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arXiv 2023年

作者： Grattan, George Barton, Brandon A. Feeney, Sean Mossi, Gianni Patnaik, Pratik Sagal, Jacob C. Carr, Lincoln D. Oganesyan, Vadim Kapit, Eliot Quantum Engineering Program Colorado School of Mines 1523 Illinois St CO Golden80401 United States Department of Computer Science Colorado School of Mines 1500 Illinois St CO Golden80401 United States Department of Applied Mathematics and Statistics Colorado School of Mines 1500 Illinois St CO Golden80401 United States Department of Physics Colorado School of Mines 1523 Illinois St CO Golden80401 United States KBR Inc. 601 Jefferson St. HoustonTX77002 United States NASA Ames Research Center Moffett FieldCA94035 United States Department of Physics and Astronomy College of Staten Island CUNY Staten IslandNY10314 United States Physics program and Initiative for the Theoretical Sciences The Graduate Center CUNY New YorkNY10016 United States Center for Computational Quantum Physics Flatiron Institute 162 5th Avenue New YorkNY10010 United States

The exponential suppression of macroscopic quantum tunneling (MQT) in the number of elements to be reconfigured is an essential element of broken symmetry phases. Slow MQT is also a core bottleneck in quantum algorithms, such as traversing an energy landscape in optimization, and adiabatic state preparation more generally. In this work, we demonstrate the possibility to accelerate MQT through Floquet engineering with the application of a uniform, high frequency transverse drive field. Using the ferromagnetic phase of the transverse field Ising model in one and two dimensions as a prototypical example, we identify three qualitatively distinct regimes as a function of drive strength: (i) for weak drive, the system exhibits exponentially slow MQT alongside robust magnetic order, as expected;(ii) at intermediate drive strength, we find polynomial decay of rates alongside vanishing magnetic order consistent with critical or paramagnetic state;(iii) at very strong drive strengths both the tunnelling rate and time-averaged magnetic order remain finite with increasing system size. We support these claims with extensive full wavefunction and matrix-product state numerical simulations, and theoretical analysis. An experimental test of these results presents a technologically important and novel scientific question accessible on NISQ-era quantum computers. © 2023, CC BY.

关键词： Ising model

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Long term study of the blazar S5 0716+714: investigating a turbulent jet at all wavelengths 38

Long term study of the blazar S5 0716+714: investigating a t...

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38th International Cosmic Ray Conference, ICRC 2023

作者： Podobnik, F. Manganaro, M. Jormanainen, J. Lindfors, E. Bonnoli, G. Paoletti, R. Jorstad, S. Kiehlmann, S. Agudo, I. Elsasser, D. Lorey, C. Raiteri, C. Villata, M. Redhead, A.C. Marscher, A. Abe, H. Abe, S. Abhir, J. Acciari, V.A. Aniello, T. Ansoldi, S. Antonelli, L.A. Arbet Engels, A. Arcaro, C. Artero, M. Asano, K. Baack, D. Babić, A. Baquero, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Baxter, J. Becerra González, J. Bednarek, W. Bernardini, E. Bernardos, M. Bernete, J. Berti, A. Besenrieder, J. Bigongiari, C. Biland, A. Blanch, O. Bošnjak, Ž. Burelli, I. Busetto, G. Campoy-Ordaz, A. Carosi, A. Carosi, R. Carretero-Castrillo, M. Castro-Tirado, A.J. Ceribella, G. Chai, Y. Chilingarian, A. Cifuentes, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D’Amico, G. D’Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Del Popolo, A. Delfino, M. Delgado, J. Delgado Mendez, C. Depaoli, D. Di Pierro, F. Di Venere, L. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsaesser, D. Emery, G. Escudero, J. Fariña, L. Fattorini, A. Foffano, L. Font, L. Fröse, S. Fukami, S. Fukazawa, Y. García López, R.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giesbrecht Paiva, J.G. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Grau, R. Green, D. Green, J.G. Hadasch, D. Hahn, A. Hassan, T. Heckmann, L. Herrera, J. Hrupec, D. Hütten, M. Imazawa, R. Inada, T. Iotov, R. Ishio, K. Jiménez Martínez, I. Kerszberg, D. Kluge, G.W. Kobayashi, Y. Kouch, P.M. Kubo, H. Kushida, J. Láinez Lezáun, M. Lamastra, A. Lelas, D. Leone, F. Linhoff, L. Lombardi, S. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Lyard, E. Machado de Oliveira Fraga, B. Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Martínez-Chicharro, M. Mas-Aguilar, A. Mazin, D. Menchiari, S. Mender, S. Mićanović, S. Miceli, D. Miener, T. Miranda, J.M. Università di Siena INFN Pisa Via Roma 56 SienaI-53100 Italy Faculty of Physics University of Rijeka Radmile Matječić 2 Rijeka51000 Croatia Finnish MAGIC Group Finnish Centre for Astronomy with ESO University of Turku TurkuFI-20014 Finland RomeI-00136 Italy Institute of Astrophysics Foundation for Research and Technology-Hellas HeraklionGR-71110 Greece Instituto de Astrofisica de Andalucia-CSIC Glorieta de la Astronomía Granada18008 Spain Department of Physics Otto-Hahn-Str. 4a Dortmund44227 Germany Hans-Haffner-Sternwarte Naturwissenschaftliches Labor für Schüler am FKG Friedrich-Koenig-Gymnasium WürzburgD-97082 Germany INAF Osservatorio Astrofisico di Torino via Osservatorio 20 Pino TorineseI-10025 Italy Caltech The Division of Physics Mathematics and Astronomy 1200 E California Blvd PasadenaCA91125 United States Institute for Astrophysical Research Boston University 725 Commonwealth Avenue BostonMA02215 United States The University of Tokyo Kashiwa Chiba 277-8582 Japan ETH Zürich ZürichCH-8093 Switzerland Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN PadovaI-35131 Italy Bellaterra BarcelonaE-08193 Spain Technische Universität Dortmund DortmundD-44221 Germany Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 S

