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Erratum to “Chemical and biological activity in open flows: a dynamical system approach”

physics Reports 2005年第5-6期415卷 360-360页

作者： Tamás Tél Alessandro de Moura Celso Grebogi György Károlyi Institute for Theoretical Physics Eötvös University P.O. Box 32 H-1518 Budapest Hungary Instituto de Física Universidade de São Paulo Caixa Postal 66318 05315-970 São Paulo SP Brazil Max-Plank-Institute for the Physics of Complex Systems Nöthnitzer Str. 38 D-01187 Dresden Germany Center for Applied Mathematics and Computational Physics and Department of Structural Mechanics Budapest University of Technology and Economics Müegyetem rkp. 3 H-1521 Budapest Hungary

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Fundamental physics with the square kilometre array

arXiv

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arXiv 2018年

作者： Weltman, A. Bull, P. Camera, S. Kelley, K. Padmanabhan, H. Pritchard, J. Racanelli, A. Riemer-Sørensen, S. Shao, L. Andrianomena, S. Athanassoula, E. Bacon, D. Barkana, R. Bertone, G. Bonvin, C. Bosma, A. Brüggen, M. Burigana, C. Bœhm, C. Calore, F. Cembranos, J.A.R. Clarkson, C. Connors, R.M.T. de la Cruz-Dombriz, Á. Dunsby, P.K.S. Fonseca, J. Fornengo, N. Gaggero, D. Harrison, I. Larena, J. Ma, Y.-Z. Maartens, R. Méndez-Isla, M. Mohanty, S.D. Murray, S.G. Parkinson, D. Pourtsidou, A. Quinn, P. Regis, M. Saha, P. Sahlén, M. Sakellariadou, M. Silk, J. Trombetti, T. Vazza, F. Venumadhav, T. Vidotto, F. Villaescusa-Navarro, F. Wang, Y. Weniger, C. Wolz, L. Zhang, F. Gaensler, B.M. Department of Mathematics & Applied Mathematics University of Cape Town 7701 Rondebosch Cape Town South Africa Department of Astronomy University of California Berkeley BerkeleyCA94720 United States Dipartimento di Fisica Università degli Studi di Torino INFN Sezione di Torino INAF – Istituto Nazionale di Astrofisica Via P. Giuria 1 Torino10125 Italy University of Western Australia Ken and Julie Michael Building 7 Fairway CrawleyWA6009 Australia ETH Zurich Wolfgang-Pauli-Strasse 27 ZurichCH 8093 Switzerland Department of Physics Imperial College London Prince Consort Road LondonSW7 2AZ United Kingdom Martí Franquès 1 BarcelonaE08028 Spain Institute of Theoretical Astrophysics University of Oslo P.O. Box 1029 Blindern OsloN-0315 Norway Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China The Park Park Road Cape Town7405 South Africa Aix Marseille Univ CNRS CNES LAM Marseille France Institute of Cosmology & Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel GRAPPA Institute of Physics University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands School of Physics University of Sydney NSW Australia 2006 Australia Département de Physique Théorique Center for Astroparticle Physics Université de Genève Genève 41211 Switzerland Aix Marseille Univ CNRS CNES LAM Marseille France University of Hamburg Gojenbergsweg 112 Hamburg21029 Germany INAF Istituto di Radioastronomia Via Piero Gobetti 101 BolognaI-40129 Italy GRAPPA Institute of Physics University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Departamento de Física Teórica I and UPARCOS Universidad Complutense de Madrid MadridE-28040 Spain School of Physics & Astronomy Queen Mary University of London LondonE1 4NS United Kingdom Cahill Center for Astronomy and Astrophysics California Instit

The Square Kilometre Array (SKA) is a planned large radio interferometer designed to operate over a wide range of frequencies, and with an order of magnitude greater sensitivity and survey speed than any current radio telescope. The SKA will address many important topics in astronomy, ranging from planet formation to distant galaxies. However, in this work, we consider the perspective of the SKA as a facility for studying physics. We review four areas in which the SKA is expected to make major contributions to our understanding of fundamental physics: cosmic dawn and reionisation;gravity and gravitational radiation;cosmology and dark energy;and dark matter and astroparticle physics. These discussions demonstrate that the SKA will be a spectacular physics machine, which will provide many new breakthroughs and novel insights on matter, energy and spacetime. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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Dynamics of nanosecond laser pulse propagation and of associated instabilities in a magnetized underdense plasma

