data in the Project Plan phase. The created sampling methodology was utilized for learning activities of Project Plan, in order to detect deviations. This Chi-Squared methodology was employed by empirical results. The results have shown that the selection strategy identify better forecasting approach between two different proposals, aiming to provide the forecasting process of Project Plan, presenting better precisions based on the diagnose deviations detection, within this Chi-Squared methodology.

关键词： Planning Software Production Algorithm design and analysis Software algorithms Monitoring Standards

A multi-component matched filter cluster confirmation tool for eROSITA: Initial application to the RASS and DES-SV datasets

学校读者我要写书评

暂无评论

arXiv 2017年

作者： Klein, M. Mohr, J.J. Desai, S. Israel, H. Allam, S. Benoit-Levy, A. Brooks, D. Buckley-Geer, E. Rosel, A. Carnero Kind, M. Carrasco Cunha, C.E. da Costa, L.N. Dietrich, J.P. Eier, T.F. Evrard, A.E. Frieman, J. Gruen, D. Gruendl, R.A. Gutierrez, G. Honscheid, K. James, D.J. Kuehn, K. Lima, M. Maia, M.A.G. March, M. Melchior, P. Menanteau, F. Miquel, R. Plazas, A.A. Reil, K. Romer, A.K. Sanchez, E. Santiago, B. Scarpine, V. Schubnell, M. Sevilla-Noarbe, I. Smith, M. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M.E.C. Tarle, G. Faculty of Physics Ludwig-Maximilians-Universitat Scheinerstr. 1 Munich81679 Germany Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse Garching85748 Germany Excellence Cluster Universe Boltzmannstr. 2 Garching85748 Germany Department of Physics IIT Hyderabad Kandi Telangana502285 India Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States CNRS UMR 7095 Institut d'Astrophysique de Paris ParisF-75014 France Department of Physics & Astronomy University College London Gower Street LondonWC1E6BT United Kingdom Sorbonne Universites UPMC Univ Paris 06 UMR 7095 Institut d'Astrophysique de Paris ParisF-75014 France Laboratorio Interinstitucional de e-Astronomia-LIneA Rua Gal. Jose Cristino 77 Rio de Janeiro RJ20921-400 Brazil Observatorio Nacional Rua Gal. Jose Cristino 77 Rio de Janeiro RJ20921-400 Brazil Department of Astronomy University of Illinois 1002 W. Green Street UrbanaIL61801 United States National Center for Supercomputing Applications 1205 West Clark St. UrbanaIL61801 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Dr. PasadenaCA91109 United States Department of Astronomy University of Michigan Ann ArborMI48109 United States Department of Physics University of Michigan Ann ArborMI48109 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Department of Physics Ohio State University ColumbusOH43210 United States Astronomy Department University of Washington Box 351580 SeattleWA98195 United States Cerro Tololo Inter-American Observatory National Optical Astronomy Observatory Casilla 6

We describe a multi-component matched filter cluster confirmation tool (MCMF) designed for the study of large X-ray source catalogs produced by the upcoming X-ray all-sky survey mission eROSITA. We apply the method to... 详细信息

关键词： Galaxies