The blazar S5 0716+714 is an intermediate BL Lacertae object remarkable for its variability in many energy bands. It was discovered by MAGIC in the very-high-energy (VHE) gamma-ray range in 2008. Later in 2015 an impressive electric vector polarization angle (EVPA) swing was detected in connection with a multiwavelength flaring event including the VHE gamma-ray band. This generated interest in further studies of the jet of this source and its electromagnetic emission at all wavelengths. Since then, MAGIC has monitored the source in coordination with other observatories and here we present the long-term study using data from 2015 to 2022 in a MWL context. The data set also includes the extraordinary flaring activity of 2017, so far the historical maximum detected for this source in the optical and VHE gamma-ray band. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Gamma rays

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Second gadolinium loading to Super-Kamiokande

arXiv

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arXiv 2024年

作者： Abe, K. Bronner, C. Hayato, Y. Hiraide, K. Hosokawa, K. Ieki, K. Ikeda, M. Kameda, J. Kanemura, Y. Kaneshima, R. Kashiwagi, Y. Kataoka, Y. Miki, S. Mine, S. Miura, M. Moriyama, S. Nakano, Y. Nakahata, M. Nakayama, S. Noguchi, Y. Sato, K. Sekiya, H. Shiba, H. Shimizu, K. Shiozawa, M. Sonoda, Y. Suzuki, Y. Takeda, A. Takemoto, Y. Tanaka, H. Yano, T. Han, S. Kajita, T. Okumura, K. Tashiro, T. Tomiya, T. Wang, X. Yoshida, S. Fernandez, P. Labarga, L. Ospina, N. Zaldivar, B. Pointon, B.W. Kearns, E. Raaf, J.L. Wan, L. Wester, T. Bian, J. Griskevich, N.J. Smy, M.B. Sobel, H.W. Takhistov, V. Yankelevich, A. Hill, J. Jang, M.C. Lee, S.H. Moon, D.H. Park, R.G. Bodur, B. Scholberg, K. Walter, C.W. Beauchêne, A. Drapier, O. Giampaolo, A. Mueller, Th.A. Santos, A.D. Paganini, P. Quilain, B. Rogly, R. Nakamura, T. Jang, J.S. Machado, L.N. Learned, J.G. Choi, K. Iovine, N. Cao, S. Anthony, L.H.V. Martin, D. Prouse, N.W. Scott, M. Uchida, Y. Berardi, V. Calabria, N.F. Catanesi, M.G. Radicioni, E. Langella, A. De Rosa, G. Collazuol, G. Iacob, F. Mattiazzi, M. Ludovici, L. Gonin, M. Périssé, L. Pronost, G. Fujisawa, C. Maekawa, Y. Nishimura, Y. Okazaki, R. Akutsu, R. Friend, M. Hasegawa, T. Ishida, T. Kobayashi, T. Jakkapu, M. Matsubara, T. Nakadaira, T. Nakamura, K. Oyama, Y. Sakashita, K. Sekiguchi, T. Tsukamoto, T. Bhuiyan, N. Burton, G.T. Di Lodovico, F. Gao, J. Goldsack, A. Katori, T. Migenda, J. Ramsden, R.M. Xie, Z. Zsoldos, S. Suzuki, A.T. Takagi, Y. Takeuchi, Y. Zhong, H. Feng, J. Feng, L. Hu, J.R. Hu, Z. Kawaue, M. Kikawa, T. Mori, M. Nakaya, T. Wendell, R.A. Yasutome, K. Jenkins, S.J. McCauley, N. Mehta, P. Tarant, A. Wilking, M.J. Fukuda, Y. Itow, Y. Menjo, H. Ninomiya, K. Yoshioka, Y. Lagoda, J. Mandal, M. Mijakowski, P. Prabhu, Y.S. Zalipska, J. Jia, M. Jiang, J. Shi, W. Yanagisawa, C. Harada, M. Hino, Y. Ishino, H. Koshio, Y. Nakanishi, F. Sakai, S. Tada, T. BMCC CUNY Science Department New YorkNY1007 United States University of Victoria Department of Physics and Astronomy PO Box 1700 STN