arXiv

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arXiv 2022年

作者： Yao, W. Higginson, A. Marquès, J.-R. Antici, P. Béard, J. Burdonov, K. Borghesi, M. Castan, A. Ciardi, A. Coleman, B. Chen, S.N. D'Humières, E. Gangolf, T. Gremillet, L. Khiar, B. Lancia, L. Loiseau, P. Ribeyre, X. Soloviev, A. Starodubtsev, M. Wang, Q. Fuchs, J. Luli Cnrs Cea Upmc Univ Paris 06 : Sorbonne Université Ecole Polytechnique Institut Polytechnique de Paris PalaiseauF-91128 cedex France Sorbonne Université Observatoire de Paris Université Psl CNRS Lerma ParisF-75005 France Center for Energy Research University of California San Diego 9500 Gilman Drive La Jolla CA92093-0417 United States INRS-EMT 1650 boul Lionel-Boulet VarennesQCJ3X 1S2 Canada Cnrs Lncmi Univ Toulouse 3 Insa Toulouse Univ Grenoble Alpes Emfl Toulouse31400 France Jiht Russian Academy of Sciences Moscow125412 Russia School of Mathematics and Physics The Queen's University Belfast Belfast United Kingdom Cea Dam Dif F-91297 France 'Horia Hulubei' National Institute for Physics and Nuclear Engineering Bucharest-MagureleRO-077125 Romania University of Bordeaux Celia Cnrs Cea Umr 5107 TalenceF-33405 France Université Paris-Saclay Cea Lmce Bruyères-le-Châtel91680 France Palaiseau91123 France IAP-RAS Nizhny Novgorod Russia Institute of Applied Physics and Computational Mathematics Beijing100094 China Department of Electrical and Computer Engineering University of Alberta 9211 116 St. NW EdmontonABT6G 1H9 Canada

The propagation and energy coupling of intense laser beams in plasmas are critical issues in laser-driven inertial confinement fusion. Applying magnetic fields to such a setup has been evoked to enhance fuel confinement and heating, and mitigate laser energy losses. Here we report on experimental measurements demonstrating improved transmission and increased smoothing of a high-power laser beam propagating in an underdense magnetized plasma. We also measure enhanced backscattering, which our simulations show is due to hot electrons confinement, thus leading to reduced target preheating. © 2022, CC BY-NC-SA.

关键词： Hot electrons

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Snowmass2021 CMB-HD White Paper

arXiv

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arXiv 2022年

作者： Aiola, Simone Akrami, Yashar Basu, Kaustuv Boylan-Kolchin, Michael Brinckmann, Thejs Bryan, Sean Casey, Caitlin M. Chluba, Jens Clesse, Sébastien Cyr-Racine, Francis-Yan Di Mascolo, Luca Dicker, Simon Essinger-Hileman, Thomas Farren, Gerrit S. Fedderke, Michael A. Ferraro, Simone Fuller, George M. Galitzki, Nicholas Gluscevic, Vera Grin, Daniel Han, Dongwon Hasselfield, Matthew Hložek, Renée Holder, Gil Hotinli, Selim C. Jain, Bhuvnesh Johnson, Bradley Johnson, Matthew Klaassen, Pamela MacInnis, Amanda Madhavacheril, Mathew Mandal, Sayan Mauskopf, Philip Meerburg, Daan Meyers, Joel Miranda, Vivian Mroczkowski, Tony Mukherjee, Suvodip Münchmeyer, Moritz Munoz, Julian Naess, Sigurd Nagai, Daisuke Namikawa, Toshiya Newburgh, Laura Nguyên, Hô Nam Niemack, Michael Oppenheimer, Benjamin D. Pierpaoli, Elena Raghunathan, Srinivasan Schaan, Emmanuel Sehgal, Neelima Sherwin, Blake Simon, Sara M. Slosar, Anže Smith, Kendrick Spergel, David Switzer, Eric R. Trivedi, Pranjal Tsai, Yu-Dai van Engelen, Alexander Wandelt, Benjamin D. Wollack, Edward J. Wu, Kimmy Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States CERCA ISO Department of Physics Case Western Reserve University 10900 Euclid Avenue ClevelandOH44106 United States Department of Physics Imperial College London Blackett Laboratory Prince Consort Road LondonSW7 2AZ United Kingdom Laboratoire de Physique de l’École Normale Supérieure ENS Université PSL CNRS Sorbonne Université ParisF-75005 France Observatoire de Paris Université PSL Sorbonne Université LERMA Paris750 France Argelander Institute for Astronomy University of Bonn Auf dem Hügel 71 BonnD-53121 Germany Department of Astronomy The University of Texas at Austin 2515 Speedway Stop C1400 AustinTX78712 United States Dipartimento di Fisica e Scienze della Terra Universitá degli Studi di Ferrara via Giuseppe Saragat 1 Ferrara44122 Italy Sezione di Ferrara Via Giuseppe Saragat 1 Ferrara44122 Italy School of Earth and Space Exploration Arizona State University 781 Terrace Mall TempeAZ85287 United States Jodrell Bank Centre for Astrophysics Alan Turing Building University of Manchester ManchesterM13 9PL United Kingdom Université Libre de Bruxelles Boulevard du Triomphe Brussels1050 Belgium Department of Physics and Astronomy University of New Mexico 210 Yale Blvd NE AlbuquerqueNM87106 United States Astronomy Unit Department of Physics University of Trieste via Tiepolo 11 Trieste34131 Italy INAF Osservatorio Astronomico di Trieste via Tiepolo 11 Trieste34131 Italy IFPU - Institute for Fundamental Physics of the Universe Via Beirut 2 Trieste340 Italy Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States NASA/Goddard Space Flight Center GreenbeltMD20771 United States Department of Applied Mathematics and Theoretical Physics University of Cambridge CambridgeCB3 0WA United Kingdom Department of Physics and Astronomy Haverford College 370 Lancaste

