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arXiv 2018年

作者： Ade, Peter Aguirre, James Ahmed, Zeeshan Aiola, Simone Ali, Aamir Alonso, David Alvarez, Marcelo A. Arnold, Kam Ashton, Peter Austermann, Jason Awan, Humna Baccigalupi, Carlo Baildon, Taylor Barron, Darcy Battaglia, Nick Battye, Richard Baxter, Eric Bazarko, Andrew Beall, James A. Bean, Rachel Beck, Dominic Beckman, Shawn Beringue, Benjamin Bianchini, Federico Boada, Steven Boettger, David Bond, J. Richard Borrill, Julian Brown, Michael L. Bruno, Sarah Marie Bryan, Sean Calabrese, Erminia Calafut, Victoria Calisse, Paolo Carron, Julien Challinor, Anthony Chesmore, Grace Chinone, Yuji Chluba, Jens Cho, Hsiao-Mei Sherry Choi, Steve Coppi, Gabriele Cothard, Nicholas F. Coughlin, Kevin Crichton, Devin Crowley, Kevin D. Crowley, Kevin T. Cukierman, Ari D’Ewart, John M. Dünner, Rolando de Haan, Tijmen Devlin, Mark Dicker, Simon Didier, Joy Dobbs, Matt Dober, Bradley Duell, Cody J. Duff, Shannon Duivenvoorden, Adri Dunkley, Jo Dusatko, John Errard, Josquin Fabbian, Giulio Feeney, Stephen Ferraro, Simone Fluxà, Pedro Freese, Katherine Frisch, Josef C. Frolov, Andrei Fuller, George Fuzia, Brittany Galitzki, Nicholas Gallardo, Patricio A. Ghersi, Jose Tomas Galvez Gao, Jiansong Gawiser, Eric Gerbino, Martina Gluscevic, Vera Goeckner-Wald, Neil Golec, Joseph Gordon, Sam Gralla, Megan Green, Daniel Grigorian, Arpi Groh, John Groppi, Chris Guan, Yilun Gudmundsson, Jon E. Han, Dongwon Hargrave, Peter Hasegawa, Masaya Hasselfield, Matthew Hattori, Makoto Haynes, Victor Hazumi, Masashi He, Yizhou Healy, Erin Henderson, Shawn W. Hervias-Caimapo, Carlos Hill, Charles A. Hill, J. Colin Hilton, Gene Hilton, Matt Hincks, Adam D. Hinshaw, Gary Hložek, Renée Ho, Shirley Ho, Shuay-Pwu Patty Howe, Logan Huang, Zhiqi Hubmayr, Johannes Huffenberger, Kevin Hughes, John P. Ijjas, Anna Ikape, Margaret Irwin, Kent Jaffe, Andrew H. Jain, Bhuvnesh Jeong, Oliver Kaneko, Daisuke Karpel, Ethan D. Katayama, Nobuhiko Keating, Brian Kernasovskiy, Sarah S. Keskitalo, Reijo Kisner, Theodore Kiuchi, Kenji Klein, Jeff Knowles, Kenda Koopman, Brian Kosowsk School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Kavli Institute for Particle Astrophysics and Cosmology Menlo ParkCA94025 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Department of Physics University of California BerkeleyCA94720 United States University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics University of California San Diego CA92093 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States University of Tokyo Kashiwa277- 8583 Japan NIST Quantum Sensors Group 325 Broadway Mailcode 687.08 BoulderCO80305 United States Department of Physics and Astronomy Rutgers State University of New Jersey PiscatawayNJ08854-8019 United States Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste Padriciano 99 Trieste34149 Italy Department of Physics University of Michigan Ann Arbor48103 United States Department of Physics and Astronomy University of New Mexico AlbuquerqueNM87131 United States Department of Astronomy Cornell University IthacaNY14853 United States Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester Manchester United Kingdom AstroParticule et Cosmologie Univ Paris Diderot CNRS/IN2P3 CEA/Irfu Obs de Paris Sorbonne Paris Cité France DAMTP Centre for Mathematical Sciences University of Cambridge Wilberforce Road CambridgeCB3 OWA United Kingdom School of Physics Universi

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 µK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r) = 0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 µK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev–Zel’dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sou

关键词： Tensors

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Symbol Emergence in Cognitive Developmental Systems: A Survey

arXiv

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arXiv 2018年

作者： Taniguchi, Tadahiro Ugur, Emre Hoffmann, Matej Jamone, Lorenzo Nagai, Takayuki Rosman, Benjamin Matsuka, Toshihiko Iwahashi, Naoto Oztop, Erhan Piater, Justus Wörgötter, Florentin College of Information Science and Engineering Ritsumeikan University 1-1-1 Noji Higashi Shiga Kusatsu525-8577 Japan Dept. of Computer Engineering Bogazici University Istanbul Turkey Dept. Cybernetics Faculty of Electrical Engineering Czech Technical University Prague Czech Republic School of Electronic Engineering and Computer Science Queen Mary University of London United Kingdom Faculty of Informatics and Engineering The University of Electro-communications Japan Mobile Intelligent Autonomous Systems The Council for Scientific and Industrial Research The School of Computer Science and Applied Mathematics The University of the Witwatersrand South Africa Department of Cognitive and Information Science Chiba University Japan Faculty of Computer Science and Systems Engineering Okayama Prefectural University Japan Dept. of Computer Science Ozyegin University Istanbul Turkey The Dept. of Computer Science Universität Innsbruck Austria The Department for Computational Neuroscience The Bernstein Center of the University of Göttingen Inst. F. Physics Iii Germany

