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37th International Cosmic Ray conference, ICRC 2021

作者： vuillaume, Thomas Jacquemont, Mikaël de Bony de Lavergne, Mathieu Sanchez, David A. Poireau, vincent Maurin, Gilles Benoit, Alexandre Lambert, Patrick Lamanna, Giovanni Abe, H. Aguasca, A. Agudo, I. Antonelli, L.A. Aramo, C. Armstrong, T. Artero, M. Asano, K. Ashkar, H. Aubert, P. Baktash, A. Bamba, A. Baquero Larriva, A. Baroncelli, L. Barres de Almeida, U. Barrio, J.A. Batkovic, I. Becerra González, J. Bernardos, M.I. Berti, A. Biederbeck, N. Bigongiari, C. Blanch, O. Bonnoli, G. Bordas, P. Bose, D. Bulgarelli, A. Burelli, I. Buscemi, M. Cardillo, M. Caroff, S. Carosi, A. Cassol, F. Cerruti, M. Chai, Y. Cheng, K. Chikawa, M. Chytka, L. Contreras, J.L. Cortina, J. Costantini, H. Dalchenko, M. De Angelis, A. Deleglise, G. Delgado, C. Delgado Mengual, J. della volpe, D. Depaoli, D. Di Pierro, F. Di venere, L. Díaz, C. Dominik, R.M. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsässer, D. Emery, G. Escudero, J. Fiasson, A. Foffano, L. Fonseca, M.v. Freixas Coromina, L. Fukami, S. Fukazawa, Y. Garcia, E. Garcia López, R. Giglietto, N. Giordano, F. Gliwny, P. Godinovic, N. Green, D. Grespan, P. Gunji, S. Hackfeld, J. Hadasch, D. Hahn, A. Hassan, T. Hayashi, K. Heckmann, L. Heller, M. Herrera Llorente, J. Hirotani, K. Hoffmann, D. Horns, D. Houles, J. Hrabovsky, M. Hrupec, D. Hui, D. Hütten, M. Inada, T. Inome, Y. Iori, M. Ishio, K. Iwamura, Y. Jimenez Martinez, I. Jouvin, L. Jurysek, J. Kagaya, M. Karas, v. Katagiri, H. Kataoka, J. Kerszberg, D. Kobayashi, Y. Kong, A. Kubo, H. Kushida, J. Lamastra, A. Le Flour, T. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Luque-Escamilla, P.L. Majumdar, P. Makariev, M. Mandat, D. Manganaro, M. Mannheim, K. Mariotti, M. Marquez, P. Marsella, G. Martí, J. Martinez, O. Martínez, G. Martínez, M. Marusevec, P. Mas, A. Mazin, D. Mestre Guillen, E. Micanovic, S. Miceli, D. Miener, T. Miranda, J.M. Miranda, L.D.M. Mirzoyan, R. Mizuno, T. Molina, E. Montaruli, T. Monteiro, I. Moralejo, A. Morcuende, D. Moretti, E. Laboratoire d'Annecy de Physique des Particules Univ. Grenoble Alpes Univ. Savoie Mont Blanc CNRS-IN2P3 LAPP 9 chemin de bellevue Annecy74940 France LISTIC Université Savoie Mont-Blanc Polytech Annecy-Chambéry 5 chemin de bellevue Annecy74940 France Institute for Cosmic Ray Research University of Tokyo Japan Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Spain Instituto de Astrofísica de Andalucía CSIC Spain INAF - Osservatorio Astronomico di Roma Italy INFN Sezione di Napoli Italy Aix Marseille Univ CNRS IN2P3 CPPM France The Barcelona Institute of Science and Technology Spain IRFU CEA Université Paris-Saclay France Universität Hamburg Institut für Experimentalphysik Germany Graduate School of Science University of Tokyo Japan EMFTEL department IPARCOS Universidad Complutense de Madrid Spain INAF - Osservatorio di Astrofisica e Scienza dello spazio di Bologna Italy Centro Brasileiro de Pesquisas Físicas Brazil INFN Sezione di Padova Università degli Studi di Padova Italy Instituto de Astrofísica de Canarias Departamento de Astrofísica Universidad de La Laguna Spain Max-Planck-Institut für Physik Germany Department of Physics TU Dortmund University Germany Saha Institute of Nuclear Physics India INFN Sezione di Trieste Università degli Studi di Udine Italy INFN Sezione di Catania Italy Italy University of Geneva Département de Physique Nucléaire et Corpusculaire Switzerland Palacky University Olomouc Faculty of Science Czech Republic CIEMAT Spain Port d'Informació Científica Spain INFN Sezione di Torino Italy Dipartimento di Fisica Universitá degli Studi di Torino Italy INFN Sezione di Bari Università di Bari Italy University of Rijeka Department of Physics Croatia Institute for Theoretical Physics and Astrophysics Universität Würzburg Germany Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Japan INFN Sezione di Bari Politecnico di Bari

