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Using physical features of protein core packing to distinguish real proteins from decoys

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arXiv 2020年

作者： Grigas, Alex T. Mei, Zhe Treado, John D. Levine, Zachary A. Regan, Lynne O'Hern, Corey S. Graduate Program in Computational Biology and Bioinformatics Yale University New HavenCT06520 United States Integrated Graduate Program in Physical and Engineering Biology Yale University New HavenCT06520 United States Department of Chemistry Yale University New HavenCT06520 United States Department of Mechanical Engineering and Materials Science Yale University New HavenCT06520 United States Department of Pathology Yale University New HavenCT06520 United States Department of Molecular Biophysics and Biochemistry Yale University New HavenCT06520 United States Institute of Quantitative Biology Biochemistry and Biotechnology Centre for Synthetic and Systems Biology School of Biological Sciences University of Edinburgh Department of Physics Yale University New HavenCT06520 United States Department of Applied Physics Yale University New HavenCT06520 United States

The ability to consistently distinguish real protein structures from computationally generated model decoys is not yet a solved problem. One route to distinguish real protein structures from decoys is to delineate the important physical features that specify a real protein. For example, it has long been appreciated that the hydrophobic cores of proteins contribute signifficantly to their stability. As a dataset of decoys to compare with real protein structures, we studied submissions to the bi-annual CASP competition (speciffically CASP11, 12, and 13), in which researchers attempt to predict the structure of a protein only knowing its amino acid sequence. Our analysis reveals that many of the submissions possess cores that do not recapitulate the features that define real proteins. In particular, the model structures appear more densely packed (because of energetically unfavorable atomic overlaps), contain too few residues in the core, and have improper distributions of hydrophobic residues throughout the structure. Based on these observations, we developed a deep learning method, which incorporates key physical features of protein cores, to predict how well a computational model recapitulates the real protein structure without knowledge of the structure of the target sequence. By identifying the important features of protein structure, our method is able to rank decoys from the CASP competitions equally well, if not better than, state-of-the-art methods that incorporate many additional features. Copyright © 2020, The Authors. All rights reserved.

关键词： Proteins

Modeling dense star clusters in the milky way and beyond with the cluster monte carlo code

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arXiv 2021年

作者： Rodriguez, Carl L. Weatherford, Newlin C. Coughlin, Scott C. Seoane, Pau Amaro Breivik, Katelyn Chatterjee, Sourav Fragione, Giacomo Kiroǧlu, Fulya Kremer, Kyle Rui, Nicholas Z. Ye, Claire S. Zevin, Michael Rasio, Frederic A. McWilliams Center for Cosmology and Department of Physics Carnegie Mellon University PittsburghPA15213 United States Department of Physics & Astronomy Northwestern University EvanstonIL60208 United States Northwestern University EvanstonIL60208 United States Universitat Politècnica de València Camino de Vera s/n 46022 Valencia Spain DESY Zeuthen Platanenallee 6 ZeuthenD-15738 Germany Institute of Applied Mathematics Academy of Mathematics and Systems Science CAS Beijing100190 China Kavli Institute for Astronomy and Astrophysics Beijing100871 China Zentrum für Astronomie und Astrophysik TU Berlin Hardenbergstraße 36 Berlin10623 Germany Center for Computational Astrophysics Flatiron Institute 162 Fifth Ave New YorkNY10010 United States Tata Institute of Fundamental Research Homi Bhabha Road Mumbai400005 India TAPIR California Institute of Technology PasadenaCA91125 United States The Observatories of the Carnegie Institution for Science PasadenaCA91101 United States Kavli Institute for Cosmological Physics The University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute The University of Chicago 933 East 56th Street ChicagoIL60637 United States

