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arXiv 2020年

作者： Aiola, Simone Calabrese, Erminia Maurin, Loïc Naess, Sigurd Schmitt, Benjamin L. Abitbol, Maximilian H. Addison, Graeme E. Ade, Peter A.R. Alonso, David Amiri, Mandana Amodeo, Stefania Angile, Elio Austermann, Jason E. Baildon, Taylor Battaglia, Nick Beall, James A. Bean, Rachel Becker, Daniel T. Bond, J. Richard Bruno, Sarah Marie Calafut, Victoria Campusano, Luis E. Carrero, Felipe Chesmore, Grace E. Cho, Hsiao-Mei Choi, Steve K. Clark, Susan E. Cothard, Nicholas F. Crichton, Devin Crowley, Kevin T. Darwish, Omar Datta, Rahul Denison, Edward V. Devlin, Mark J. Duell, Cody J. Duff, Shannon M. Duivenvoorden, Adriaan J. Dunkley, Jo Dünner, Rolando Essinger-Hileman, Thomas Fankhanel, Max Ferraro, Simone Fox, Anna E. Fuzia, Brittany Gallardo, Patricio A. Gluscevic, Vera Golec, Joseph E. Grace, Emily Gralla, Megan Guan, Yilun Hall, Kirsten Halpern, Mark Han, Dongwon Hargrave, Peter Hasselfield, Matthew Helton, Jakob M. Henderson, Shawn Hensley, Brandon Hill, J. Colin Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hložek, Renée Ho, Shuay-Pwu Patty Hubmayr, Johannes Huffenberger, Kevin M. Hughes, John P. Infante, Leopoldo Irwin, Kent Jackson, Rebecca Klein, Jeff Knowles, Kenda Koopman, Brian Kosowsky, Arthur Lakey, Victoria Li, Dale Li, Yaqiong Li, Zack Lokken, Martine Louis, Thibaut Lungu, Marius MacInnis, Amanda Madhavacheril, Mathew Maldonado, Felipe Mallaby-Kay, Maya Marsden, Danica McMahon, Jeff Menanteau, Felipe Moodley, Kavilan Morton, Tim Namikawa, Toshiya Nati, Federico Newburgh, Laura Nibarger, John P. Nicola, Andrina Niemack, Michael D. Nolta, Michael R. Orlowski-Sherer, John Page, Lyman A. Pappas, Christine G. Partridge, Bruce Phakathi, Phumlani Pisano, Giampaolo Prince, Heather Puddu, Roberto Qu, Frank J. Rivera, Jesus Robertson, Naomi Rojas, Felipe Salatino, Maria Schaan, Emmanuel Schillaci, Alessandro Sehgal, Neelima Sherwin, Blake D. Sierra, Carlos Sievers, Jon Sifon, Cristobal Sikhosana, Precious Simon, Sara Spergel, David N. Staggs, Suzanne T. Stevens, Jason Storer, Emilie Sunder, Dhaneshwar D. Switzer, Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States School of Physics and Astronomy Cardiff University The Parade Wales CardiffCF24 3AA United Kingdom Université Paris-Saclay CNRS Institut d'astrophysique spatiale Orsay 91405 France Instituto de Astrofísica Centro de Astro-Ingeniería Facultad de Fìsica Pontificia Universidad Católica de Chile Av. Vicuña Mackenna 4860 Macul Santiago7820436 Chile Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Dept. of Physics and Astronomy The Johns Hopkins University 3400 N. Charles St. BaltimoreMD21218-2686 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada Department of Astronomy Cornell University IthacaNY14853 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Michigan Ann Arbor48103 United States Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada Universidad de Chile Dept Astronomía Casilla Santiago36-D Chile Sociedad Radiosky Asesorías de Ingeniería Limitada Camino a Toconao 145-A Ayllu de Solor San Pedro de Atacama Chile Department of Physics University of Chicago ChicagoIL60637 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Department of Physics Cornell University IthacaNY14853 United States Institute for Advanced Study 1 Einstein Dr PrincetonNJ08540 United States Department of Applied and Engineering Physics Cornell University IthacaNY14853 United States Astrophysics Research Centre School of Mathematics Statistics and Computer Scie