The Cherenkov Telescope Array (CTA) is the future ground-based gamma-ray observatory and will be composed of two arrays of imaging atmospheric Cherenkov telescopes (IACTs) located in the Northern and Southern hemispheres respectively. The first CTA prototype telescope built on-site, the Large-Sized Telescope (LST-1), is under commissioning in La Palma and has already taken data on numerous known sources. IACTs detect the faint flash of Cherenkov light indirectly produced after a very energetic gamma-ray photon has interacted with the atmosphere and generated an atmospheric shower. reconstruction of the characteristics of the primary photons is usually done using a parameterization up to the third order of the light distribution of the images. In order to go beyond this classical method, new approaches are being developed using state-of-the-art methods based on convolutional neural networks (CNN) to reconstruct the properties of each event (incoming direction, energy and particle type) directly from the telescope images. While promising, these methods are notoriously difficult to apply to real data due to differences (such as different levels of night sky background) between Monte Carlo (MC) data used to train the network and real data. The GammaLearn project, based on these CNN approaches, has already shown an increase in sensitivity on MC simulations for LST-1 as well as a lower energy threshold. This work applies the GammaLearn network to real data acquired by LST-1 and compares the results to the classical approach that uses random forests trained on extracted image parameters. The improvements on the background rejection, event direction, and energy reconstruction are discussed in this contribution. © 2022 Sissa Medialab Srl. All rights reserved.

关键词： Telescopes

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Processing potential and analysis of aspects influencing the results of analyses performed by digital image correlation

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AIP conference Proceedings 2023年第1期2976卷

作者： Martin Hagara Miroslav Pástor Jozef Bocko Technical University of Košice Faculty of Mechanical Engineering Department of Applied Mechanics and Mechanical Engineering Letná 1/9 042 00 Košice Slovakia

Digital image correlation belongs to the group of the modern full-field optical methods designed for 2D or 3D (depending on the configuration of the camera system) analysis of displacement or strain fields. This paper describes the processing capabilities of the experimental data acquired by Dantec Dynamics digital image correlation systems. For this purpose, a program called MOSTRAN v.1.0 has been specially developed at the authors’ workplace, enabling the processing of results from both deformation and motion analyses. The possibilities of using the mentioned program are described in the paper by means of several practical applications. In addition, the paper highlights chosen aspects influencing the results of experimental analyses, such as the method of generating a random speckle pattern required for the observation and reconstruction of the analyzed object contour, illumination conditions ensured during realization of the measurements, parameters obtained by the calibration of the cameras as well as the analysis of the appropriate facet size and corresponding method with properly set level of contour/displacement smoothing.

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Improving PET sensitivity with a Compton algorithm

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Journal of Physics: conference Series 2017年第1期931卷

作者： v. Ilisie v. Giménez-Alventosa L. Moliner A. Aguilar E. Lamprou A. González F. Sánchez J.M. Benlloch Instituto de Instrumentación para Imagen Molecular (I3M) Centro Mixto CSIC - Universitat Politècnica de València Camino de Vera S/N.

Current PET detectors have a very low sensitivity, of the order of a few percent. One of the reasons is that Compton events are being rejected. In this work we aim to prove that Compton events are a very rich source of additional information that can play a crucial role in the image reconstruction process. With this additional data, the detector sensitivity will be substantially improved and thus, the applied dose on the patient can also be reduced. This could be a really breaking point for PET detector technology as one should be able to obtain better image quality with less patient radiation. By means of Compton cone matching (the Compton cones coming from the same event should be compatible) one should be able to better recognize matching events and discard randoms and even events that have previously suffered scattering within the patient's body.