We describe the public release of the Cluster Monte Carlo Code (CMC) a parallel, star-by-star N-body code for modeling dense star clusters. CMC treats collisional stellar dynamics using Hénon's method, where the cumulative effect of many two-body encounters is statistically reproduced as a single effective encounter between nearest-neighbor particles on a relaxation timescale. The star-by-star approach allows for the inclusion of additional physics, including strong gravitational three- and four-body encounters, two-body tidal and gravitational-wave captures, mass loss in arbitrary galactic tidal fields, and stellar evolution for both single and binary stars. The public release of CMC is pinned directly to the COSMIC population synthesis code, allowing dynamical star cluster simulations and population synthesis studies to be performed using identical assumptions about the stellar physics and initial conditions. As a demonstration, we present two examples of star cluster modeling: first, we perform the largest (N = 108) star-by-star N-body simulation of a Plummer sphere evolving to core collapse, reproducing the expected self-similar density profile over more than 15 orders of magnitude;second, we generate realistic models for typical globular clusters, and we show that their dynamical evolution can produce significant numbers of black hole mergers with masses greater than those produced from isolated binary evolution (such as GW190521, a recently reported merger with component masses in the pulsational pair-instability mass gap). © 2021, CC BY.

关键词： Stars

Unprivileged groups are less served by green cooling services in major European urban areas

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Nature Cities

Nature Cities 2024年 424-435页

作者： Alby Duarte Rocha Stenka Vulova Michael Förster Birgit Kleinschmit Beniamino Gioli Bradley Matthews Carole Helfter Fred Meier Gert-Jan Steeneveld Janet F. Barlow Leena Järvi Nektarios Chrysoulakis Giacomo Nicolini Geoinformation in Environmental Planning Lab Technische Universität Berlin Berlin Germany Department of Environmental Meteorology University of Kassel Kassel Germany Institute of BioEconomy National Research Council (IBE-CNR) Florence Italy Department of Forest- and Soil Sciences Institute of Forest Ecology University of Natural Resources and Life Sciences Vienna Austria Environment Agency Austria Vienna Austria UK Center for Ecology and Hydrology Penicuik UK Chair of Climatology Institute of Ecology Technische Universität Berlin Berlin Germany Meteorology and Air Quality Section Wageningen University Wageningen the Netherlands Department of Meteorology University of Reading Reading UK Institute for Atmospheric and Earth System Research/Physics Helsinki Institute of Sustainability Science University of Helsinki Helsinki Finland Remote Sensing Lab Institute of Applied and Computational Mathematics Foundation for Research and Technology Hellas Heraklion Greece CMCC Foundation Euro-Mediterranean Center on Climate Change Viterbo Italy

Heat stress is the leading climate-related cause of premature deaths in Europe. Major heatwaves have struck Europe recently and are expected to increase in magnitude and length. Large cities are particularly threatened due to the urban morphology and imperviousness. Green spaces mitigate heat, providing cooling services through shade provision and evapotranspiration. However, the distribution of green cooling and the population most affected are often unknown. Here we reveal environmental injustice regarding green cooling in 14 major European urban areas. Vulnerable residents in Europe are not concentrated in the suburbs but in run-down central areas that coincide with low-cooling regions. In all studied areas, lower-income residents, tenants, immigrants and unemployed citizens receive below-average green cooling, while upper-income residents, nationals and homeowners experience above-average cooling provision. The fatality risk during extreme heatwaves may increase as vulnerable residents are unable to afford passive or active cooling mitigation.

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The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers

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Astrophysical Journal, Supplement Series 2020年第1期249卷

作者： Stone, James M. Tomida, Kengo White, Christopher J. Felker, Kyle G. Department of Astrophysical Sciences Princeton University Princeton 08544 NJ United States Program in Applied and Computational Mathematics Princeton University Princeton 08544 NJ United States Department of Earth and Space Science Osaka University Toyonaka Osaka 560-0043 Japan Kavli Institute for Theoretical Physics University of California Santa Barbara Santa Barbara 93107 CA United States School of Natural Sciences Institute for Advanced Study Princeton 08544 NJ United States Astronomical Institute Tohoku University Sendai Miyagi 980-8578 Japan Argonne National Laboratory Lemont 60439 IL United States