CMB-HD is a proposed millimeter-wave survey over half the sky that would be ultra-deep (0.5 µK-arcmin) and have unprecedented resolution (15 arcseconds at 150 GHz). Such a survey would answer many outstanding questions about the fundamental physics of the Universe. Major advances would be 1.) the use of gravitational lensing of the primordial microwave background to map the distribution of matter on small scales (k ∼ 10 hMpc-1), which probes dark matter particle properties. It will also allow 2.) measurements of the thermal and kinetic Sunyaev-Zel’dovich effects on small scales to map the gas density and velocity, another probe of cosmic structure. In addition, CMB-HD would allow us to cross critical thresholds: 3.) ruling out or detecting any new, light ( © 2022, CC BY.

关键词： Telescopes

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Systematic study of flow vector fluctuations in sNN=5.02 TeV Pb-Pb collisions

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Physical Review C 2024年第6期109卷 065202-065202页

作者： S. Acharya D. Adamová A. Agarwal G. Aglieri Rinella L. Aglietta M. Agnello N. Agrawal Z. Ahammed S. Ahmad S. U. Ahn I. Ahuja A. Akindinov V. Akishina M. Al-Turany D. Aleksandrov B. Alessandro H. M. Alfanda R. Alfaro Molina B. Ali A. Alici N. Alizadehvandchali A. Alkin J. Alme G. Alocco T. Alt A. R. Altamura I. Altsybeev J. R. Alvarado M. N. Anaam C. Andrei N. Andreou A. Andronic E. Andronov V. Anguelov F. Antinori P. Antonioli N. Apadula L. Aphecetche H. Appelshäuser C. Arata S. Arcelli M. Aresti R. Arnaldi J. G. M. C. A. Arneiro I. C. Arsene M. Arslandok A. Augustinus R. Averbeck M. D. Azmi H. Baba A. Badalà J. Bae Y. W. Baek X. Bai R. Bailhache Y. Bailung R. Bala A. Balbino A. Baldisseri B. Balis D. Banerjee Z. Banoo V. Barbasova F. Barile L. Barioglio M. Barlou B. Barman G. G. Barnaföldi L. S. Barnby E. Barreau V. Barret L. Barreto C. Bartels K. Barth E. Bartsch N. Bastid S. Basu G. Batigne D. Battistini B. Batyunya D. Bauri J. L. Bazo Alba I. G. Bearden C. Beattie P. Becht D. Behera I. Belikov A. D. C. Bell Hechavarria F. Bellini R. Bellwied S. Belokurova L. G. E. Beltran Y. A. V. Beltran G. Bencedi A. Bensaoula S. Beole Y. Berdnikov A. Berdnikova L. Bergmann M. G. Besoiu L. Betev P. P. Bhaduri A. Bhasin M. A. Bhat B. Bhattacharjee L. Bianchi N. Bianchi J. Bielčík J. Bielčíková A. P. Bigot A. Bilandzic G. Biro S. Biswas N. Bize J. T. Blair D. Blau M. B. Blidaru N. Bluhme C. Blume G. Boca F. Bock T. Bodova J. Bok L. Boldizsár M. Bombara P. M. Bond G. Bonomi H. Borel A. Borissov A. G. Borquez Carcamo H. Bossi E. Botta Y. E. M. Bouziani L. Bratrud P. Braun-Munzinger M. Bregant M. Broz G. E. Bruno M. D. Buckland D. Budnikov H. Buesching S. Bufalino P. Buhler N. Burmasov Z. Buthelezi A. Bylinkin S. A. Bysiak J. C. Cabanillas Noris M. F. T. Cabrera M. Cai H. Caines A. Caliva E. Calvo Villar J. M. M. Camacho P. Camerini F. D. M. Canedo S. L. Cantway M. Carabas A. A. Carballo F. Carnesecchi R. Caron L. A. D. Carvalho J. Castillo Castellanos M. Castoldi F. Catalano S. Cattaruzzi C. Ceballos Sanchez R. Cerri I. Chakabe CNRS/IN2P3 LPC Clermont-Ferrand France Nuclear Physics Institute of the Czech Academy of Sciences Husinec-Řež Czech Republic Homi Bhabha National Institute Kolkata India Geneva Switzerland and Sezione INFN Turin Italy and Sezione INFN Bologna Italy Department of Physics Daejeon Republic of Korea Faculty of Science Affiliated with an institute covered by a cooperation agreement with CERN Frankfurt Institute for Advanced Studies Research Division and ExtreMe Matter Institute EMMI Turin Italy Wuhan China Instituto de Física Houston Texas USA Sungkyunkwan University Suwon City Republic of Korea Department of Physics and Technology Cagliari Italy Institut für Kernphysik Bari Italy Physik Department Technische Universität München Munich Germany High Energy Physics Group Bucharest Romania University of Derby Derby United Kingdom Institut für Kernphysik Münster Germany Physikalisches Institut Padova Italy Bologna Italy Berkeley California USA SUBATECH Université Grenoble-Alpes CNRS-IN2P3 Grenoble France and Sezione INFN Cagliari Italy São Paulo Brazil New Haven Connecticut USA Tokyo Japan Catania Italy Gangneung Republic of Korea Hefei China Indore India Physics Department Université Paris-Saclay Centre d'Etudes de Saclay (CEA) IRFU Départment de Physique Nucléaire (DPhN) Saclay France Cracow Poland Department of Physics and Centre for Astroparticle Physics and Space Science (CAPSS) Kolkata India and Sezione INFN Bari Italy School of Science Department of Physics Athens Greece Department of Physics Guwahati India Budapest Hungary Liverpool United Kingdom Department of Physics Division of Particle Physics Lund Sweden Affiliated with an international laboratory covered by a cooperation agreement with CERN Mumbai India Sección Física Departamento de Ciencias Niels Bohr Institute CNRS IPHC UMR 7178 F-67000 Strasbourg France Strasbourg France Universidad Autónoma de Sinaloa Culiacá