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Leveraging the checkpoint-restart technique for optimizing CPU efficiency of ATLAS production applications on opportunistic platforms

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Journal of Physics: conference Series 2018年第3期1085卷

作者： D Cameron J Elmsheuser L Heinrich W Lavrijsen P Nilsson v Tsulaia M vogel on behalf of theATLAS Collaboration University of Oslo P.b. 1048 Blindern 0316 Oslo Norway Brookhaven National Laboratory PO Box 5000 Upton NY 11973 USA New York University 70 Washington Square South New York NY 10012 USA Lawrence Berkeley National Laboratory 1 Cyclotron Road Berkeley CA 94720 USA University of Wuppertal Gausstrasse 20 42119 Wuppertal Germany

data processing applications of the ATLAS experiment, such as event simulation and reconstruction, spend considerable amount of time in the initialization phase. This phase includes loading a large number of shared libraries, reading detector geometry and condition data from external databases, building a transient representation of the detector geometry and initializing various algorithms and services. In some cases the initialization step can take as long as 10-15 minutes. Such slow initialization has a significant negative impact on overall CPU efficiency of the production job, especially when the job is executed on opportunistic, often short-lived, resources such as commercial clouds or volunteer computing. In order to improve this situation, we can take advantage of the fact that ATLAS runs large numbers of production jobs with similar configuration parameters (e.g. jobs within the same production task). This allows us to checkpoint one job at the end of its configuration step and then use the generated checkpoint image for rapid startup of thousands of production jobs. By applying this technique we can bring the initialization time of a job from tens of minutes down to just a few seconds. In addition to that we can leverage container technology for restarting checkpointed applications on the variety of computing platforms, in particular of platforms different from the one on which the checkpoint image was created. We will describe the mechanism of creating checkpoint images of Geant4 simulation jobs with AthenaMP (the multi-process version of the ATLAS data simulation, reconstruction and analysis framework Athena) and the usage of these images for running ATLAS Simulation production jobs on volunteer computing resources (ATLAS@Home) and on Supercomputers.

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MATISSE status report and science forecast 4

MATISSE status report and science forecast

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conference on Optical and Infrared Interferometry Iv

作者： Lopez, B. Lagarde, S. Jaffe, W. Petrov, R. Schoeller, M. Antonelli, P. Beckman, U. Berio, Ph. Bettonvil, F. Graser, U. Millour, F. Robbe-Dubois, S. venema, L. Wolf, S. Bristow, P. Glindemann, A. Gonzalez, J. -C. Lanz, Th. Henning, T. Weigelt, G. Agocs, T. Augereau, J. -C. Avila, G. Bailet, C. Behrend, J. Berger, J. -P. von Boekel, R. Bonhomme, S. Bourget, P. Brast, R. Bresson, Y. Clausse, J. M. Chesneau, O. Csepany, G. Connot, C. Crida, A. Danchy, W. C. Delbo, M. Delplancke, F. Dominik, C. Dugue, M. Elswijk, E. Fantei, Y. Finger, G. Gabasch, A. Girard, P. Girault, v. Gitton, P. Glazenborg, A. Gonte, F. Guitton, F. Guniat, S. De Haan, M. Haguenauer, P. Hanenburg, H. Heininger, M. Hofmann, K. -H. Hogerheijde, M. ter Horst, R. Hron, J. Hugues, Y. Ives, D. Jakob, G. Jasko, A. Jolley, P. Kragt, J. Koehler, R. Kroener, T. Kroes, G. Labadie, L. Laun, W. Lehmitz, M. Leinert, Ch. Lizon, J. L. Lucuix, Ch. Marcotto, A. Martinache, F. Matter, A. Martinot-Lagarde, G. Mauclert, N. Mehrgan, L. Meilland, A. Mellein, M. Menardi, S. Menut, J. L. Meisenheimer, K. Morel, S. Mosoni, L. Navarro, R. Neumann, U. Nussbaum, E. Ottogalli, S. Palsa, R. Panduro, J. Pantin, E. Percheron, I. Phan Duc, T. Pott, J. -U. Pozna, E. Przygodda, F. Richichi, A. Rigal, F. Rupprecht, G. Schertl, D. Stegmeier, J. Thiam, L. Tromp, N. vannier, M. vakili, F. van Belle, G. Wagner, K. Woillez, J. Univ Nice Sophia Antipolis UMR7293 Lab Lagrange CNRSObserv Cote dAzur F-06304 Nice France Max Planck Inst Astron D-69117 Heidelberg Germany Leiden Univ Leiden Observ NL-2300 RA Leiden Netherlands NOVA Opt IR Instrument Grp ASTRON NL-7990 AA Dwingeloo Netherlands Max Planck Inst Radioastron D-53121 Bonn Germany Univ Kiel Inst Theoret Phys & Astrophys D-24118 Kiel Germany Univ Vienna Inst Astrophys A-1180 Vienna Austria European So Observ D-85748 Garching Germany MTA Res Ctr Astron & Earth Sci Konkoly Thege Miklos Astron Inst H-1525 Budapest Hungary Univ Cologne Inst Phys 1 D-50937 Cologne Germany Univ Grenoble Alpes CNRS IPAG F-38000 Grenoble France Kernfys Versneller Inst NL-9747 AA Groningen Netherlands Univ Paris Diderot CNRS CEA DSM Lab AIMIRFUServ AstrophysCEA Saclay F-91191 Gif Sur Yvette France Deutsch Thomson OHG D-78048 Villingen Schweninger Germany Natl Astron Res Inst Thailand Chiang Mai 50200 Thailand Lowell Observ Flagstaff AZ 86001 USA NASA Goddard Space Flight Ctr Greenbelt MD 20771 USA