The design and implementation of a new framework for adaptive mesh refinement calculations are described. It is intended primarily for applications in astrophysical fluid dynamics, but its flexible and modular design enables its use for a wide variety of physics. The framework works with both uniform and nonuniform grids in Cartesian and curvilinear coordinate systems. It adopts a dynamic execution model based on a simple design called a "task list"that improves parallel performance by overlapping communication and computation, simplifies the inclusion of a diverse range of physics, and even enables multiphysics models involving different physics in different regions of the calculation. We describe physics modules implemented in this framework for both nonrelativistic and relativistic magnetohydrodynamics (MHD). These modules adopt mature and robust algorithms originally developed for the Athena MHD code and incorporate new extensions: support for curvilinear coordinates, higher-order time integrators, more realistic physics such as a general equation of state, and diffusion terms that can be integrated with super-time-stepping algorithms. The modules show excellent performance and scaling, with well over 80% parallel efficiency on over half a million threads. The source code has been made publicly available. © 2020. The American Astronomical Society. All rights reserved..

关键词： Astronomy software Magnetohydrodynamics

A demonstration of improved constraints on primordial gravitational waves with delensing

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Physical Review D 2021年第2期103卷 022004-022004页

作者： P. A. R. Ade Z. Ahmed M. Amiri A. J. Anderson J. E. Austermann J. S. Avva D. Barkats R. Basu Thakur J. A. Beall A. N. Bender B. A. Benson F. Bianchini C. A. Bischoff L. E. Bleem J. J. Bock H. Boenish E. Bullock V. Buza J. E. Carlstrom C. L. Chang J. R. Cheshire, IV H. C. Chiang T-L. Chou R. Citron J. Connors C. Corbett Moran J. Cornelison T. M. Crawford A. T. Crites M. Crumrine A. Cukierman T. de Haan M. Dierickx M. A. Dobbs L. Duband W. Everett S. Fatigoni J. P. Filippini S. Fliescher J. Gallicchio E. M. George T. St. Germaine N. Goeckner-Wald D. C. Goldfinger J. Grayson N. Gupta G. Hall M. Halpern N. W. Halverson S. Harrison S. Henderson J. W. Henning S. R. Hildebrandt G. C. Hilton G. P. Holder W. L. Holzapfel J. D. Hrubes N. Huang J. Hubmayr H. Hui K. D. Irwin J. Kang K. S. Karkare E. Karpel S. Kefeli S. A. Kernasovskiy L. Knox J. M. Kovac C. L. Kuo K. Lau A. T. Lee E. M. Leitch D. Li A. Lowitz A. Manzotti J. J. McMahon K. G. Megerian S. S. Meyer M. Millea L. M. Mocanu L. Moncelsi J. Montgomery A. Nadolski T. Namikawa T. Natoli C. B. Netterfield H. T. Nguyen J. P. Nibarger G. Noble V. Novosad R. O’Brient R. W. Ogburn, IV Y. Omori S. Padin S. Palladino S. Patil T. Prouve C. Pryke B. Racine C. L. Reichardt C. D. Reintsema S. Richter J. E. Ruhl B. R. Saliwanchik K. K. Schaffer A. Schillaci B. L. Schmitt R. Schwarz C. D. Sheehy C. Sievers G. Smecher A. Soliman A. A. Stark B. Steinbach R. V. Sudiwala G. P. Teply K. L. Thompson J. E. Tolan C. Tucker A. D. Turner C. Umiltà T. Veach J. D. Vieira A. G. Vieregg A. Wandui G. Wang A. C. Weber N. Whitehorn D. V. Wiebe J. Willmert C. L. Wong W. L. K. Wu H. Yang V. Yefremenko K. W. Yoon E. Young C. Yu L. Zeng C. Zhang Cardiff University Cardiff CF10 3XQ United Kingdom SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park California 94025 USA Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall Stanford California 94305 USA Department of Physics and Astronomy University of British Columbia Vancouver British Columbia V6T 1Z1 Canada Fermi National Accelerator Laboratory MS209 P.O. Box 500 Batavia Illinois 60510 USA NIST Quantum Devices Group 325 Broadway Mailcode 817.03 Boulder Colorado 80305 USA Department of Physics University of Colorado Boulder Colorado 80309 USA Department of Physics University of California Berkeley California 94720 USA Harvard-Smithsonian Center for Astrophysics 60 Garden Street Cambridge Massachusetts 02138 USA California Institute of Technology MS 249-17 1216 E. California Blvd. Pasadena California 91125 USA High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue Argonne Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA School of Physics University of Melbourne Parkville Victoria 3010 Australia Department of Physics University of Cincinnati Cincinnati Ohio 45221 USA Jet Propulsion Laboratory Pasadena California 91109 USA Department of Physics Harvard University Cambridge Massachusetts 02138 USA Minnesota Institute for Astrophysics University of Minnesota Minneapolis Minnesota 55455 USA Department of Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Department of Physics McGill University 3600 Rue University Montreal Quebec H3A 2T8 Canada School of Mathematics Statistics and Computer Science University of KwaZulu-Natal Dur

