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arXiv 2021年

作者： Combes, Francoise Gupta, N. Muller, S. Balashev, S. Józsa, G.I.G. Srianand, R. Momjian, E. Noterdaeme, P. Klöckner, H.-R. Baker, A.J. Boettcher, E. Bosma, A. Chen, H.-W. Dutta, R. Jagannathan, P. Jose, J. Knowles, K. Krogager, J.-K. Kulkarni, V.P. Moodley, K. Pandey, S. Petitjean, P. Sekhar, S. Observatoire de Paris LERMA Collège de France CNRS PSL University Sorbonne University Paris75014 France Inter-University Centre for Astronomy and Astrophysics Post Bag 4 Ganeshkhind Pune411 007 India Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory Onsala43992 Sweden Ioffe Institute Polyteknicheskaya 26 Saint-Petersburg194021 Russia South African Radio Astronomy Observatory 2 Fir Street Black River Park Observatory7925 South Africa Department of Physics and Electronics Rhodes University P.O. Box 94 Makhanda6140 South Africa Argelander-Institut für Astronomie Auf dem Hügel 71 BonnD-53121 Germany National Radio Astronomy Observatory SocorroNM87801 United States Institut d’Astrophysique de Paris CNRS-SU UMR 7095 98bis bd Arago Paris75014 France Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Department of Physics and Astronomy Rutgers State University of New Jersey 136 Frelinghuysen Road PiscatawayNJ08854-8019 United States Department of Astronomy & Astrophysics University of Chicago 5640 S Ellis Ave. ChicagoIL60637 United States Aix Marseille Univ. CNRS CNES LAM Marseille France Institute for Computational Cosmology Durham University South Road DurhamDH1 3LE United Kingdom Centre for Extragalactic Astronomy Durham University South Road DurhamDH1 3LE United Kingdom ThoughtWorks Technologies India Private Limited Yerawada Pune411 006 India Astrophysics Research Centre and School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban4041 South Africa Department of Physics and Astronomy University of South Carolina ColumbiaSC29208 United States School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban4041 South Africa Dep. of Astronomy Univ. of Cape Town Private Bag X3 Rondebosch7701 South Africa Univ. of the Western Cape Dep. of Physics and Astronomy Bellville7535 South Africa

The Large Survey Project (LSP) "MeerKAT Absorption Line Survey" (MALS) is a blind H i 21-cm and OH 18-cm absorption line survey in the L- and UHF-bands, with the primary goal to better determine the occurrence of atomic and molecular gas in the circumgalactic and inter-galactic medium, and its redshift evolution. Here we present the first results using the UHF-band, obtained towards the strongly lensed radio source PKS 1830−211, detecting absorption produced by the lensing galaxy. With merely 90 mins of data acquired on-source for science verification and processed using the Automated Radio Telescope Imaging Pipeline (ARTIP), we detect in absorption the known H i 21-cm and OH 18-cm main lines at z = 0.89 at an unprecedented signal-to-noise ratio (4000 in the continuum, in each 6 km s−1 wide channel). For the first time we report the detection at z = 0.89 of OH satellite lines, so far not detected at z > 0.25. We decompose the OH lines into a thermal and a stimulated contribution, where the 1612 and 1720 MHz lines are conjugate. The total OH 1720 MHz emission line luminosity is 6100 L . This is the most luminous known 1720 MHz maser line. It is also among the highest luminosities for the OH-main lines megamasers. The absorption components of the different images of the background source sample different light paths in the lensing galaxy, and their weights in the total absorption spectrum are expected to vary in time, on daily and monthly time scales. We compare our normalized spectra with those obtained more than 20 yrs ago, and find no variation, in spite of the high signal-to-noise ratios. We interpret the absorption spectra with the help of a lens galaxy model, derived from an N-body hydro-dynamical simulation, with a morphology similar to its optical HST image. The resulting absorption lines dep.nd mainly on the background continuum, and the radial distribution of the gas surface density, for each atomic /molecular species. We show that it is possible to reproduc