Humans use signs, e.g., sentences in a spoken language, for communication and thought. Hence, symbol systems like language are crucial for our communication with other agents and adaptation to our real-world environment. The symbol systems we use in our human society adaptively and dynamically change over time. In the context of artificial intelligence (AI) and cognitive systems, the symbol grounding problem has been regarded as one of the central problems related to symbols. However, the symbol grounding problem was originally posed to connect symbolic AI and sensorimotor information and did not consider many interdisciplinary phenomena in human communication and dynamic symbol systems in our society, which semiotics considered. In this paper, we focus on the symbol emergence problem, addressing not only cognitive dynamics but also the dynamics of symbol systems in society, rather than the symbol grounding problem. We first introduce the notion of a symbol in semiotics from the humanities, to leave the very narrow idea of symbols in symbolic AI. Furthermore, over the years, it became more and more clear that symbol emergence has to be regarded as a multifaceted problem. Therefore, secondly, we review the history of the symbol emergence problem in different fields, including both biological and artificial systems, showing their mutual relations. We summarize the discussion and provide an integrative viewpoint and comprehensive overview of symbol emergence in cognitive systems. Additionally, we describe the challenges facing the creation of cognitive systems that can be part of symbol emergence systems. Copyright © 2018, The Authors. All rights reserved.

关键词： Cognitive systems

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Neural physical engines for inferring the halo mass distribution function

arXiv

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arXiv 2019年

作者： Charnock, Tom Lavaux, Guilhem Wandelt, Benjamin D. Boruah, Supranta Sarma Jasche, Jens Hudson, Michael J. Sorbonne Université CNRS UMR 7095 Institut d’Astrophysique de Paris 98 bis boulevard Arago Paris75014 France Sorbonne Universités Institut Lagrange de Paris 98 bis boulevard Arago Paris75014 France Center for Computational Astrophysics Flatiron Institute 162 5th Avenue 10010 New YorkNY United States Dept. of Applied Mathematics University of Waterloo 200 University Avenue West WaterlooONN2L 3G1 Canada Waterloo Centre for Astrophysics University of Waterloo 200 University Avenue West WaterlooONN2L 3G1 Canada The Oskar Klein Centre Department of Physics Stockholm University Albanova University Center StockholmSE 106 91 Sweden Dept. of Physics and Astronomy University of Waterloo 200 University Avenue West WaterlooONN2L 3G1 Canada Perimeter Institute for Theoretical Physics 31 Caroline St N WaterlooONN2L 2Y5 Canada

An ambitious goal in cosmology is to forward-model the observed distribution of galaxies in the nearby Universe today from the initial conditions of large-scale structures. For practical reasons, the spatial resolution at which this can be done is necessarily limited. Consequently, one needs a mapping between the density of dark matter averaged over ~ Mpc scales, and the distribution of dark matter halos (used as a proxy for galaxies) in the same region. Here we demonstrate a method for determining the halo mass distribution function by learning the tracer bias between density fields and halo catalogues using a neural bias model. The method is based on the Bayesian analysis of simple, physically motivated, neural network-like architectures, which we denote as neural physical engines, and neural density estimation. As a result, we are able to sample the initial phases of the dark matter density field whilst inferring the parameters describing the halo mass distribution function, providing a fully Bayesian interpretation of both the initial dark matter density distribution and the neural bias model. We successfully run an upgraded borg inference using our new likelihood and neural bias model with halo catalogues derived from full N-body simulations. We notice orders of magnitude improvement in modelling compared to classical biasing techniques. Copyright © 2019, The Authors. All rights reserved.

关键词： Galaxies

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CEPC Technical Design Report

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Radiation Detection Technology and Methods 2024年第1期8卷 I0003-I0016,1-1091页