Measurements of the pT-dependent flow vector fluctuations in Pb–Pb collisions at sNN=5.02TeV using azimuthal correlations with the ALICE experiment at the Large Hadron Collider are presented. A four-particle correlation approach [ALICE Collaboration, Phys. Rev. C 107, L051901 (2023)] is used to quantify the effects of flow angle and magnitude fluctuations separately. This paper extends previous studies to additional centrality intervals and provides measurements of the pT-dependent flow vector fluctuations at sNN=5.02TeV with two-particle correlations. Significant pT-dependent fluctuations of the V⃗2 flow vector in Pb–Pb collisions are found across different centrality ranges, with the largest fluctuations of up to ∼15% being present in the 5% most central collisions. In parallel, no evidence of significant pT-dependent fluctuations of V⃗3 or V⃗4 is found. Additionally, evidence of flow angle and magnitude fluctuations is observed with more than 5σ significance in central collisions. These observations in Pb–Pb collisions indicate where the classical picture of hydrodynamic modeling with a common symmetry plane breaks down. This has implications for hard probes at high pT, which might be biased by pT-dependent flow angle fluctuations of at least 23% in central collisions. Given the presented results, existing theoretical models should be reexamined to improve our understanding of initial conditions, quark–gluon plasma properties, and the dynamic evolution of the created system.

关键词： Particle correlations & fluctuations Quark-gluon plasma Relativistic heavy-ion collisions

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The Building of Galactic Disks: Insights from the Triangulum Spiral Galaxy Messier 33

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Proceedings of the International Astronomical Union 2006年第S235期2卷 29-35页