关键词： Galaxies

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Quantum Computing for High-Energy Physics State of the Art and Challenges Summary of the QC4HEP Working Group

arXiv

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arXiv 2023年

作者： Di Meglio, Alberto Jansen, Karl Tavernelli, Ivano Alexandrou, Constantia Arunachalam, Srinivasan Bauer, Christian W. Borras, Kerstin Carrazza, Stefano Crippa, Arianna Croft, Vincent de Putter, Roland Delgado, Andrea Dunjko, Vedran Egger, Daniel J. Fernández-Combarro, Elias Fuchs, Elina Funcke, Lena González-Cuadra, Daniel Grossi, Michele Halimeh, Jad C. Holmes, Zoë Kühn, Stefan Lacroix, Denis Lewis, Randy Lucchesi, Donatella Martinez, Miriam Lucio Meloni, Federico Mezzacapo, Antonio Montangero, Simone Nagano, Lento Radescu, Voica Ortega, Enrique Rico Roggero, Alessandro Schuhmacher, Julian Seixas, Joao Silvi, Pietro Spentzouris, Panagiotis Tacchino, Francesco Temme, Kristan Terashi, Koji Tura, Jordi Tüysüz, Cenk Vallecorsa, Sofia Wiese, Uwe-Jens Yoo, Shinjae Zhang, Jinglei GenevaCH-1211 Switzerland CQTA Deutsches Elektronen-Synchrotron DESY Platanenallee 6 Zeuthen15738 Germany Computation-based Science and Technology Research Center The Cyprus Institute 20 Constantinou Kavafi str. Nicosia2121 Cyprus IBM Quantum IBM Research – Zurich Rüschlikon8803 Switzerland Department of Physics University of Cyprus PO Box 20537 Nicosia1678 Cyprus IBM Quantum IBM Research 1101 Kitchawan Rd Yorktown HeightsNY United States Physics Division LBNL - M/S 50A5104 1 Cyclotron Rd BerkeleyCA United States Deutsches Elektronen-Synchrotron DESY Notkestrasse 85 Hamburg22607 Germany RWTH Aachen University Templergraben 55 Aachen52062 Germany TIF Lab Dipartimento di Fisica Università degli Studi di Milano INFN Sezione di Milano Milan Italy Institut für Physik Humboldt-Universität zu Berlin Newtonstr. 15 Berlin12489 Germany haQaLi Applied Quantum Algorithms Leiden Netherlands Physics Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Department of Computer Science Facultad de Ciencias University of Oviedo Asturias33007 Spain Institute of Theoretical Phyiscs Leibniz University Hannover Hannover30167 Germany Physikalisch-Technische Bundesanstalt Braunschweig38116 Germany University of Bonn Nußallee 14-16 Bonn53115 Germany Institute for Theoretical Physics University of Innsbruck Innsbruck6020 Austria Institute for Quantum Optics and Quantum Information the Austrian Academy of Sciences Innsbruck6020 Austria Department of Physics Arnold Sommerfeld Center for Theoretical Physics Ludwig-Maximilians-Universität München Germany Munich Center for Quantum Science and Technology Germany LausanneCH-1015 Switzerland Paris-Saclay University CNRS IN2P3 IJCLab Orsay91405 France Department of Physics and Astronomy York University TorontoONM3J 1P3 Canada Department of Physics and Astronomy Università di Padova V. Marzolo 8 PadovaI-35131 Italy INFN - Sezione di Padova Via Marzolo 8 Padova35131 Italy Ni

Quantum computers offer an intriguing path for a paradigmatic change of computing in the natural sciences and beyond, with the potential for achieving a so-called quantum advantage, namely a significant (in some cases exponential) speed-up of numerical simulations. The rapid development of hardware devices with various realizations of qubits enables the execution of small scale but representative applications on quantum computers. In particular, the high-energy physics community plays a pivotal role in accessing the power of quantum computing, since the field is a driving source for challenging computational problems. This concerns, on the theoretical side, the exploration of models which are very hard or even impossible to address with classical techniques and, on the experimental side, the enormous data challenge of newly emerging experiments, such as the upgrade of the Large Hadron Collider. In this roadmap paper, led by CERN, DESY and IBM, we provide the status of high-energy physics quantum computations and give examples for theoretical and experimental target benchmark applications, which can be addressed in the near future. Having the IBM 100 100 challenge in mind, where possible, we also provide resource estimates for the examples given using error mitigated quantum computing. © 2023, CC BY-SA.