作者： Waleed Abdallah Tiago Carlos Adorno de Freitas Konstantin Afanaciev Shakeel Ahmad Ijaz Ahmed Xiaocong Ai Abid Aleem Wolfgang Altmannshofer Fabio Alves Weiming An Rui An Daniele Paolo Anderle Stefan Antusch Yasuo Arai Andrej Arbuzov Abdesslam Arhrib Mustafa Ashry Sha Bai Yu Bai Yang Bai Vipul Bairathi Csaba Balazs Philip Bambade Yong Ban Tripamo Bandyopadhyay Shou-Shan Bao Desmond P.Barber Ayse Bat Varvara Batozskaya Subash Chandra Behera Alexander Belyaev Michele Bertucci Xiao-Jun Bi Yuanjie Bi Tianjian Bian Fabrizio Bianchi Thomas Biekotter Michela Biglietti Shalva Bilanishvili Deng Binglin Denis Bodrov Anton Bogomyagkov Serge Bondarenko Stewart Boogert Maarten Boonekamp Marcello Borri Angelo Bosotti Vincent Boudry Mohammed Boukidi Igor Boyko Ivanka Bozovic Giuseppe Bozzi Jean-Claude Brient Anastasiia Budzinskaya Masroor Bukhari Vladimir Bytev Giacomo Cacciapaglia Hua Cai Wenyong Cai Wujun Cai Yijian Cai Yizhou Cai Yuchen Cai Haiying Cai Huacheng Cai Lorenzo Calibbi Junsong Cang Guofu Cao Jianshe Cao Antoine Chance Xuejun Chang Yue Chang Zhe Chang Xinyuan Chang Wei Chao Auttakit Chatrabhuti Yimin Che Yuzhi Che Bin Chen Danping Chen Fuqing Chen Fusan Chen Gang Chen Guoming Chen Hua-Xing Chen Huirun Chen Jinhui Chen Ji-Yuan Chen Kai Chen Mali Chen Mingjun Chen Mingshui Chen Ning Chen Shanhong Chen Shanzhen Chen Shao-Long Chen Shaomin Chen Shiqiang Chen Tianlu Chen Wei Chen Xiang Chen Xiaoyu Chen Xin Chen Xun Chen Xurong Chen Ye Chen Ying Chen Yukai Chen Zelin Chen Zilin Chen Gang Chen Boping Chen Chunhui Chen Hok Chuen Cheng Huajie Cheng Shan Cheng Tongguang Cheng Yunlong Chi Pietro Chimenti Wen Han Chiu Guk Cho Ming-Chung Chu Xiaotong Chu Ziliang Chu Guglielmo Coloretti Andreas Crivellin Hanhua Cui Xiaohao Cui Zhaoyuan Cui Brunella D'Anzi Ling-Yun Dai Xinchen Dai Xuwen Dai Antonio De Maria Nicola De Filippis Christophe De La Taille Francesca De Mori Chiara De Sio Elisa Del Core Shuangxue Deng Wei-Tian Deng Zhi Deng Ziyan Deng Bhupal Dev Tang Dewen Biagio Di Micco Ran Ding Siqin Dingl Yadong Ding Haiyi Dong Jianin AGH University of Science and Technology Faculty of Physics and Applied Computer ScienceKrakow Anhui University HefeiAnhui Applied Physics Department Federal Urdu University of ArtsScience and TechnologyIslamabad Banaras Hindu University Institute of ScienceVaranasi Bandirma Onyedi Eylul University Bandirma Beihang University Beijing Beijing Computational Science Research Center Beijing Beijing Conveyi LTD Beijing Beijing Glass Research Institute Co. LtdBeijing Beijing Institute of Technology Beijing Beijing Normal University Beijing Brown University ProvidenceRI Budker Institute of Nuclear Physics Novosibirsk Cadi Ayyad University Laboratory of Fundamental and Applied PhysicsPolydisciplinary FacultyMarrakech Cairo University Giza Center for Theory and Computation National Tsing Hua UniversityHsinchu Central China Normal University WuhanHubei Central South University ChangshaHunan Centro de Fisica Teorica de Particulas Universidade Tecnica de LisboaLisboa Chengdu KaitengSifang Digital Radio&TV Equipment Co. LtdChengduSichuan China academy of engineering physics MianyangSichuan China building materials academy Beijing China Center of Advanced Science and Technology Beijing China Institute of Atomic Energy Beijing China Jiliang University HangzhouZhejiang China Nuclear Instrument CO. LTDBeijing China University of Geosciences Beijing China University of Geosciences WuhanHubei China University of Mining and Technology XuzhouJiangsu China West Normal University NanchongSichuan Chongqing University Department of PhysicsChongqing Chulalongkorn University Bangkok City University of Hong Kong Department of PhysicsHong Kong Cockcroft Institute Daresbury Cornell University IthacaNY CPPM(AMU/IPhU&CNRS/INP) Marseille Dalian Minzu University DalianLiaoning Dalian University of Technology Department of PhysicsDalian Deutsches Elektronen-Synchrotron DESY Hamburg Dzhelepov Laboratory of Nuclear Problems of Joint Institute for Nuclear Research(DLNP JINR) Dubna East China University Of Science And Technol