We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013-2016 at 98 and 150 GHz. The maps cover more than 17,000 deg2, the deepest 600 deg2 with noise levels below 10µK-arcmin. We use the power spectrum derived from almost 6,000 deg2 of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, H0. By combining ACT data with large-scale information from WMAP we measure H0 = 67.6±1.1 km/s/Mpc, at 68% confidence, in excellent agreement with the independently-measured Planck satellite estimate (from ACT alone we find H0 = 67.9 ±1.5 km/s/Mpc). The ΛCDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1σ;the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with ΛCDM predictions to within 1.5-2.2σ. We compare ACT, WMAP, and Planck at the parameter level and find good consistency;we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis. Copyright © 2020, The Authors. All rights reserved.

关键词： Cosmology

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The Atacama Cosmology Telescope: A measurement of the cosmic microwave background power spectra at 98 and 150 GHZ

arXiv

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arXiv 2020年

作者： Choi, Steve K. Hasselfield, Matthew Ho, Shuay-Pwu Patty Koopman, Brian Lungu, Marius Abitbol, Maximilian H. Addison, Graeme E. Ade, Peter A.R. Aiola, Simone Alonso, David Amiri, Mandana Amodeo, Stefania Angile, Elio Austermann, Jason E. Baildon, Taylor Battaglia, Nick Beall, James A. Bean, Rachel Becker, Daniel T. Bond, J. Richard Bruno, Sarah Marie Calabrese, Erminia Calafut, Victoria Campusano, Luis E. Carrero, Felipe Chesmore, Grace E. Cho, Hsiao-Mei Clark, Susan E. Cothard, Nicholas F. Crichton, Devin Crowley, Kevin T. Darwish, Omar Datta, Rahul Denison, Edward V. Devlin, Mark J. Duell, Cody J. Duff, Shannon M. Duivenvoorden, Adriaan J. Dunkley, Jo Dünner, Rolando Essinger-Hileman, Thomas Fankhanel, Max Ferraro, Simone Fox, Anna E. Fuzia, Brittany Gallardo, Patricio A. Gluscevic, Vera Golec, Joseph E. Grace, Emily Gralla, Megan Guan, Yilun Hall, Kirsten Halpern, Mark Han, Dongwon Hargrave, Peter Henderson, Shawn Hensley, Brandon Hill, J. Colin Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hložek, Renée Hubmayr, Johannes Huffenberger, Kevin M. Hughes, John P. Infante, Leopoldo Irwin, Kent Jackson, Rebecca Klein, Jeff Knowles, Kenda Kosowsky, Arthur Lakey, Victoria Li, Dale Li, Yaqiong Li, Zack Lokken, Martine Louis, Thibaut MacInnis, Amanda Madhavacheril, Mathew Maldonado, Felipe Mallaby-Kay, Maya Marsden, Danica Maurin, Loïc McMahon, Jeff Menanteau, Felipe Moodley, Kavilan Morton, Tim Naess, Sigurd Namikawa, Toshiya Nati, Federico Newburgh, Laura Nibarger, John P. Nicola, Andrina Niemack, Michael D. Nolta, Michael R. Orlowski-Sherer, John Page, Lyman A. Pappas, Christine G. Partridge, Bruce Phakathi, Phumlani Prince, Heather Puddu, Roberto Qu, Frank J. Rivera, Jesus Robertson, Naomi Rojas, Felipe Salatino, Maria Schaan, Emmanuel Schillaci, Alessandro Schmitt, Benjamin L. Sehgal, Neelima Sherwin, Blake D. Sierra, Carlos Sievers, Jon Sifon, Cristobal Sikhosana, Precious Simon, Sara Spergel, David N. Staggs, Suzanne T. Stevens, Jason Storer, Emilie Sunder, Dhaneshwar D. Switzer, Eric R. Thorne, Ben Thornton, Robe Department of Physics Cornell University IthacaNY14853 United States Department of Astronomy Cornell University IthacaNY14853 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 Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics Yale University 217 Prospect St New HavenCT06511 United States Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Dept. of Physics and Astronomy The Johns Hopkins University 3400 N. Charles St. BaltimoreMD21218-2686 United States School of Physics and Astronomy Cardiff University The Parade Wales CardiffCF24 3AA United Kingdom Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Michigan Ann Arbor48103 United States Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada Universidad de Chile Dept Astronomía Casilla Santiago36-D Chile Sociedad Radiosky Asesorías de Ingeniería Limitada Camino a Toconao 145-A Ayllu de Solor San Pedro de Atacama Chile Department of Physics University of Chicago ChicagoIL60637 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Institute for Advanced Study 1 Einstein Dr PrincetonNJ08540 United States Department of Applied and Engineering Physics Cornell University IthacaNY14853 United States Astrophysics Res