关键词： High energy physics

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Giant radio array for neutrino detection: Science and design

arXiv

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arXiv 2018年

作者： Álvarez-Muñiz, Jaime Batista, Rafael Alves Balagopal, Aswathi V. Bolmont, Julien Bustamante, Mauricio Jr, Washington Carvalho Charrier, Didier Cognard, Ismaël Decoene, Valentin Denton, Peter B. de Jong, Sijbrand de Vries, Krijn D. Engel, Ralph Fang, Ke Finley, Chad Gabici, Stefano Gou, QuanBu Gu, Junhua Guépin, Claire Hu, Hongbo Huang, Yan Kotera, Kumiko Le Coz, Sandra Lenain, Jean-Philippe Lü, Guoliang Martineau-Huynh, Olivier Mostafá, Miguel Mottez, Fabrice Murase, Kohta Niess, Valentin Oikonomou, Foteini Pierog, Tanguy Qian, Xiangli Qin, Bo Ran, Duan Renault-Tinacci, Nicolas Roth, Markus Schröder, Frank G. Schüssler, Fabian Tasse, Cyril Timmermans, Charles Tueros, Matías Wu, Xiangping Zarka, Philippe Zech, Andreas Zhang, B. Theodore Zhang, Jianli Zhang, Yi Zheng, Qian Zilles, Anne Departamento de Física de Partículas Instituto Galego de Física de Altas Enerxías Universidad de Santiago de Compostela Santiago de Compostela15782 Spain Instituto de Astronomia Geofísica e Ciências Atmosféricas Universidade de São Paulo Rua do Matão 1226 São Paulo-SP05508-090 Brazil Department of Physics – Astrophysics University of Oxford DWB Keble Road OxfordOX1 3RH United Kingdom KarlsruheD-76021 Germany 4 place Jussieu Paris Cedex 5F-75252 France Niels Bohr International Academy and DARK Niels Bohr Institute Copenhagen2100 Denmark Discovery Center Niels Bohr Institute Copenhagen2100 Denmark Dep. of Physics Ohio State University ColumbusOH43210 United States Universidade de Santiago de Compostela Santiago de Compostela15782 Spain SUBATECH Institut Mines-Telecom Atlantique – CNRS/IN2P3 Université de Nantes Nantes France Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E CNRS-Université d’Orléans OrléansF-45071 France Station de Radioastronomie de Nançay Observatoire de Paris CNRS/INSU NançayF-18330 France Sorbonne Université UMR 7095 Institut d’Astrophysique de Paris 98 bis bd Arago Paris75014 France Radboud Universiteit Nijmegen Netherlands Nationaal Instituut voor Kernfysica en Hoge Energie Fysica Nikhef Netherlands IIHE/ELEM Vrije Universiteit Brussel Pleinlaan 2 Brussels1050 Belgium KarlsruheD-76021 Germany Einstein Fellow Stanford University StanfordCA94305 United States Department of Astronomy University of Maryland College ParkMD20742-2421 United States Joint Space-Science Institute College ParkMD20742-2421 United States Oskar Klein Centre Stockholm University StockholmSE-10691 Sweden Department of Physics Stockholm University StockholmSE-10691 Sweden Univ. Paris Diderot CNRS/IN2P3 CEA/Irfu Obs. de Paris Sorbonne Paris Cité France Institute of High Energy Physics Chinese Academy of Sciences 19B YuquanLu Beijing100049 China National Astronomical Observatories Chinese Ac