作者： David L. Block Ivânio Puerari Giovanni G. Fazio Alan Stockton Gabriela Canalizo Kenneth C. Freeman Thomas H. Jarrett Françoise Combes Robert Groess Guy Worthey Anglo American Cosmic Dust Laboratory School of Computational and Applied Mathematics University of Witwatersrand Johannesburg 2050 South Africa email: block@cam.wits.ac.za Instituto Nacional de Astrofísica Optica y Electrónica Tonantzintla 72840 México email: puerari@inaoep.mx Harvard-Smithsonian Center for Astrophysics 60 Garden St. Cambridge MA 02138 USA email: gfazio@cfa.harvard.edu Institute for Astronomy University of Hawaii 2680 Woodlawn Drive Honolulu Hawaii USA email: stockton@ifa.hawaii.edu Institute of Geophysics and Planetary Physics and Department of Physics University of California Riverside CA 92521 USA Mount Stromlo and Siding Spring Observatories Research School of Astronomy and Astrophysics Australian National University Australia email: kcf@mso.anu.edu.au Infrared Processing and Analysis Centre 100-22 CALTECH 770 South Wilson Ave Pasadena CA 91125 USA email: jarrett@ipac.caltech.edu Observatoire de Paris LERMA 61 Av. de l'Observatoire F-75014 Paris France email: francoise.combes@obspm.fr Washington State University 1245 Webster Hall Pullman WA 99163-2814 USA email: gworthey@wsu.edu

The Triangulum Spiral Galaxy Messier 33 offers unique insights into the building of a galactic disk. We identify spectacular arcs of intermediate age (0.6 Gyr − 2 Gyr) stars in the low-metallicity outer disk. The northern arc spans ~120 degrees in azimuth and up to 5 arcmin in width. The arcs are located 2-3 disk scale lengths from the galaxy centre (where 1 disk scale length is equivalent to 0.1 degrees in the V-band) and lie precisely where there is a warp in the HI profile of M33. Warps and infall are inextricably linked (Binney, 1992). We present spectroscopy of candidate stars in the outer northern arc, secured using the Keck I telescope in Hawaii. The target stars have estimated visual magnitudes as faint as V~ 25m. Absorption bands of CN are seen in all spectra reported in this review talk, confirming their carbon star status. Also presented are PAH emissivity radial profiles generated from IRAC observations of M33 using the Spitzer Space Telescope. A dramatic change of phase in the m = 2 Fourier component is detected at the domain of the arcs. M33 serves as an excellent example how the disks of spiral galaxies in our Universe are built: as dynamically open systems, growing from the inward, outward.

关键词： galaxies: evolution – galaxies: spiral – galaxies: individual (M33 = NGC598)

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computational Identification and Experimental Demonstration of High-Performance Methane Sorbents

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Angewandte Chemie 2022年第25期134卷

作者： Dr. Karabi Nath Dr. Alauddin Ahmed Prof. Dr. Donald J. Siegel Prof. Dr. Adam J. Matzger Department of Chemistry and Macromolecular Science and Engineering Program University of Michigan 930 North University Avenue Ann Arbor MI 48109 USA Mechanical Engineering Department University of Michigan Ann Arbor MI 48109 USA Materials Science and Engineering Applied Physics Program and University of Michigan Energy Institute University of Michigan Ann Arbor MI 48109 USA Current address: Walker Department of Mechanical Engineering Texas Materials Institute and Oden Institute for Computational Engineering and Sciences University of Texas at Austin 204 E. Dean Keeton Street ETC II 5.160 Austin TX 78712-1591 USA

Remarkable methane uptake is demonstrated experimentally in three metal-organic frameworks (MOFs) identified by computational screening: UTSA-76, UMCM-152 and DUT-23-Cu. These MOFs outperform the benchmark sorbent, HKUST-1, both volumetrically and gravimetrically, under a pressure swing of 80 to 5 bar at 298 K. Although high uptake at elevated pressure is critical for achieving this performance, a low density of high-affinity sites (coordinatively unsaturated metal centers) also contributes to a more complete release of stored gas at low pressure. The identification of these MOFs facilitates the efficient storage of natural gas via adsorption and provides further evidence of the utility of computational screening in identifying overlooked sorbents.

关键词： computational Screening Deliverable Capacity Interatomic Potentials Metal Organic Framework (MOF) Methane Storage

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Artificial Intelligence for Science in Quantum, Atomistic, and Continuum Systems