CSC VictoriaBCV8W 2Y2 Canada Kamioka Observatory Institute for Cosmic Ray Research Univerity of Tokyo Gifu Kamioka506-1205 Japan Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Department of Theoretical Physics University Autonoma Madrid Madrid28049 Spain Department of Physics Boston University BostonMA02215 United States Department of Physics British Columbia Institute of Technology BurnabyBCV5G 3H2 Canada Department of Physics and Astronomy University of California Irvine IrvineCA92697-4575 United States Department of Physics California State University Dominguez Hills CarsonCA90747 United States Institute for Universe and Elementary Particles Chonnam National University Gwangju61186 Korea Republic of Department of Physics Duke University DurhamNC27708 United States Ecole Polytechnique IN2P3-CNRS Laboratoire Leprince-Ringuet PalaiseauF-91120 France Department of Physics Gifu University Gifu Gifu501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju500-712 Korea Republic of School of Physics and Astronomy University of Glasgow GlasgowG12 8QQ United Kingdom Department of Physics and Astronomy University of Hawaii HonoluluHI96822 United States Daejeon34126 Korea Republic of Institute For Interdisciplinary Research in Science and Education ICISE Quy Nhon55121 Viet Nam Department of Physics Imperial College London LondonSW7 2AZ United Kingdom Dipartimento Interuniversitario di Fisica INFN Sezione di Bari Università e Politecnico di Bari BariI-70125 Italy Dipartimento di Fisica INFN Sezione di Napoli Università di Napoli NapoliI-80126 Italy Dipartimento di Fisica INFN Sezione di Padova Università di Padova PadovaI-35131 Italy INFN Sezione di Roma Università di Roma "La Sapienza" R

The first loading of gadolinium (Gd) into Super-Kamiokande in 2020 was successful, and the neutron capture efficiency on Gd reached 50%. To further increase the Gd neutron capture efficiency to 75%, 26.1 tons of Gd2(SO4)3·8H2O was additionally loaded into Super-Kamiokande (SK) from May 31 to July 4, 2022. As the amount of loaded Gd2(SO4)3·8H2O was doubled compared to the first loading, the capacity of the powder dissolving system was doubled. We also developed new batches of gadolinium sulfate with even further reduced radioactive impurities. In addition, a more efficient screening method was devised and implemented to evaluate these new batches of Gd2(SO4)3 · 8H2O . Following the second loading, the Gd concentration in SK was measured to be 333.5 ±2.5 ppm via an Atomic Absorption Spectrometer (AAS). From the mean neutron capture time constant of neutrons from an Am/Be calibration source, the Gd concentration was independently measured to be 332.7 ± 6.8(sys.) ± 1.1(stat.) ppm, consistent with the AAS result. Furthermore, during the loading the Gd concentration was monitored continually using the capture time constant of each spallation neutron produced by cosmic-ray muons, and the final neutron capture efficiency was shown to become 1.5 times higher than that of the first loaded phase, as expected. Copyright © 2024, The Authors. All rights reserved.