The Giant Radio Array for Neutrino Detection (GRAND)1 is a planned large-scale observatory of ultra-high-energy (UHE) cosmic particles — cosmic rays, gamma rays, and neutrinos with energies exceeding 108 GeV. Its ultimate goal is to solve the long-standing mystery of the origin of UHE cosmic rays. It will do so by detecting an unprecedented number of UHECRs and by looking with unmatched sensitivity for the undiscovered UHE neutrinos and gamma rays associated to them. Three key features of GRAND will make this possible: its large exposure at ultra-high energies, sub-degree angular resolution, and sensitivity to the unique signals made by UHE neutrinos. The strategy of GRAND is to detect the radio emission coming from large particle showers that develop in the terrestrial atmosphere — extensive air showers — as a result of the interaction of UHE cosmic rays, gamma, rays, and neutrinos. To achieve this, GRAND will be the largest array of radio antennas ever built. The relative affordability of radio antennas makes the scale of construction possible. GRAND will build on years of progress in the field of radio-detection and apply the large body of technological, theoretical, and numerical advances, for the first time, to the radio-detection of air showers initiated by UHE neutrinos. The design of GRAND will be modular, consisting of several indep.ndent sub-arrays, each of 10 000 radio antennas dep.oyed over 10 000 km2 in radio-quiet locations. A staged construction plan ensures that key techniques are progressively validated, while simultaneously achieving important science goals in UHECR physics, radioastronomy, and cosmology early during construction. Already by 2025, using the first sub-array of 10 000 antennas, GRAND could discover the long-sought cosmogenic neutrinos — produced by interactions of ultra-high-energy cosmic-rays with cosmic photon fields — if their flux is as high as presently allowed, by reaching a sensitivity comparable to planned upgraded versions o

关键词： Gamma rays

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Special Issue on Variable Structure System Control — New Designs and Applications

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Asian Journal of Control 2008年第4期5卷

作者： Prof. Jian-Xin Xu Prof. Leonid Fridman Department of Electrical and Computer Eng. National University of Singapore 4 Engineering Drive 3 Singapore 117576 Tel +65 6874-2566 Fax +65 6779-1103 Dr Jian-Xin Xu received his Bachelor degree from Zhejiang University China in 1982. He attended the University of Tokyo Japan where he received his Master's and Ph.D. degrees in 1986 and 1989 respectively. All his degrees are in Electrical Engineering. He worked for one year in the Hitachi research Laboratory Japan and for more than one year in Ohio State University U.S.A. as a Visiting Scholar. In 1991 he joined the National University of Singapore and is currently an associate professor in the Department of Electrical Engineering. His research interests lie in the fields of learning control variable structure control fuzzy logic control discontinuous signal processing and applications to motion control and process control problems. He is the associate editor of Asian Journal of Control member of TC on variable structure systems and sliding mode control of IEEE Control Systems Society and a senior member of IEEE. He has produced more than 90 peer-refereed journal papers near 160 technical papers in conference proceedings and authored/edited 4 books. Division de Estudios de Posgrado Facultad de Ingenieria National Autonomous University of Mexico DEP-FI UNAM Edificio “A” Circuito Exterior Ciudad Universitaria A. P. 70–256 C.P.04510 Mexico D.F. Mexico Tel +52 55 56223014 Fax +52 55 56161719 Dr. Leonid M. Fridman received his M.S in mathematics from Kuibyshev (Samara) State University Russia Ph.D. in Applied Mathematics from Institute of Control Science (Moscow) and Dr. of Science degrees in Control Science from Moscow State University of Mathematics and Electronics in 1976 1988 and 1998 respectively. In 1976–1999 Dr. Fridman was with the Department of Mathematics at the Samara State Architecture and Civil Engineering Academy Samara Russia. In 2000–2002 he was with the Department of Postgraduate Study and Investigations at the Chihuahu