arXiv

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arXiv 2023年

作者： Zhang, Xuan Wang, Limei Helwig, Jacob Luo, Youzhi Fu, Cong Xie, Yaochen Liu, Meng Lin, Yuchao Xu, Zhao Yan, Keqiang Adams, Keir Weiler, Maurice Li, Xiner Fu, Tianfan Wang, Yucheng Strasser, Alex Yu, Haiyang Xie, YuQing Fu, Xiang Xu, Shenglong Liu, Yi Du, Yuanqi Saxton, Alexandra Ling, Hongyi Lawrence, Hannah Stärk, Hannes Gui, Shurui Edwards, Carl Gao, Nicholas Ladera, Adriana Wu, Tailin Hofgard, Elyssa F. Tehrani, Aria Mansouri Wang, Rui Daigavane, Ameya Bohde, Montgomery Kurtin, Jerry Huang, Qian Phung, Tuong Xu, Minkai Joshi, Chaitanya K. Mathis, Simon V. Azizzadenesheli, Kamyar Fang, Ada Aspuru-Guzik, Alán Bekkers, Erik Bronstein, Michael Zitnik, Marinka Anandkumar, Anima Ermon, Stefano Liò, Pietro Yu, Rose Günnemann, Stephan Leskovec, Jure Ji, Heng Sun, Jimeng Barzilay, Regina Jaakkola, Tommi Coley, Connor W. Qian, Xiaoning Qian, Xiaofeng Smidt, Tess Ji, Shuiwang Department of Computer Science & Engineering Texas A&M University College StationTX United States Department of Chemical Engineering Massachusetts Institute of Technology Cambridge United Kingdom AMLab University of Amsterdam Amsterdam Netherlands Department of Computer Science University of Illinois Urbana-Champaign UrbanaIL United States Department of Electrical & Computer Engineering Texas A&M University College StationTX United States Department of Electrical Engineering and Computer Science Massachusetts Institute of Technology Cambridge United Kingdom Department of Materials Science & Engineering Texas A&M University College StationTX United States Department of Physics & Astronomy Texas A&M University College StationTX United States Department of Applied Mathematics & Statistics Stony Brook University Stony BrookNY United States Department of Computer Science Stony Brook University Stony BrookNY United States Department of Computer Science Cornell University IthacaNY United States Department of Computer Science Technical University of Munich München Germany Department of Computer Science Stanford University StanfordCA United States Department of Computer Science & Engineering University of California San Diego La Jolla CA United States Department of Computer Science & Technology University of Cambridge Cambridge United Kingdom Nvidia Santa ClaraCA United States Department of Chemistry and Chemical Biology Harvard University Cambridge United Kingdom Department of Chemistry University of Toronto Toronto Canada Department of Computer Science University of Toronto Toronto Canada Department of Computer Science University of Oxford Oxford United Kingdom Department of Biomedical Informatics Harvard University BostonMA United States Department of Computing & Mathematical Sciences California Institute of Technology PasadenaCA United States Computational Science Initiative Brookhaven National Laboratory UptonNY United States

Advances in artificial intelligence (AI) are fueling a new paradigm of discoveries in natural sciences. Today, AI has started to advance natural sciences by improving, accelerating, and enabling our understanding of natural phenomena at a wide range of spatial and temporal scales, giving rise to a new area of research known as AI for science (AI4Science). Being an emerging research paradigm, AI4Science is unique in that it is an enormous and highly interdisciplinary area. Thus, a unified and technical treatment of this field is needed yet challenging. This work aims to provide a technically thorough account of a subarea of AI4Science;namely, AI for quantum, atomistic, and continuum systems. These areas aim at understanding the physical world from the subatomic (wavefunctions and electron density), atomic (molecules, proteins, materials, and interactions), to macro (fluids, climate, and subsurface) scales and form an important subarea of AI4Science. A unique advantage of focusing on these areas is that they largely share a common set of challenges, thereby allowing a unified and foundational treatment. A key common challenge is how to capture physics first principles, especially symmetries, in natural systems by deep learning methods. We provide an in-depth yet intuitive account of techniques to achieve equivariance to symmetry transformations. We also discuss other common technical challenges, including explainability, out-of-distribution generalization, knowledge transfer with foundation and large language models, and uncertainty quantification. To facilitate learning and education, we provide categorized lists of resources that we found to be useful. We strive to be thorough and unified and hope this initial effort may trigger more community interests and efforts to further advance AI4Science. Copyright © 2023, The Authors. All rights reserved.

关键词： Deep learning

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Cross-correlation of Dark Energy Survey Year 3 lensing data with ACT and Planck thermal Sunyaev-Zel’dovich effect observations. II. Modeling and constraints on halo pressure profiles

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Physical Review D 2022年第12期105卷 123526-123526页