关键词： Neutrons

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The rank of contextuality

arXiv

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arXiv 2022年

作者： Horodecki, Karol Zhou, Jingfang Stankiewicz, Maciej Salazar, Roberto Horodecki, Pawel Raussendorf, Robert Horodecki, Ryszard Ramanathan, Ravishankar Tyhurst, Emily Institute of Informatics National Quantum Information Centre Faculty of Mathematics Physics and Informatics University of Gdańsk Wita Stwosza 57 Gdańsk80-308 Poland International Centre for Theory of Quantum Technologies University of Gdańsk Wita Stwosza 63 Gdańsk80-308 Poland Department of Applied Physics Graduate School of Engineering University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-8656 Japan Faculty of Physics Astronomy and Applied Computer Science Jagiellonian University Kraków30-348 Poland Faculty of Applied Physics and Mathematics National Quantum Information Centre Gdańsk University of Technology Gabriela Narutowicza 11/12 Gdańsk80-233 Poland Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z1 Canada Department of Computer Science The University of Hong Kong Pokfulam Road Hong Kong Department of Physics University of Toronto TorontoON Canada

Quantum contextuality is one of the most recognized resources in quantum communication and computing scenarios. We provide a new quantifier of this resource, the rank of contextuality (RC). We define RC as the minimum number of non-contextual behaviors that are needed to simulate a contextual behavior. We show that the logarithm of RC is a natural contextuality measure satisfying several properties considered in the spirit of the resource-theoretic approach. The properties include faithfulness, monotonicity, and additivity under tensor product. We also give examples of how to construct contextual behaviors with an arbitrary value of RC exhibiting a natural connection between this quantifier and the arboricity of an underlying hypergraph. We also discuss exemplary areas of research in which the new measure appears as a natural quantifier. Copyright © 2022, The Authors. All rights reserved.

关键词： Quantum communication

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Length Scales in Brownian yet Non-Gaussian Dynamics

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Physical Review X 2021年第3期11卷 031002-031002页

作者： José M. Miotto Simone Pigolotti Aleksei V. Chechkin Sándalo Roldán-Vargas Leiden Institute of Advanced Computer Science 2333 CA Leiden Netherlands Biological Complexity Unit Okinawa Institute for Science and Technology and Graduate University Onna Okinawa 904-0495 Japan Institute for Physics and Astronomy University of Potsdam 14476 Potsdam-Golm Germany Akhiezer Institute for Theoretical Physics Kharkov 61108 Ukraine Max Planck Institute for the Physics of Complex Systems 01187 Dresden Germany Department of Applied Physics Faculty of Sciences University of Granada 18071 Granada Spain

According to the classical theory of Brownian motion, the mean-squared displacement of diffusing particles evolves linearly with time, whereas the distribution of their displacements is Gaussian. However, recent experiments on mesoscopic particle systems have discovered Brownian yet non-Gaussian regimes where diffusion coexists with an exponential tail in the distribution of displacements. Here we show that, contrary to the present theoretical understanding, the length scale λ associated with this exponential distribution does not necessarily scale in a diffusive way. Simulations of Lennard-Jones systems reveal a behavior λ∼t1/3 in three dimensions and λ∼t1/2 in two dimensions. We propose a scaling theory based on the idea of hopping motion to explain this result. In contrast, simulations of a tetrahedral gelling system, where particles interact by a nonisotropic potential, yield a temperature-dependent scaling of λ. We interpret this behavior in terms of an intermittent hopping motion. Our findings link the Brownian yet non-Gaussian phenomenon with generic features of glassy dynamics and open new experimental perspectives on the class of molecular and supramolecular systems whose dynamics is ruled by rare events.

关键词： Brownian motion Collective behavior Diffusion Gels Glassy systems Liquids Extreme event statistics Molecular dynamics

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Impacts of the 12C(α, γ)16O reaction rate on 56Ni nucleosynthesis in pair-instability supernovae

arXiv

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arXiv 2023年

作者： Kawashimo, Hiroki Sawada, Ryo Suwa, Yudai Moriya, Takashi J. Tanikawa, Ataru Tominaga, Nozomu Department of Earth Science and Astronomy Graduate School of Arts and Sciences The University of Tokyo Tokyo Meguro153-8902 Japan RIKEN Nishina Center for Accelerator-based Science RIKEN Saitama Wako351-0198 Japan Institute for Cosmic Ray Research The University of Tokyo Chiba Kashiwa277-8582 Japan Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan National Astronomical Observatory of Japan National Institutes of Natural Sciences Mitaka Tokyo181-8588 Japan Astronomical Science Program Graduate Institute for Advanced Studies SOKENDAI Mitaka Tokyo181-8588 Japan School of Physics and Astronomy Faculty of Science Monash University ClaytonVIC3800 Australia Center for Information Science Fukui Prefectural University Eiheiji Fukui910-1195 Japan Department of Physics Faculty of Science and Engineering Konan University Hyogo Kobe658-8501 Japan