We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg2 of the 2013-2016 survey, which covers >15000 deg2 at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the likelihood for the cosmological analysis we constrain secondary sources of anisotropy and foreground emission, and derive a "CMB-only" spectrum that extends to = 4000. At large angular scales, foreground emission at 150 GHz is ∼1% of TT and EE within our selected regions and consistent with that found by Planck. Using the same likelihood, we obtain the cosmological parameters for ΛCDM for the ACT data alone with a prior on the optical depth of τ = 0.065 ± 0.015. ΛCDM is a good fit. The best-fit model has a reduced χ2 of 1.07 (PTE = 0.07) with H0 = 67.9 ± 1.5 km/s/Mpc. We show that the lensing BB signal is consistent with ΛCDM and limit the celestial EB polarization angle to ψP = −0.07◦ ± 0.09◦. We directly cross correlate ACT with Planck and observe generally good agreement but with some discrepancies in TE. All data on which this analysis is based will be publicly released. Copyright © 2020, The Authors. All rights reserved.

关键词： Cosmology

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Free-energy landscapes of DNA and its assemblies: Perspectives from coarse-grained modelling

arXiv

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arXiv 2021年

作者： Doye, Jonathan P.K. Louis, Ard A. Schreck, John S. Romano, Flavio Harrison, Ryan M. Mosayebi, Majid Engel, Megan C. Ouldridge, Thomas E. Physical and Theoretical Chemistry Laboratory Department of Chemistry University of Oxford OxfordOX1 3QZ United Kingdom Rudolf Peierls Centre for Theoretical Physics University of Oxford Parks Road OxfordOX1 3PU United Kingdom National Center for Atmospheric Research Computational and Information Systems Laboratory 850 Table Mesa Drive BoulderCO80305 United States Dipartimento di Scienze Molecolari e Nanosistemi Università Ca' Foscari di Venezia via Torino 155 Venezia Mestre30170 Italy School of Mathematics University of Bristol BristolBS8 1QU United Kingdom School of Engineering and Applied Sciences Harvard University 29 Oxford Street CambridgeMA02138 United States Department of Bioengineering and Centre for Synthetic Biology Imperial College London LondonSW7 2AZ United Kingdom

This chapter will provide an overview of how characterizing free-energy landscapes can provide insights into the biophysical properties of DNA, as well as into the behaviour of the DNA assemblies used in the field of DNA nanotechnology. The landscapes for these complex systems are accessible through the use of accurate coarse-grained descriptions of DNA. Particular foci will be the landscapes associated with DNA self-assembly and mechanical deformation, where the latter can arise from either externally imposed forces or internal stresses. © 2021, CC BY.

关键词： DNA

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THE SIMONS OBSERVATORY: SCIENCE GOALS AND FORECASTS

arXiv

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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

引用

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

引用

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

引用

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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