We present a constraint on the tensor-to-scalar ratio, r, derived from measurements of cosmic microwave background (CMB) polarization B-modes with “delensing,” whereby the uncertainty on r contributed by the sample variance of the gravitational lensing B-modes is reduced by cross-correlating against a lensing B-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, bicep/Keck, and Planck data. We expand the bicep/Keck likelihood analysis framework to accept a lensing template and apply it to the bicep/Keck dataset collected through 2014 using the same parametric foreground modeling as in the previous analysis. From simulations, we find that the uncertainty on r is reduced by ∼10%, from σ(r)=0.024 to 0.022, which can be compared with a ∼26% reduction obtained when using a perfect lensing template or if there were zero lensing B-modes. Applying the technique to the real data, the constraint on r is improved from r0.05<0.090 to r0.05<0.082 (95% C.L.). This is the first demonstration of improvement in an r constraint through delensing.

关键词： Cosmic microwave background Inflation Large scale structure of the Universe

Imaging the geometrical structure of complex symmetric molecules by above-threshold ionization spectrum in an ir+xuv laser field

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arXiv 2019年

作者： Zhou, Xu-Cong Shi, Shang Li, Fei Guo, Ying-Chun Yang, Yu-Jun Meng, Qing-Tian Chen, Jing Liu, Xiao-Jun Wang, Bingbing Laboratory of Optical Physics Institute of Physics Chinese Academy of Sciences Beijing100190 China School of Physics and Electronics Shandong Normal University Jinan250358 China Department of Physics School of Physics and Electronics East China Normal University Shanghai200062 China Jilin University Insititute of Atomic and Molecular Physics Changchun130012 China Center for Applied Physics and Technology Peking University Hedps Beijing100871 China Institute of Applied Physics and Computational Mathematics Beijing100088 China State Key Laboratory of Magnetic Resonance and Atomic and Molecular Physics Wuhan Institute of Physics and Mathematics Chinese Academy of Sciences Wuhan430071 China University of Chinese Academy of Sciences Beijing100049 China

Based on the frequency-domain theory, we put forward a method of imaging the complex symmetrical polyatomic molecules by using IR+XUV two-color laser fields. Although the wave function of a polyatomic molecule, such as SF6, is quite complex in momentum space, it can be simplified by several terms in the region of high value of momentum, where the destructive interference fringes from these terms carry the information of the molecular structure. In this work, we find that, since the XUV laser field may increases the kinetic energy of the photoelectron dramatically in the above-threshold ionization (ATI) process of a molecule in an IR+XUV two-color laser field, the information of the molecular structure can be obtained by analyzing the interference fringes of the ATI spectrum in the high-energy region, where the simplified wave function of the molecule plays a dominant role in this part of the ATI spectrum. This method provides a unique accessible route towards imaging polyatomic molecules from a frequency perspective. Copyright © 2019, The Authors. All rights reserved.