The Circular Electron Positron Collider(CEPC)is a large scientific project initiated and hosted by China,fostered through extensive collaboration with international *** complex comprises four accelerators:a 30 GeV Linac,a 1.1 GeV Damping Ring,a Booster capable of achieving energies up to 180 GeV,and a Collider operating at varying energy modes(Z,W,H,and tt).The Linac and Damping Ring are situated on the surface,while the subterranean Booster and Collider are housed in a 100 km circumference underground tunnel,strategically accommodating future expansion with provisions for a potential Super Proton Proton Collider(SPPC).The CEPC primarily serves as a Higgs *** its baseline design with synchrotron radiation(SR)power of 30 MW per beam,it can achieve a luminosity of 5×10^(34)cm^(-2)s^(-1)per interaction point(IP),resulting in an integrated luminosity of 13 ab^(-1)for two IPs over a decade,producing 2.6 million Higgs *** the SR power to 50 MW per beam expands the CEPC's capability to generate 4.3 million Higgs bosons,facilitating precise measurements of Higgs coupling at sub-percent levels,exceeding the precision expected from the HL-LHC by an order of *** Technical Design Report(TDR)follows the Preliminary Conceptual Design Report(Pre-CDR,2015)and the Conceptual Design Report(CDR,2018),comprehensively detailing the machine's layout,performance metrics,physical design and analysis,technical systems design,R&D and prototyping efforts,and associated civil engineering ***,it includes a cost estimate and a preliminary construction timeline,establishing a framework for forthcoming engineering design phase and site selection *** is anticipated to begin around 2027-2028,pending government approval,with an estimated duration of 8 *** commencement of experiments and data collection could potentially be initiated in the mid-2030s.

关键词： initiated exceeding precise

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Detection of RS Oph with LST-1 and modelling of its HE/VHE gamma-ray emission

arXiv

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arXiv 2025年

作者： Abe, K. Abe, S. Abhishek, A. Acero, F. Aguasca-Cabot, A. Agudo, I. Alispach, C. Crespo, N. Alvarez Ambrosino, D. Antonelli, L.A. Aramo, C. Arbet-Engels, A. Arcaro, C. Asano, K. Aubert, P. Baktash, A. Balbo, M. Bamba, A. Larriva, A. Baquero de Almeida, U. Barres Barrio, J.A. Jiménez, L. Barrios Batkovic, I. Baxter, J. González, J. Becerra Bernardini, E. Bernete, J. Berti, A. Bezshyiko, I. Bhattacharjee, P. Bigongiari, C. Bissaldi, E. Blanch, O. Bonnoli, G. Bordas, P. Borkowski, G. Brunelli, G. Bulgarelli, A. Bunse, M. Burelli, I. Burmistrov, L. Buscemi, M. Cardillo, M. Caroff, S. Carosi, A. Carrasco, M.S. Cassol, F. Castrejón, N. Cerasole, D. Ceribella, G. Chai, Y. Cheng, K. Chiavassa, A. Chikawa, M. Chon, G. Chytka, L. Cicciari, G.M. Cifuentes, A. Contreras, J.L. Cortina, J. Costantini, H. Da Vela, P. Dalchenko, M. Dazzi, F. De Angelis, A. de Bony de Lavergne, M. De Lotto, B. de Menezes, R. Del Burgo, R. Del Peral, L. Delgado, C. Delgado Mengual, J. della Volpe, D. Dellaiera, M. Di Piano, A. Di Pierro, F. Di Tria, R. Di Venere, L. Díaz, C. Dominik, R.M. Dominis Prester, D. Donini, A. Dore, D. Dorner, D. Doro, M. Eisenberger, L. Elsässer, D. Emery, G. Escudero, J. Fallah Ramazani, V. Ferrarotto, F. Fiasson, A. Foffano, L. Freixas Coromina, L. Fröse, S. Fukazawa, Y. Garcia López, R. Gasbarra, C. Gasparrini, D. Geyer, D. Giesbrecht Paiva, J. Giglietto, N. Giordano, F. Gliwny, P. Godinovic, N. Grau, R. Green, D. Green, J. Gunji, S. Günther, P. 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. Iarlori, M. Imazawa, R. Inada, T. Inome, Y. Inoue, S. Ioka, K. Iori, M. Iuliano, A. Jahanvi, J. Jimenez Martinez, I. Jimenez Quiles, J. Jurysek, J. Kagaya, M. Kalashev, O. Karas, V. Katagiri, H. Kataoka, J. Kerszberg, D. Kobayashi, Y. Kohri, K. Kong, A. Kubo, H. Kushida, J. Lacave, B. Lainez, M. Lamanna, G. Lamastra, A. Lemoigne, L. Department of Physics Tokai University 4-1-1 Kita-Kaname Kanagawa Hiratsuka259-1292 Japan Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Chiba Kashiwa277-8582 Japan Sezione di Fisica Via Roma 56 Siena53100 Italy Université Paris-Saclay Université Paris Cité CEA CNRS AIM Gif-sur-YvetteF-91191 Cedex France FSLAC IRL 2009 CNRS/IAC Tenerife La Laguna Spain Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Martí i Franquès 1 Barcelona08028 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain Department of Astronomy University of Geneva Chemin d’Ecogia 16 VersoixCH-1290 Switzerland IPARCOS-UCM Instituto de Física de Partículas y del Cosmos EMFTEL Department Universidad Complutense de Madrid Ciudad Universitaria Plaza de Ciencias 1 Madrid28040 Spain INFN Sezione di Napoli Via Cintia ed. G Napoli80126 Italy INAF - Osservatorio Astronomico di Roma Via di Frascati 33 Monteporzio Catone00040 Italy Max-Planck-Institut für Physik Föhringer Ring 6 München80805 Germany INFN Sezione di Padova Università degli Studi di Padova Via Marzolo 8 Padova35131 Italy Univ. Savoie Mont Blanc CNRS Laboratoire d’Annecy de Physique des Particules - IN2P3 Annecy74000 France Universität Hamburg Institut für Experimentalphysik Luruper Chaussee 149 Hamburg22761 Germany Graduate School of Science University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Faculty of Science and Technology Universidad del Azuay Cuenca Ecuador Centro Brasileiro de Pesquisas Físicas Rua Xavier Sigaud 150 RJ Rio de Janeiro22290-180 Brazil Instituto de Astrofísica de Canarias Departamento de Astrofísica Universidad de La Laguna C. Vía Láctea s/n Santa Cruz de Tenerife La Laguna38205 Spain CIEMAT Avda. Complutense 40 Madrid28040 Spain University of Geneva Département de physique nucléaire et corpusculaire 24 Quai Ernest Ansernet