ISBN: (纸本)9780819496140

MATISSE is the mid-infrared spectrograph and imager for the very Large Telescope Interferometer (vLTI) at Paranal. This second generation interferometry instrument will open new avenues in the exploration of our Universe. Mid-infrared interferometry with MATISSE will allow significant advances in various fundamental research fields: studies of disks around young stellar objects where planets form and evolve, surface structures and mass loss of stars in late evolutionary stages, and the environments of black holes in active galactic nuclei. MATISSE is a unique instrument. As a first breakthrough it will enlarge the spectral domain used by optical interferometry by offering the L & M bands in addition to the N band, opening a wide wavelength domain, ranging from 2.8 to 13 mu m on angular scales of 3 mas (L/M band) / 10 mas (N band). As a second breakthrough, it will allow mid-infrared imaging - closure-phase aperture-synthesis imaging with up to four Unit Telescopes (UT) or Auxiliary Telescopes (AT) of the vLTI. MATISSE will offer various ranges of spectral resolution between R similar to 30 to similar to 5000. In this article, we present some of the main science objectives that have driven the instrument design. We introduce the physical concept of MATISSE including a description of the signal on the detectors and an evaluation of the expected performance and discuss the project status. The operations concept will be detailed in a more specific future article, illustrating the observing templates operating the instrument, the data reduction and analysis, and the image reconstruction software.

关键词： eInterferometry Spectroscopy Mid-Infrared vLTI

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High energy gamma ray emission from HESS J1809-193: Morphological and Spectral studies with HAWC 38

High energy gamma ray emission from HESS J1809-193: Morpholo...

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38th International Cosmic Ray conference, ICRC 2023

作者： Babu, Rishi Albert, A. Alfaro, R. Alvarez, C. Andrés, A. Arteaga-velázquez, J.C. Avila Rojas, D. Ayala Solares, H.A. Babu, R. Belmont-Moreno, E. Caballero-Mora, K.S. Capistrán, T. Yun-Cárcamo, S. Carramiñana, A. Carreón, F. Cotti, U. Cotzomi, J. Coutiño de León, S. De la Fuente, E. Depaoli, D. de León, C. Diaz Hernandez, R. Díaz-vélez, J.C. Dingus, B.L. Durocher, M. Duvernois, M.A. Engel, K. Espinoza, C. Fan, K.L. Fang, K. Fraija, N.I. García-González, J.A. Garfias, F. Goksu, H. González, M.M. Goodman, J.A. Groetsch, S. Harding, J.P. Hernandez, S. Herzog, I. Hinton, J. Huang, D. Hueyotl-Zahuantitla, F. Hüntemeyer, P. Iriarte, A. Joshi, v. Kaufmann, S. Kieda, D. Lara, A. Lee, J. Lee, W.H. León vargas, H. Linnemann, J. Longinotti, A.L. Luis-Raya, G. Malone, K. Martínez-Castro, J. Matthews, J.A.J. Miranda-Romagnoli, P. Montes, J. Morales-Soto, J.A. Mostafá, M. Nellen, L. Nisa, M.U. Noriega-Papaqui, R. Olivera-Nieto, L. Omodei, N. Pérez Araujo, Y. Pérez-Pérez, E.G. Pratts, A. Rho, C.D. Rosa-Gonzalez, D. Ruiz-velasco, E. Salazar, H. Salazar-Gallegos, D. Sandoval, A. Schneider, M. Schwefer, G. Serna-Franco, J. Smith, A.J. Son, Y. Springer, R.W. Tibolla, O. Tollefson, K. Torres, I. Torres-Escobedo, R. Turner, R. Ureña-Mena, F. varela, E. villaseñor, L. Wang, X. Watson, I.J. Werner, F. Whitaker, K. Willox, E. Wu, H. Zhou, H. Michigan Technological University 1400 Townsend Dr HoughtonMI United States Physics Division Los Alamos National Laboratory Los AlamosNM United States Instituto de Física Universidad Nacional Autónoma de México Ciudad de México Mexico Universidad Autónoma de Chiapas Chiapas Tuxtla Gutiérrez Mexico Instituto de Astronomía Universidad Nacional Autónoma de México Ciudad de México Mexico Instituto de Física y Matemáticas Universidad Michoacana de San Nicolás de Hidalgo Michoacán Morelia Mexico Department of Physics Pennsylvania State University University ParkPA United States Department of Physics Michigan Technological University HoughtonMI United States Department of Physics University of Maryland College ParkMD United States Instituto Nacional de Astrofísica Óptica y Electrónica Tonantzintla Puebla Mexico Department of Physics University of Wisconsin-Madison MadisonWI United States CUCEI CUCEA Universidad de Guadalajara Jalisco Guadalajara Mexico Max-Planck Institute for Nuclear Physics Heidelberg Germany Tecnologico de Monterrey Escuela de Ingeniería y Ciencias Ave. Eugenio Garza Sada 2501 N.L. Monterrey64849 Mexico Department of Physics and Astronomy Michigan State University East LansingMI United States Universidad Politécnica de Pachuca Hgo Pachuca Mexico Department of Physics and Astronomy University of Utah Salt Lake CityUT United States Instituto de Geofísica Universidad Nacional Autónoma de México Ciudad de México Mexico University of Seoul Seoul Korea Republic of Space Science and Applications Group Los Alamos National Laboratory Los AlamosNM United States Centro de Investigación en Computación Instituto Politécnico Nacional Ciudad de México Mexico Department of Physics and Astronomy University of New Mexico AlbuquerqueNM United States Universidad Autónoma del Estado de Hidalgo Hgo. Pachuca Mexico Instituto de Ciencias Nucleares Universidad Nacional Autónoma de México Ciudad de México Mexico Stanford University Stanfo