关键词： Wave functions

Frequency-Resolved Optical Gating Recovery via Smoothing Gradient

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arXiv 2019年

作者： Pinilla, Samuel Bendory, Tamir Eldar, Yonina C. Arguello, Henry Department of Electrical Engineering Universidad Industrial de Santander BucaramangaSantander680002 Colombia Program in Applied and Computational Mathematics Princeton University PrincetonNJ United States Weizmann Institute of Science Rehovot7610001 Israel Department of Computer Science Universidad Industrial de Santander BucaramangaSantander680002 Colombia

Frequency-resolved optical gating (FROG) is a popular technique for complete characterization of ultrashort laser pulses. The acquired data in FROG, called FROG trace, is the Fourier magnitude of the product of the unknown pulse with a time-shifted version of itself, for several different shifts. To estimate the pulse from the FROG trace, we propose an algorithm that minimizes a smoothed non-convex least-squares objective function. The method consists of two steps. First, we approximate the pulse by an iterative spectral algorithm. Then, the attained initialization is refined based upon a sequence of block stochastic gradient iterations. The algorithm is theoretically simple, numerically scalable, and easy-to-implement. Empirically, our approach outperforms the state-of-the-art when the FROG trace is incomplete, that is, when only few shifts are recorded. Simulations also suggest that the proposed algorithm exhibits similar computational cost compared to a state-of-the-art technique for both complete and incomplete data. In addition, we prove that in the vicinity of the true solution, the algorithm converges to a critical point. A Matlab implementation is publicly available at https://***/samuelpinilla/FROG. Copyright © 2019, The Authors. All rights reserved.

关键词： Ultrashort pulses

Novel Polarimetric Analysis of Near Horizon Flaring Episodes in M87* in Millimeter Wavelength

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arXiv 2025年

作者： Emami, Razieh Liska, Matthew Chatterjee, Koushik Bower, Geoffrey C. Benbow, Wystan Finkbeiner, Douglas Wielgus, Maciek Hernquist, Lars Smith, Randall Tremblay, Grant Ricarte, Angelo Steiner, James F. Broderick, Avery E. Saurabh Davelaar, Jordy Grindlay, Josh Vogelsberger, Mark Chan, Chi-Kwan Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Center for Relativistic Astrophysics Georgia Institute of Technology Howey Physics Bldg 837 State Street NW AtlantaGA30332 United States Department of Physics University of Maryland College ParkMD United States Academia Sinica Institute of Astronomy and Astrophysics 645 N. A’ohoku Place HiloHI96720 United States Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n GranadaE-18008 Spain Black Hole Initiative Harvard University 20 Garden Street CambridgeMA02138 United States Perimeter Institute for Theoretical Physics 31 Caroline Street North WaterlooONN2L 2Y5 Canada Department of Physics and Astronomy University of Waterloo 200 University Avenue West WaterlooONN2L 3G1 Canada Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Department of Astrophysical Sciences Peyton Hall Princeton University PrincetonNJ08544 United States NASA Hubble Fellowship Program Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Department of Astronomy and Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States Data Science Institute University of Arizona 1230 N. Cherry Ave. TucsonAZ85721 United States Program in Applied Mathematics University of Arizona 617 N. Santa Rita TucsonAZ85721 United States