Context. The recurrent nova RS Ophiuchi (RS Oph) underwent a thermonuclear eruption in August 2021. In this event, RS Oph was detected by the High Energy Stereoscopic System (H.E.S.S.), the Major Atmospheric Gamma Imaging Cherenkov (MAGIC), and the first Large-Sized Telescope (LST-1) of the future Cherenkov Telescope Array Observatory (CTAO) at very-high gamma-ray energies above 100 GeV. This means that novae are a new class of very-high-energy (VHE) gamma-ray emitters. Aims. We report the analysis of the RS Oph observations with LST-1. We constrain the particle population that causes the observed emission in hadronic and leptonic scenarios. Additionally, we study the prospects of detecting further novae using LST-1 and the upcoming LST array of CTAO-North. Methods. We conducted target-of-opportunity observations with LST-1 from the first day of this nova event. The data were analysed in the framework of cta-lstchain and Gammapy, the official CTAO-LST reconstruction and analysis packages. One-zone hadronic and leptonic models were considered to model the gamma-ray emission of RS Oph using the spectral information from Fermi-LAT and LST-1, together with public data from the MAGIC and H.E.S.S. telescopes. Results. RS Oph was detected at 6.6σ with LST-1 in the first 6.35 hours of observations following the eruption. The hadronic scenario is preferred over the leptonic scenario considering a proton energy spectrum with a power-law model with an exponential cutoff whose position increases from (0.26 ± 0.08) TeV on day 1 up to (1.6 ± 0.6) TeV on day 4 after the eruption. The deep sensitivity and low energy threshold of the LST-1/LST array will allow us to detect faint novae and increase their discovery rate. © 2025, CC BY.

关键词： Gamma radiography

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Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam

arXiv

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arXiv 2019年

作者： Namikawa, T. Chinone, Y. Miyatake, H. Oguri, M. Takahashi, R. Kusaka, A. Katayama, N. Adachi, S. Aguilar, M. Aihara, H. Ali, A. Armstrong, R. Arnold, K. Baccigalupi, C. Barron, D. Beck, D. Beckman, S. Bianchini, F. Boettger, D. Borrill, J. Cheung, K. Corbett, L. Crowley, K.T. El Bouhargani, H. Elleflot, T. Errard, J. Fabbian, G. Feng, C. Galitzki, N. Goeckner-Wald, N. Groh, J. Hamada, T. Hasegawa, M. Hazumi, M. Hill, C.A. Howe, L. Jeong, O. Kaneko, D. Keating, B. Lee, A.T. Leon, D. Linder, E. Lowry, L.N. Mangu, A. Matsuda, F. Minami, Y. Miyazaki, S. Murayama, H. Navaroli, M. Nishino, H. Nishizawa, A.J. Pham, A.T.P. Poletti, D. Puglisi, G. Reichardt, C.L. Sherwin, B.D. Silva-Feaver, M. Siritanasak, P. Speagle, J.S. Stompor, R. Suzuki, A. Tait, P.J. Tajima, O. Takada, M. Takakura, S. Takatori, S. Tanabe, D. Tanaka, M. Teply, G.P. Tsai, C. Vergés, C. Westbrook, B. Zhou, Y. Department of Applied Mathematics and Theoretical Physics University of Cambridge CambridgeCB3 0WA United Kingdom Department of Physics University of California BerkeleyCA94720 United States UTIAS University of Tokyo KashiwaChiba277-8583 Japan Berkeley Satellite University of California Berkeley94720 United States Institite for Advanced Research Nagoya University Nagoya Aichi464-8601 Japan Division of Particle and Astrophysical Science Graduate School of Science Nagoya University Nagoya Aichi464-8602 Japan Department of Physics University of Tokyo Tokyo113-0033 Japan Research Center for the Early Universe School of Science University of Tokyo Bunkyo-ku Tokyo113-0033 Japan Faculty of Science and Technology Hirosaki University 3 Bunkyo-cho Hirosaki Aomori036-8588 Japan Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics Kyoto University Kyoto606-8502 Japan Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Departamento de Física FCFM Universidad de Chile Blanco Encalada 2008 Santiago Chile Lawrence Livermore National Laboratory LivermoreCA94551 United States Department of Physics University of California San DiegoCA92093-0424 United States Via Bonomea 265 Trieste34136 Italy 34151 Italy National Institute for Nuclear Physics INFN Sezione di Trieste Via Valerio 2 TriesteI-34127 Italy Department of Physics and Astronomy University of New Mexico AlbuquerqueNM87131 United States Univ Paris Diderot CNRS/IN2P3 CEA/Irfu Obs de Paris Sorbonne Paris Cité France School of Physics University of Melbourne ParkvilleVIC3010 Australia Instituto de Astrofísica Centro de Astro-Ingeniería Facultad de Física Pontificia Universidad Católica de Chile Av. Vicuña Mackenna 4860 Macul Santiago7820436 Chile Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Space Sciences Laboratory