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TOI-4860 b, a short-period giant planet transiting an M3.5 dwarf

arXiv

引用

arXiv 2023年

作者： Almenara, J.M. Bonfils, X. Bryant, E.M. Jordán, A. Hébrard, G. Martioli, E. Correia, A.C.M. Astudillo-Defru, N. Cadieux, C. Arnold, L. Artigau, É. Bakos, G.Á. Barros, S.C.C. Bayliss, D. Bouchy, F. Boué, G. Brahm, R. Carmona, A. Charbonneau, D. Ciardi, D.R. Cloutier, R. Cointepas, M. Cook, N.J. Cowan, N.B. Delfosse, X. do Nascimento, J. Dias Donati, J.-F. Doyon, R. Forveille, T. Fouqué, P. Gaidos, E. Gilbert, E.A. da Silva, J. Gomes Hartman, J.D. Hesse, K. Hobson, M.J. Jenkins, J.M. Kiefer, F. Kostov, V.B. Laskar, J. Lendl, M. L'Heureux, A. Martins, J.H.C. Menou, K. Moutou, C. Murgas, F. Polanski, A.S. Rapetti, D. Sedaghati, E. Shang, H. Univ. Grenoble Alpes CNRS IPAG GrenobleF-38000 France Observatoire de Genève Département d’Astronomie Université de Genève Chemin Pegasi 51b Versoix1290 Switzerland Mullard Space Science Laboratory University College London Holmbury St Mary Dorking SurreyRH5 6NT United Kingdom Department of Physics University of Warwick Coventry United Kingdom Facultad de Ingeniería y Ciencias Universidad Adolfo Ibáñez Av. Diagonal las Torres 2640 Peñalolén Santiago Chile Santiago Chile Data Observatory Foundation Chile Institut d’astrophysique de Paris UMR7095 CNRS Université Pierre & Marie Curie 98bis boulevard Arago Paris75014 France Observatoire de Haute-Provence CNRS Université d’AixMarseille Saint-Michel-l’Observatoire04870 France Laboratório Nacional de Astrofísica Rua Estados Unidos 154 MG Itajubá37504-364 Brazil CFisUC Departamento de Física Universidade de Coimbra Coimbra3004-516 Portugal IMCCE UMR8028 CNRS Observatoire de Paris PSL University Sorbonne Univ. 77 av. Denfert-Rochereau Paris75014 France Departamento de Matemática y Física Aplicadas Universidad Católica de la Santísima Concepción Alonso de Rivera Concepción2850 Chile Université de Montréal Département de Physique Institut Trottier de Recherche sur les Exoplanètes MontréalQCH3C 3J7 Canada Corporation CNRS UAR2208 65-1238 Mamalahoa Hwy KamuelaHI96743 United States Department of Astrophysical Sciences Princeton University NJ08544 United States Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas Porto4150-762 Portugal Departamento de Fisica e Astronomia Faculdade de Ciencias Universidade do Porto Rua Campo Alegre Porto4169-007 Portugal Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States NASA Exoplanet Science Institute Caltech/IPAC 1200 E. California Blvd PasadenaCA91125 United States Department of Physics & Astronomy McMaster University 1280 Main St W HamiltonONL8S 4L8 Canad

We report the discovery and characterisation of a giant transiting planet orbiting a nearby M3.5V dwarf (d = 80.4 pc, G = 15.1 mag, K=11.2 mag, R• = 0.358 ± 0.015 R, M• = 0.340 ± 0.009 M). Using the photometric time series from TESS sectors 10, 36, 46, and 63 and near-infrared spectrophotometry from ExTrA, we measured a planetary radius of 0.77 ± 0.03 RJ and an orbital period of 1.52 days. With high-resolution spectroscopy taken by the CFHT/SPIRou and ESO/ESPRESSO spectrographs, we refined the host star parameters ([Fe/H] = 0.27 ± 0.12) and measured the mass of the planet (0.273 ± 0.006 MJ). Based on these measurements, TOI-4860 b joins the small set of massive planets (> 80 ME) found around mid to late M dwarfs (J, but additional data would be needed to confirm this. © 2023, CC BY.

关键词： Spectroscopic analysis

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