Nuclear reactions are key to our understanding of stellar evolution, particularly the 12C(α, γ)16O rate, which is known to significantly influence the lower and upper ends of the black hole (BH) mass distribution due to pair-instability supernovae (PISNe). However, these reaction rates have not been sufficiently determined. We use the MESA stellar evolution code to explore the impact of uncertainty in the 12C(α, γ)16O rate on PISN explosions, focusing on nucleosynthesis and explosion energy by considering the high resolution of the initial mass. Our findings show that the mass of synthesized radioactive nickel (56Ni) and the explosion energy increase with 12C(α, γ)16O rate for the same initial mass, except in the high-mass edge region. With a high (about twice the STARLIB standard value) rate, the maximum amount of nickel produced falls below 70 M☉, while with a low rate (about half of the standard value) it increases up to 83.9 M☉. These results highlight that carbon "preheating" plays a crucial role in PISNe by determining core concentration when a star initiates expansion. Our results also suggest that the onset of the expansion, which means the end of compression, competes with collapse caused by helium photodisintegration, and the maximum mass that can lead to an explosion depends on the 12C(α, γ)16O reaction rate. © 2023, CC BY.

关键词： Nucleosynthesis

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Understanding the origin of the extended γ-ray emission and the physical nature of HESS J1841-055 using observations at TeV energies with the MAGIC telescopes 37

Understanding the origin of the extended γ-ray emission and...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Acciari, V.A. Ansoldi, S. Antonelli, L.A. Arbet Engels, A. Artero, M. Asano, K. Baack, D. Babić, A. Baquero, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Becerra González, J. Bednarek, W. Bellizzi, L. Bernardini, E. Bernardos, M. Berti, A. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bökenkamp, H. Bonnoli, G. Bošnjak, Ž. Busetto, G. Carosi, R. Ceribella, G. Cerruti, M. Chai, Y. Chilingarian, A. Cikota, S. Colak, S.M. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D'Amico, G. D'Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Delfino, M. Delgado, J. Delgado Mendez, C. Depaoli, D. Di Pierro, F. Di Venere, L. Do Souto Espiñeira, E. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsaesser, D. Fallah Ramazani, V. Fattorini, A. Fonseca, M.V. Font, L. Fruck, C. Fukami, S. Fukazawa, Y. García López, R.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, David Green, J.G. Hadasch, D. Hahn, A. Heckmann, L. Herrera, J. Hoang, J. Hrupec, D. Hütten, M. Inada, T. Ishio, K. Iwamura, Y. Jiménez Martínez, I. Jormanainen, J. Jouvin, L. Karjalainen, M. Kerszberg, D. Kobayashi, Y. Kubo, H. Kushida, J. Lamastra, A. Lelas, D. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, Alicia Loporchio, S. Machado de Oliveira Fraga, B. Maggio, C. Majumdar, P. Makariev, M. Mallamaci, M. Maneva, G. Manganaro, M. Mannheim, K. Maraschi, L. Mariotti, M. Martínez, M. Mazin, D. Menchiari, S. Mender, S. Mićanović, S. Miceli, D. Miener, T. Miranda, J.M. Mirzoyan, R. Molina, E. Moralejo, A. Morcuende, D. Moreno, V. Moretti, E. Nakamori, T. Nava, L. Neustroev, V. Nigro, C. Nilsson, K. Nishijima, K. Noda, K. Nozaki, S. Ohtani, Y. Oka, T. Otero-Santos, J. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J.M. Pavletić, L. Peñil, P. Persic, M. Pihet, M. Prada Moroni, P.G. Prandini, E. Priyadarshi, C. Brazil Spain Croatian MAGIC Group Ruđer Bošković Institute Croatia Croatia Croatian MAGIC Group Josip Juraj Strossmayer University of Osijek Department of Physics Croatia Croatian MAGIC Group University of Rijeka Department of Physics Croatia Croatia Germany Technische Universität Dortmund Germany ETH Zürich Switzerland Finnish MAGIC Group Finnish Centre for Astronomy with ESO University of Turku Finland Finnish MAGIC Group Astronomy Research Unit University of Oulu Finland Instituto de Astrofísica de Andalucía-CSIC Spain Instituto de Astrofísica de Canarias La LagunaE-38200 Spain Universidad de La Laguna Dpto. Astrofísica La Laguna TenerifeE-38206 Spain Spain INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica Università e del Politecnico di Bari Italy INFN MAGIC Group INFN Sezione di Perugia Italy INFN MAGIC Group INFN Roma Tor Vergata The University of Tokyo Japan Japanese MAGIC Group Department of Physics Kyoto University Japan Japanese MAGIC Group Department of Physics Tokai University Japan Japanese MAGIC Group: Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Japan Japanese MAGIC Group Department of Physics Yamagata University Japan Japanese MAGIC Group Department of Physics Konan University Japan University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Poland IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain Max-Planck-Institut für Physik MünchenD-80805 Germany Università di Padova INFN Italy Università di Pisa INFN Pisa Italy Università di Siena INFN Pisa Italy Saha Institute of Nuclear Physics India Inst. for Nucl. Research and Nucl. Energy Bulgarian Academy of Sciences Bulgaria Departament de Física CERES-IEEC Universitat Autónoma de Barcelona Spain Universitat de Barcelona ICCUB IEEC-UB Spain Università