We present the first measurement of cross-correlation between the lensing potential, reconstructed from cosmic microwave background (CMB) polarization data, and the cosmic shear field from galaxy shapes. This measurement is made using data from the Polarbear CMB experiment and the Subaru Hyper Suprime-Cam (HSC) survey. By analyzing an 11 deg2 overlapping region, we reject the null hypothesis at 3.5σ and constrain the amplitude of the cross-spectrum to Ablens = 1.70 ± 0.48, where Ablens is the amplitude normalized with respect to the Planck 2018 prediction, based on the flat Λ cold dark matter cosmology. The first measurement of this cross-spectrum without relying on CMB temperature measurements is possible due to the deep Polarbear map with a noise level of ∼6 µKarcmin, as well as the deep HSC data with a high galaxy number density of ng = 23 arcmin−2. We present a detailed study of the systematics budget to show that residual systematics in our results are negligibly small, which demonstrates the future potential of this cross-correlation technique. Copyright © 2019, The Authors. All rights reserved.

关键词： Temperature measurement

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Traceable random numbers from a nonlocal quantum advantage

arXiv

引用

arXiv 2024年

作者： Kavuri, Gautam A. Palfree, Jasper Reddy, Dileep V. Zhang, Yanbao Bienfang, Joshua C. Mazurek, Michael D. Alhejji, Mohammad A. Siddiqui, Aliza U. Cavanagh, Joseph M. Dalal, Aagam Abellán, Carlos Amaya, Waldimar Mitchell, Morgan W. Stange, Katherine E. Beale, Paul D. Brandão, Luís T.A.N. Booth, Harold Peralta, René Nam, Sae Woo Mirin, Richard P. Stevens, Martin J. Knill, Emanuel Shalm, Lynden K. Department of Physics University of Colorado BoulderCO80309 United States The National Institute of Standards and Technology BoulderCO80305 United States Quantum Information Science Section Computational Sciences and Engineering Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Joint Quantum Institute National Institute of Standards and Technology University of Maryland 100 Bureau Drive GaithersburgMD20899 United States Center for Quantum Information and Control University of New Mexico AlbuquerqueNM87131 United States Department of Electrical Computer and Energy Engineering University of Colorado BoulderCO80309 United States Physical Measurement Laboratory National Institute of Standards and Technology GaithersburgMD20899 United States Quside Technologies S.L. Castelldefels Barcelona Spain ICFO-Institut de Ciencies Fotoniques The Barcelona Institute of Science and Technology Castelldefels Barcelona08860 Spain ICREA - Institució Catalana de Recerca i Estudis Avançats Barcelona08010 Spain Department of Mathematics University of Colorado BoulderCO80309 United States GaithersburgMD20899 United States Information Technology Laboratory National Institute of Standards and Technology GaithersburgMD20899 United States Physical Measurement Laboratory National Institute of Standards and Technology BoulderCO80305 United States Center for Theory of Quantum Matter University of Colorado BoulderCO80305 United States Applied and Computational Mathematics Division National Institute of Standards and Technology BoulderCO80305 United States Quantum Engineering Initiative Department of Electrical Computer and Energy Engineering University of Colorado BoulderCO80309 United States