HESS J1809-193 is an unidentified Tev object, first detected by the High Energy Stereoscopic System (H.E.S.S.), located in a source-rich region with multiple source classes including SNR G11.1+0.1, SNR G11.0-0.0 and PSR J1809-1917. Initially classified as a pulsar wind nebula(PWN) candidate, however, recent studies show the presence of molecular clouds in the vicinity of the Tev source, indicating the evidence of a hadronic scenario for the observed very high-energy gamma rays. Marked as a potential Pevatron candidate, morphological and spectral studies for this region have been performed to better understand the nature of the particle acceleration mechanisms in the region. With 2090 days of data and new reconstruction algorithms, the High Altitude Water Cherenkov (HAWC) observatory is able to detect emission from this source above an energy of 100 Tev. In this report, we present the analysis of HESS J1809-193 with HAWC data and the multi-wavelength modeling of the region as well as potential sources of particle accceleration. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Stereo image processing

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The study of effectiveness of a high-performance crystal lattice parametric identification algorithm based on CUDA technology

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Journal of Physics: conference Series 2019年第5期1368卷

作者： Shirokanev, A S Kirsh, D v Kupriyanov, A v Samara National Research University Moskovskoe Shosse 34A Samara Russia 443086 Image Processing Systems Institute of RAS - Branch of the FSRC “Crystallography and Photonics” RAS Molodogvardejskaya street 151 Samara Russia 443001

The study of substances with a crystal structure is a complex multi-step process. The key step in the crystalline substance analysis is the unit cell parameter estimation. The estimation of the crystal lattice unit cell parameters is a particular problem that involves the search of the crystal lattice model’s parameters according to the information which can be extracted from the substance. In these recent times, the most accurate information about the substance structure can be obtained with the electron microscope whose linear resolution is high enough to observe the atomic structure of a substance. The problem of parameter estimation in this case means the reconstruction of the three-dimensional crystal lattice with 2-dimentional images received by an electron microscope, and the estimation of the crystal lattice unit cell parameters by reconstructed lattice. In the previous papers the crystal lattice parametric identification algorithms based on solving the local optimization problem were presented. However, the analysis of a large crystal lattice database requires a lot of computations. In this paper, a high-performance crystal lattices parametric identification algorithm using the CUDA technology is proposed. The investigation of the algorithm effectiveness is carried out on the GPU GeForce Nvidia GTX 1070 Ti. With data dimension more than 32 translations the acceleration is higher than 70. The algorithm runs more efficiently at the use of a large number of CUDA-blocks.

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