作者： S. Pandey M. Gatti E. Baxter J. C. Hill X. Fang C. Doux G. Giannini M. Raveri J. DeRose H. Huang E. Moser N. Battaglia A. Alarcon A. Amon M. Becker A. Campos C. Chang R. Chen A. Choi K. Eckert J. Elvin-Poole S. Everett A. Ferte I. Harrison N. Maccrann J. Mccullough J. Myles A. Navarro Alsina J. Prat R. P. Rollins C. Sanchez T. Shin M. Troxel I. Tutusaus B. Yin M. Aguena S. Allam F. Andrade-Oliveira G. M. Bernstein E. Bertin B. Bolliet J. R. Bond D. Brooks E. Calabrese A. Carnero Rosell M. Carrasco Kind J. Carretero R. Cawthon M. Costanzi M. Crocce L. N. da Costa M. E. S. Pereira J. De Vicente S. Desai H. T. Diehl J. P. Dietrich P. Doel J. Dunkley A. E. Evrard S. Ferraro I. Ferrero B. Flaugher P. Fosalba J. García-Bellido E. Gaztanaga D. W. Gerdes T. Giannantonio D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez K. Herner A. D. Hincks S. R. Hinton D. L. Hollowood K. Honscheid J. P. Hughes D. Huterer B. Jain D. J. James T. Jeltema E. Krause K. Kuehn O. Lahav M. Lima M. Lokken M. S. Madhavacheril M. A. G. Maia J. J. Mcmahon P. Melchior F. Menanteau R. Miquel J. J. Mohr K. Moodley R. Morgan F. Nati M. D. Niemack L. Page A. Palmese F. Paz-Chinchón A. Pieres A. A. Plazas Malagón M. Rodriguez-Monroy A. K. Romer E. Sanchez V. Scarpine E. Schaan S. Serrano I. Sevilla-Noarbe E. Sheldon B. D. Sherwin C. Sifón M. Smith M. Soares-Santos D. Spergel E. Suchyta M. E. C. Swanson G. Tarle D. Thomas C. To T. N. Varga J. Weller E. J. Wollack Z. Xu Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawai’i 96822 USA Department of Physics Columbia University New York New York 10027 USA Center for Computational Astrophysics Flatiron Institute New York New York 10010 USA Department of Astronomy/Steward Observatory University of Arizona 933 North Cherry Avenue Tucson Arizona 85721-0065 USA Institut de Física d’Altes Energies (IFAE) The Barcelona Institute of Science and Technology Campus UAB 08193 Bellaterra (Barcelona) Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road Berkeley California 94720 USA Department of Physics University of Arizona Tucson Arizona 85721 USA Department of Astronomy Cornell University Ithaca New York 14853 USA Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15312 USA Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics Duke University Durham North Carolina 27708 USA Center for Cosmology and Astro-Particle Physics The Ohio State University Columbus Ohio 43210 USA Department of Physics The Ohio State University Columbus Ohio 43210 USA Santa Cruz Institute for Particle Physics Santa Cruz California 95064 USA Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive Pasadena California 91109 USA Department of Physics University of Oxford Denys Wilkinson Building Keble Road Oxford OX1 3RH United Kingdom Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road Manchester M13 9PL United Kin

Hot, ionized gas leaves an imprint on the cosmic microwave background via the thermal Sunyaev-Zel’dovich (tSZ) effect. The cross-correlation of gravitational lensing (which traces the projected mass) with the tSZ effect (which traces the projected gas pressure) is a powerful probe of the thermal state of ionized baryons throughout the Universe and is sensitive to effects such as baryonic feedback. In a companion paper (Gatti et al. Phys. Rev. D 105, 123525 (2022)), we present tomographic measurements and validation tests of the cross-correlation between Galaxy shear measurements from the first three years of observations of the Dark Energy Survey and tSZ measurements from a combination of Atacama Cosmology Telescope and Planck observations. In this work, we use the same measurements to constrain models for the pressure profiles of halos across a wide range of halo mass and redshift. We find evidence for reduced pressure in low-mass halos, consistent with predictions for the effects of feedback from active Galactic nuclei. We infer the hydrostatic mass bias (B≡M500c/MSZ) from our measurements, finding B=1.8±0.1 when adopting the Planck-preferred cosmological parameters. We additionally find that our measurements are consistent with a nonzero redshift evolution of B, with the correct sign and sufficient magnitude to explain the mass bias necessary to reconcile cluster count measurements with the Planck-preferred cosmology. Our analysis introduces a model for the impact of intrinsic alignments (IAs) of galaxy shapes on the shear-tSZ correlation. We show that IA can have a significant impact on these correlations at current noise levels.