The unpredictability of random numbers is fundamental to both digital security [1, 2] and applications that fairly distribute resources [3, 4]. However, existing random number generators have limitations—the generation processes cannot be fully traced, audited, and certified to be unpredictable. The algorithmic steps used in pseudorandom number generators [5] are auditable, but they cannot guarantee that their outputs were a priori unpredictable given knowledge of the initial seed. Device-independent quantum random number generators [6–9] can ensure that the source of randomness was unknown beforehand, but the steps used to extract the randomness are vulnerable to tampering. Here, for the first time, we demonstrate a fully traceable random number generation protocol based on device-independent techniques. Our protocol extracts randomness from unpredictable non-local quantum correlations, and uses distributed intertwined hash chains to cryptographically trace and verify the extraction process. This protocol is at the heart of a public traceable and certifiable quantum randomness beacon that we have launched [10]. Over the first 40 days of operation, we completed the protocol 7434 out of 7454 attempts—a success rate of 99.7%. Each time the protocol succeeded, the beacon emitted a pulse of 512 bits of traceable randomness. The bits are certified to be uniform with error times actual success probability bounded by 2−64. The generation of certifiable and traceable randomness represents one of the first public services that operates with an entanglement-derived advantage over comparable classical approaches. Copyright © 2024, The Authors. All rights reserved.

关键词： Random number generation

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A light in the dark: searching for electromagnetic counterparts to black hole-black hole mergers in LIGO/Virgo O3 with the Zwicky Transient Facility

arXiv

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arXiv 2022年

作者： Graham, Matthew J. McKernan, Barry Ford, K.E. Saavik Stern, Daniel Djorgovski, S.G. Coughlin, Michael Burdge, Kevin B. Bellm, Eric C. Helou, George Mahabal, Ashish A. Masci, Frank J. Purdum, Josiah Rosnet, Philippe Rusholme, Ben California Institute of Technology 1200 E. California Blvd PasadenaCA91125 United States Department of Science CUNY Borough of Manhattan Community College 199 Chambers Street New YorkNY10007 United States Department of Astrophysics American Museum of Natural History Central Park West New YorkNY10028 United States Physics Program CUNY Graduate Center 365 5th Avenue New YorkNY10016 United States Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Department of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States DIRAC Institute Department of Astronomy University of Washington 3910 15th Avenue NE SeattleWA98195 United States IPAC California Institute of Technology 1200 E. California Blvd PasadenaCA91125 United States Division of Physics Mathematics and Astronomy California Institute of Technology PasadenaCA91125 United States Center for Data Driven Discovery California Institute of Technology PasadenaCA91125 United States Caltech Optical Observatories California Institute of Technology PasadenaCA91125 United States Université Clermont Auvergne CNRS IN2P3 LPC Clermont-FerrandF-63000 France

The accretion disks of active galactic nuclei (AGN) are promising locations for the merger of compact objects detected by gravitational wave (GW) observatories. Embedded within a baryon-rich, high density environment, mergers within AGN are the only GW channel where an electromagnetic (EM) counterpart must occur (whether detectable or not). Considering AGN with unusual flaring activity observed by the Zwicky Transient Facility (ZTF), we describe a search for candidate EM counterparts to binary black hole (BBH) mergers detected by LIGO/Virgo in O3. After removing probable false positives, we find nine candidate counterparts to BBH mergers during O3 (seven in O3a, two in O3b) with a p-value of 0.0019. Based on ZTF sky coverage, AGN geometry, and merger geometry, we expect ≈ 3(NBBH/83)(fAGN/0.5) potentially detectable EM counterparts from O3, where NBBH is the total number of observed BBH mergers and fAGN is the fraction originating in AGN. Further modeling of breakout and flaring phenomena in AGN disks is required to reduce our false positive rate. Two of the events are also associated with mergers with total masses > 100M☉, which is the expected rate for O3 if hierarchical (large mass) mergers occur in the AGN channel. Candidate EM counterparts in future GW observing runs can be better constrained by coverage of the Southern sky as well as spectral monitoring of unusual AGN flaring events in LIGO/Virgo alert volumes. A future set of reliable AGN EM counterparts to BBH mergers will yield an independent means of measuring cosmic expansion (H0) as a function of redshift. © 2022, CC BY.

关键词： Gravity waves

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Light, the universe, and everything-12 Herculean tasks for quantum cowboys and black diamond skiers