With the improved sensitivity with respect to the previous generation, current space-borne and ground-based gamma-ray telescopes have made the number of γ-ray sources detected at GeV-TeV energies increase many folds over the last decade. Many of the detected extended gamma-ray sources are not associated with any known sources at other wavelengths. Understanding the nature of these sources and the origin of the observed high energy gamma-ray emission remains a great challenge. Using the MAGIC telescopes, we have observed one such unassociated gamma-ray source, named HESS J1841-055 at TeV energies. We investigate the physical nature and origin of the γ-ray emission from this extended source. In this paper, we present the results of our detailed investigation on this source using MAGIC data and other multi-waveband information on nearby sources. The results included in this proceeding and shown in this presentation were published in ref. [1]. The details about the analysis, interpretation and modelling can be found in the aforementioned reference. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)

关键词： Gamma rays

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Macroscopically Self-Aligned and Chiralized Carbon Nanotubes: From Filtration to Innovation

arXiv

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arXiv 2023年

作者： Doumani, Jacques Zahn, Keshav Yu, Shengjie Barrios, Gustavo Rodriguez Sasmal, Somesh Kikuchi, Rikuta Kritzell, T. Elijah Xu, Hongjing Baydin, Andrey Kono, Junichiro Department of Electrical and Computer Engineering Rice University 6100 Main Street HoustonTX77005 United States Applied Physics Graduate Program Smalley–Curl Institute Rice University 6100 Main Street HoustonTX77005 United States Carbon Hub Rice University 6100 Main Street HoustonTX77005 United States Smalley–Curl Institute Rice University 6100 Main Street HoustonTX77005 United States Department of Physics and Astronomy Rice University 6100 Main Street HoustonTX77005 United States Department of Materials Science and NanoEngineering Rice University 6100 Main Street HoustonTX77005 United States

Because of their natural one-dimensional (1D) structure combined with intricate chiral variations, carbon nanotubes (CNTs) exhibit various exceptional physical properties, such as ultrahigh electrical and thermal conductivity, exceptional mechanical strength, and chirality-dependent metallicity. These properties make CNTs highly promising for diverse applications, including field-effect transistors, sensors, photodetectors, and thermoelectric devices. While CNTs excel individually at the nanoscale, their 1D and chiral nature can be lost on a macroscopic scale when they are randomly assembled. Therefore, the alignment and organization of CNTs in macroscopic structures is crucial for harnessing their full potential. In this review, we explore recent advancements in understanding CNT alignment mechanisms, improving CNT aligning methods, and demonstrating macroscopically 1D properties of ordered CNT assemblies. We also focus on a newly discovered class of CNT architectures, combining CNT alignment and twisting mechanisms to create artificial radial and chiral CNT films at wafer scales. Finally, we summarize recent developments related to aligned and chiral CNT films in optoelectronics, highlighting their unique roles in solar cells, thermal emitters, and optical modulators. Copyright © 2023, The Authors. All rights reserved.