关键词： Cosmic microwave background Cosmological parameters Gravitational lenses Large scale structure of the Universe Optical, UV, & IR astronomy

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The SRG/eROSITA All-Sky Survey: Dark Energy Survey Year 3 Weak Gravitational Lensing by eRASS1 selected Galaxy Clusters

arXiv

引用

arXiv 2024年

作者： Grandis, S. Ghirardini, V. Bocquet, S. Garrel, C. Mohr, J.J. Liu, A. Kluge, M. Kimmig, L. Reiprich, T.H. Alarcon, A. Amon, A. Artis, E. Bahar, Y.E. Balzer, F. Bechtol, K. Becker, M.R. Bernstein, G. Bulbul, E. Campos, A. Carnero Rosell, A. Carrasco Kind, M. Cawthon, R. Chang, C. Chen, R. Chiu, I. Choi, A. Clerc, N. Comparat, J. Cordero, J. Davis, C. Derose, J. Diehl, H.T. Dodelson, S. Doux, C. Drlica-Wagner, A. Eckert, K. Elvin-Poole, J. Everett, S. Ferte, A. Gatti, M. Giannini, G. Giles, P. Gruen, D. Gruendl, R.A. Harrison, I. Hartley, W.G. Herner, K. Huff, E.M. Kleinebreil, F. Kuropatkin, N. Leget, P.F. Maccrann, N. McCullough, J. Merloni, A. Myles, J. Nandra, K. Navarro-Alsina, A. Okabe, N. Pacaud, F. Pandey, S. Prat, J. Predehl, P. Ramos, M. Raveri, M. Rollins, R.P. Roodman, A. Ross, A.J. Rykoff, E.S. Sanchez, C. Sanders, J. Schrabback, T. Secco, L.F. Seppi, R. Sevilla-Noarbe, I. Sheldon, E. Shin, T. Troxel, M. Tutusaus, I. Varga, T.N. Wu, H. Yanny, B. Yin, B. Zhang, X. Zhang, Y. Alves, O. Bhargava, S. Brooks, D. Burke, D.L. Carretero, J. Costanzi, M. da Costa, L.N. Pereira, M.E.S. De Vicente, J. Desai, S. Doel, P. Ferrero, I. Flaugher, B. Friedel, D. Frieman, J. García-Bellido, J. Gutierrez, G. Hinton, S.R. Hollowood, D.L. Honscheid, K. James, D.J. Jeffrey, N. Lahav, O. Lee, S. Marshall, J.L. Menanteau, F. Ogando, R.L.C. Pieres, A. Plazas Malagón, A.A. Romer, A.K. Sanchez, E. Schubnell, M. Smith, M. Suchyta, E. Swanson, M.E.C. Tarle, G. Weaverdyck, N. Weller, J. Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstr. 25/8 Innsbruck6020 Austria Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse 1 Garching85748 Germany Faculty of Physics Ludwig-Maximilians-Universität München Scheinerstr. 1 Munich81679 Germany Universität Bonn Auf dem Hügel 71 Bonn53121 Germany Kavli Institute for Cosmology University of Cambridge Mading- ley Road CambridgeCB3 0HA United Kingdom Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Physics Department University of Wisconsin-Madison MadisonWI53706 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Physics Carnegie Mellon University PittsburghPA15312 United States Instituto de Astrofisica de Canarias Tenerife La LagunaE-38205 Spain Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Universidad de La Laguna Dpto. Astrofísica Tenerife La LagunaE-38206 Spain Center for Astrophysical Surveys National Center for Supercom- puting Applications 1205 West Clark St. UrbanaIL61801 United States Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street UrbanaIL61801 United States Physics Department William Jewell College LibertyMO64068 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Physics Duke University DurhamNC27708 United States Department of Physics National Cheng Kung University Tainan70101 Taiwan NASA Goddard Space Flight Center 8800 Greenbelt Rd Green- belt MD20771 United States IRAP Université de Toulouse CNRS UPS CNES Toulouse France Jodrell Bank Center f

Context. Number counts of galaxy clusters across redshift are a powerful cosmological probe, if a precise and accurate reconstruction of the underlying mass distribution is performed - a challenge called mass calibration. With the advent of wide and deep photometric surveys, weak gravitational lensing by clusters has become the method of choice to perform this measurement. Aims. We measure and validate the weak gravitational lensing (WL) signature in the shape of galaxies observed in the first 3 years of the Dark Energy Survey (DES Y3) caused by galaxy clusters and groups selected in the first all-sky survey performed by SRG (Spectrum Roentgen Gamma)/eROSITA (eRASS1). These data are then used to determine the scaling between X-ray photon count rate of the clusters and their halo mass and redshift. Methods. We empirically determine the degree of cluster member contamination in our background source sample. The individual cluster shear profiles are then analysed with a Bayesian population model that self-consistently accounts for the lens sample selection and contamination, and includes marginalization over a host of instrumental and astrophysical systematics. To quantify the accuracy of the mass extraction of that model, we perform mass measurements on mock cluster catalogs with realistic synthetic shear profiles. This allows us to establish that hydro-dynamical modelling uncertainties at low lens redshifts (z © 2024, CC BY.

关键词： Calibration

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