arXiv

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arXiv 2018年

作者： Agarwal, Girish Allen, Roland E. Bezdìková, Iva Boyd, Robert W. Chen, Goong Hanson, Ronald Hawthorne, Dean L. Hemmer, Philip Kim, Moochan B. Kocharovskaya, Olga Lee, David M. Lidström, Sebastian K. Lidström, Suzy Losert, Harald Maier, Helmut Neuberger, John W. Padgett, Miles J. Raizen, Mark Rajendran, Surjeet Rasel, Ernst Schleich, Wolfgang P. Scully, Marlan O. Shchedrin, Gavriil Shvets, Gennady Sokolov, Alexei Svidzinsky, Anatoly Walsworth, Ronald L. Weiss, Rainer Wilczek, Frank Willner, Alan E. Yablonovich, Eli Zheludev, Nikolay Department of Physics and Astronomy Texas A&M University College StationTX77843 United States Department of Physics Faculty of Nuclear Sciences and Physical Engineering Czech Technical University in Prague Brehova 7 Praha 1-Staré mìsto11519 Czech Republic Department of Physics Technical University of Ostrava 17 Listopadu 15 Ostrava-Poruba70833 Czech Republic Department of Physics School of Electrical Engineering and Computer Science University of Ottawa OttawaONK1N6N5 Canada Institute of Optics Department of Physics and Astronomy University of Rochester RochesterNY14627 United States School of Physics and Astronomy University of Glasgow GlasgowG128QQ United Kingdom Department of Mathematics Texas A&M University College StationTX77843 United States Science Program Texas A&M University at Qatar Education City Doha Qatar Texas A&M University College StationTX77843 United States QuTech and Kavli Institute of Nanoscience Delft University of Technology P.O. Box 5046 Delft2600 GA Netherlands Cornell Laboratory of Ornithology Cornell University IthacaNY14850 United States Laboratory of Atomic and Solid State Physics Cornell University IthacaNY14853 United States Department of Electrical & Computer Engineering Texas A&M Energy Institute Texas A&M University TX77843 United States Department of Physics Strathclyde University GlasgowG11XJ United Kingdom Physica Scripta Royal Swedish Academy of Sciences StockholmSE-10405 Sweden Universität Ulm Albert-Einstein-Allee 11 Ulm89081 Germany Institut für Zahlentheorie und Wahrscheinlichkeitstheorie Universität Ulm Albert-Einstein-Allee 11 Ulm89081 Germany Department of Mathematics University of North Texas DentonTX76203-5017 United States College of Natural Sciences University of Texas AustinTX78712 United States Department of Physics University of California BerkeleyCA94720-7300 United States Institut fuer Quantenoptik QUEST-LFS Welfengarten 1 Hannover30167 Germany Hagler Insti

The Winter Colloquium on the physics of Quantum Electronics (PQE) has been a seminal force in quantum optics and related areas since 1971. It is rather mindboggling to recognize how the concepts presented at these conferences have transformed scientific understanding and human society. In January, 2017, the participants of PQE were asked to consider the equally important prospects for the future, and to formulate a set of questions representing some of the greatest aspirations in this broad field. The result is this multi-authored paper, in which many of the world's leading experts address the following fundamental questions: (1) What is the future of gravitational wave astronomy? (2) Are there new quantum phases of matter away from equilibrium that can be found and exploited-such as the time crystal? (3) Quantum theory in uncharted territory: What can we learn? (4) What are the ultimate limits for laser photon energies? (5) What are the ultimate limits to temporal, spatial, and optical resolution? (6) What novel roles will atoms play in technology? (7) What applications lie ahead for nitrogen-vacancy centers in diamond? (8) What is the future of quantum coherence, squeezing, and entanglement for enhanced superresolution and sensing? (9) How can we solve (some of) humanity's biggest problems through new quantum technologies? (10) What new understanding of materials and biological molecules will result from their dynamical characterization with free electron lasers? (11) What new technologies and fundamental discoveries might quantum optics achieve by the end of this century? (12) What novel topological structures can be created and employed in quantum optics? Copyright © 2018, The Authors. All rights reserved.

关键词： Quantum optics

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Full Dissolution of the Whole Lithium Sulfide Family (Li2S8to Li2S) in a Safe Eutectic Solvent for Rechargeable Lithium–Sulfur Batteries

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Angewandte Chemie 2019年第17期131卷

作者： Qian Cheng Weiheng Xu Shiyi Qin Subhabrata Das Tianwei Jin Aijun Li Alex Ceng Li Boyu Qie Pengcheng Yao Haowei Zhai Changmin Shi Xin Yong Yuan Yang Program of Materials Science and Engineering Department of Applied Physics and Applied Mathematics Columbia University 500 W 120th St New York NY 10027 USA Department of Mechanical Engineering The State University of New York Binghamton 85 Murray Hill Rd. Suite 1300 Rm#1320 Binghamton NY 13902 USA Langmuir Center of Colloids and Interfaces Columbia University 500 W 120th St New York NY 10027 USA

The lithium–sulfur battery is an attractive option for next‐generation energy storage owing to its much higher theoretical energy density than state‐of‐the‐art lithium‐ion batteries. However, the massive volume changes of the sulfur cathode and the uncontrollable deposition of Li 2 S 2 /Li 2 S significantly deteriorate cycling life and increase voltage polarization. To address these challenges, we develop an ϵ‐caprolactam/acetamide based eutectic‐solvent electrolyte, which can dissolve all lithium polysulfides and lithium sulfide (Li 2 S 8 –Li 2 S). With this new electrolyte, high specific capacity (1360 mAh g −1 ) and reasonable cycling stability are achieved. Moreover, in contrast to conventional ether electrolyte with a low flash point (ca. 2 °C), such low‐cost eutectic‐solvent‐based electrolyte is difficult to ignite, and thus can dramatically enhance battery safety. This research provides a new approach to improving lithium–sulfur batteries in aspects of both safety and performance.

关键词： Elektrolyte Eutektische Lösungsmittel Feuerschutzmittel Lithium-Schwefel-Batterien Sicherheit

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