关键词： Carbon nanotubes

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Control noise reduction of cryogenic suspension in KAGRA

Control noise reduction of cryogenic suspension in KAGRA

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38th International Cosmic Ray Conference, ICRC 2023

作者： Tamaki, Masahide Abe, H. Ando, M. Aoumi, M. Chang, R.-J. Chen, A.H.-Y. Chen, H. Chen, Y. Chiba, A. Chiba, R. Chou, C. Eisenmann, M. Fujii, S. Fukunaga, I. Haba, D. Haino, S. Hayakawa, H. Hayama, K. Hirata, N. Hirose, C. Hoshino, S. Hsiung, C. Iwaya, M. Kato, J. Kato, T. Kimura, N. Kiyota, T. Koyama, N. Kuwahara, S. Lai, S. Ma, L.-T. Maeda, K. Matsuyama, M. Mio, N. Miyamoto, S. Murakoshi, M. Nishino, Y. Obayashi, K. Sakai, K. Sako, T. Sato, R. Sato, S. Sato, Y. Shiota, J. Suzuki, T. Takatani, K. Takeda, M. Tamaki, M. Tomita, K. Toriyama, A. Yamamoto, M. Yamamura, S. Yang, L.-C. Yeh, S.-W. Yokozawa, T. Graduate School of Science Tokyo Institute of Technology 2-12-1 Ookayama Meguro-ku Tokyo152-8551 Japan Gravitational Wave Science Project National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo181-8588 Japan Department of Physics The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Institute for Cosmic Ray Research KAGRA Observatory The University of Tokyo 238 Higashi-Mozumi Kamioka-cho Hida City Gifu506-1205 Japan Department of Physics National Cheng Kung University No.1 University Road Tainan City701 Taiwan Institute of Physics National Yang Ming Chiao Tung University 101 Univ. Street Hsinchu Taiwan Department of Physics National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Faculty of Science University of Toyama 3190 Gofuku Toyama City Toyama930-8555 Japan Institute for Cosmic Ray Research KAGRA Observatory The University of Tokyo 5-1-5 Kashiwa-no-Ha Chiba Kashiwa City277-8582 Japan Department of Electrophysics National Yang Ming Chiao Tung University 101 Univ. Street Hsinchu Taiwan Department of Physics Graduate School of Science Osaka Metropolitan University 3-3-138 Sugimoto-cho Sumiyoshi-ku Osaka City Osaka558-8585 Japan Institute of Physics Academia Sinica 128 Sec. 2 Academia Rd. Nankang Taipei11529 Taiwan Department of Applied Physics Fukuoka University 8-19-1 Nanakuma Jonan Fukuoka Fukuoka City814-0180 Japan Faculty of Engineering Niigata University 8050 Ikarashi-2-no-cho Nishi-ku Niigata City Niigata950-2181 Japan Institute of Astronomy National Tsing Hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Department of Physics Tamkang University No. 151 Yingzhuan Rd. Danshui Dist. New Taipei City25137 Taiwan Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwa-no-Ha Chiba Kashiwa City277-8582 Japan Institute for Photon Science and Technol

In gravitational wave detectors, the laser is used to observe how the distance between mirrors changes due to space distortions caused by gravitational waves. The displacement of the mirrors is minute, so the mirrors must be sufficiently isolated from ground vibrations to achieve the required sensitivity. Therefore, the main mirrors are suspended by nine-stage pendulums in KAGRA, the gravitational wave detector in Japan. In such a pendulum-based vibration isolator, the mirror oscillates significantly at the resonant frequency. Hence we need the control system to damp the resonances, but the noise from the sensors used in such a control system can be a problem. In fact, the sensitivity of KAGRA was limited by the noise from the cryogenic payload control system at 10-50 Hz in the previous observation. Therefore, a low-noise control filter was designed and implemented for use during the previous observing run. As a result, the control noise of the cryogenic payload at 10-100 Hz was reduced by 2-3 orders of magnitude, and the target sensitivity for the O4 observing run was achieved at low frequency (below 100 Hz). © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Pendulums

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Erratum to: Search for single top-quark production via flavour-changing neutral currents at 8 TeV with the ATLAS detector

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The European Physical Journal C 2022年第1期82卷 1-15页

作者： Aad, G. Abbott, B. Abdallah, J. Abdinov, O. Aben, R. Abolins, M. AbouZeid, O. S. Abramowicz, H. Abreu, H. Abreu, R. Abulaiti, Y. Acharya, B. S. Adamczyk, L. Adams, D. L. Adelman, J. Adomeit, S. Adye, T. Affolder, A. A. Agatonovic-Jovin, T. Agricola, J. Aguilar-Saavedra, J. A. Ahlen, S. P. Ahmadov, F. Aielli, G. Akerstedt, H. Åkesson, T. P. A. Akimov, A. V. Alberghi, G. L. Albert, J. Albrand, S. Alconada Verzini, M. J. Aleksa, M. Aleksandrov, I. N. Alexa, C. Alexander, G. Alexopoulos, T. Alhroob, M. Alimonti, G. Alio, L. Alison, J. Alkire, S. P. Allbrooke, B. M. M. Allport, P. P. Aloisio, A. Alonso, A. Alonso, F. Alpigiani, C. Altheimer, A. Alvarez Gonzalez, B. Álvarez Piqueras, D. Alviggi, M. G. Amadio, B. T. Amako, K. Amaral Coutinho, Y. Amelung, C. Amidei, D. Amor Dos Santos, S. P. Amorim, A. Amoroso, S. Amram, N. Amundsen, G. Anastopoulos, C. Ancu, L. S. Andari, N. Andeen, T. Anders, C. F. Anders, G. Anders, J. K. Anderson, K. J. Andreazza, A. Andrei, V. Angelidakis, S. Angelozzi, I. Anger, P. Angerami, A. Anghinolfi, F. Anisenkov, A. V. Anjos, N. Annovi, A. Antonelli, M. Antonov, A. Antos, J. Anulli, F. Aoki, M. Aperio Bella, L. Arabidze, G. Arai, Y. Araque, J. P. Arce, A. T. H. Arduh, F. A. Arguin, J-F. Argyropoulos, S. Arik, M. Armbruster, A. J. Arnaez, O. Arnal, V. Arnold, H. Arratia, M. Arslan, O. Artamonov, A. Artoni, G. Asai, S. Asbah, N. Ashkenazi, A. Åsman, B. Asquith, L. Assamagan, K. Astalos, R. Atkinson, M. Atlay, N. B. Augsten, K. Aurousseau, M. Avolio, G. Axen, B. Ayoub, M. K. Azuelos, G. Baak, M. A. Baas, A. E. Baca, M. J. Bacci, C. Bachacou, H. Bachas, K. Backes, M. Backhaus, M. Bagiacchi, P. Bagnaia, P. Bai, Y. Bain, T. Baines, J. T. Baker, O. K. Baldin, E. M. Balek, P. Balestri, T. Balli, F. Banas, E. Banerjee, Sw. Bannoura, A. A. E. Bansil, H. S. Barak, L. Barberio, E. L. Barberis, D. Barbero, M. Barillari, T. Barisonzi, M. Barklow, T. Barlow, N. Barnes, S. L. Barnett, B. M. Barnett, R. M. Barnovska, Z. Baroncelli, A. Barone, G. Barr, A. J. Barreiro, F. Barreiro Guimarães da Costa, J. Bartol CPPM Aix-Marseille Université and CNRS/IN2P3 Marseille France Homer L. Dodge Department of Physics and Astronomy University of Oklahoma Norman USA Institute of Physics Academia Sinica Taipei Taiwan Institute of Physics Azerbaijan Academy of Sciences Baku Azerbaijan Nikhef National Institute for Subatomic Physics and University of Amsterdam Amsterdam The Netherlands Department of Physics and Astronomy Michigan State University East Lansing USA Department of Physics University of Toronto Toronto Canada Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv Israel Department of Physics Technion: Israel Institute of Technology Haifa Israel Center for High Energy Physics University of Oregon Eugene USA Department of Physics Stockholm University Stockholm Sweden The Oskar Klein Centre Stockholm Sweden INFN Gruppo Collegato di Udine Sezione di Trieste Udine Italy ICTP Trieste Italy Department of Physics King’s College London London UK AGH University of Science and Technology Faculty of Physics and Applied Computer Science Kraków Poland Physics Department Brookhaven National Laboratory Upton USA Department of Physics Northern Illinois University De Kalb USA Fakultät für Physik Ludwig-Maximilians-Universität München Munich Germany Particle Physics Department Rutherford Appleton Laboratory Didcot UK Oliver Lodge Laboratory University of Liverpool Liverpool UK Institute of Physics University of Belgrade Belgrade Serbia II Physikalisches Institut Georg-August-Universität Göttingen Germany Laboratório de Instrumentação e Física Experimental de Partículas-LIP Lisbon Portugal Departamento de Fisica Teorica y del Cosmos and CAFPE Universidad de Granada Granada Spain Department of Physics Boston University Boston USA Joint Institute for Nuclear Research JINR Dubna Dubna Russia INFN Sezione di Roma Tor Vergata Rome Italy Dipartimento di Fisica Università di Roma Tor Vergata Rome Italy Fysiska institutionen Lunds uni

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