Recent multi-wavelength observations of M87* (Algaba et al. 2024) revealed a high-energy γ-ray flare without a corresponding millimeter counterpart. We present a theoretical polarimetric study to evaluate the presence and nature of a potential millimeter flare in M87*, using a suite of general relativistic magnetohydrodynamical simulations with varying black hole (BH) spins and magnetic field configurations. We find that the emergence of a millimeter flare is strongly influenced by both spin and magnetic structure, with limited sensitivity to the electron distribution (thermal vs. non-thermal). We model the intensity light curve with a damped random walk (DRW) and compare the characteristic timescale (τ) with recent SMA observations, finding that the simulated τ exceeds observed values by over an order of magnitude. In a flaring case with BH spin a=+0.5, we identify a distinct millimeter flare followed by an order-of-magnitude flux drop. All Stokes parameters show variability near the flare, including a sign reversal in the electric vector position angle. While most βm modes remain stable, the EB-correlation phase is highly sensitive to both the flare peak and decay. We examine polarimetric signatures in photon sub-rings, focusing on modes ns=0 and ns=1. The ns=0 signal closely matches the full image, while ns=1 reveals distinct behaviors, highlighting the potential of space VLBI to isolate sub-ring features. Finally, we analyze the magnetic and velocity field evolution during the flare, finding that magnetic reconnection weakens during the flux decay, and the clockwise velocity flow transitions into an outflow-dominated regime. These results suggest that transient radio variability near flares encodes key information about BH spin and magnetic field structure, offering a novel probe into the physics of active galactic nuclei. © 2025, CC BY.

关键词： Magnetohydrodynamics

Dark Energy Survey Year 3 results: Cosmology from cosmic shear and robustness to modeling uncertainty

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Physical Review D 2022年第2期105卷 023515-023515页

作者： L. F. Secco S. Samuroff E. Krause B. Jain J. Blazek M. Raveri A. Campos A. Amon A. Chen C. Doux A. Choi D. Gruen G. M. Bernstein C. Chang J. DeRose J. Myles A. Ferté P. Lemos D. Huterer J. Prat M. A. Troxel N. MacCrann A. R. Liddle T. Kacprzak X. Fang C. Sánchez S. Pandey S. Dodelson P. Chintalapati K. Hoffmann A. Alarcon O. Alves F. Andrade-Oliveira E. J. Baxter K. Bechtol M. R. Becker A. Brandao-Souza H. Camacho A. Carnero Rosell M. Carrasco Kind R. Cawthon J. P. Cordero M. Crocce C. Davis E. Di Valentino A. Drlica-Wagner K. Eckert T. F. Eifler M. Elidaiana F. Elsner J. Elvin-Poole S. Everett P. Fosalba O. Friedrich M. Gatti G. Giannini R. A. Gruendl I. Harrison W. G. Hartley K. Herner H. Huang E. M. Huff M. Jarvis N. Jeffrey N. Kuropatkin P.-F. Leget J. Muir J. Mccullough A. Navarro Alsina Y. Omori Y. Park A. Porredon R. Rollins A. Roodman R. Rosenfeld A. J. Ross E. S. Rykoff J. Sanchez I. Sevilla-Noarbe E. S. Sheldon T. Shin A. Troja I. Tutusaus T. N. Varga N. Weaverdyck R. H. Wechsler B. Yanny B. Yin Y. Zhang J. Zuntz T. M. C. Abbott M. Aguena S. Allam J. Annis D. Bacon E. Bertin S. Bhargava S. L. Bridle D. Brooks E. Buckley-Geer D. L. Burke J. Carretero M. Costanzi L. N. da Costa J. De Vicente H. T. Diehl J. P. Dietrich P. Doel I. Ferrero B. Flaugher J. Frieman J. García-Bellido E. Gaztanaga D. W. Gerdes T. Giannantonio J. Gschwend G. Gutierrez S. R. Hinton D. L. Hollowood K. Honscheid B. Hoyle D. J. James T. Jeltema K. Kuehn O. Lahav M. Lima H. Lin M. A. G. Maia J. L. Marshall P. Martini P. Melchior F. Menanteau R. Miquel J. J. Mohr R. Morgan R. L. C. Ogando A. Palmese F. Paz-Chinchón D. Petravick A. Pieres A. A. Plazas Malagón M. Rodriguez-Monroy A. K. Romer E. Sanchez V. Scarpine M. Schubnell D. Scolnic S. Serrano M. Smith M. Soares-Santos E. Suchyta M. E. C. Swanson G. Tarle D. Thomas C. To Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA McWilliams Center for Cosmology Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15213 USA Department of Physics Northeastern University Boston Massachusetts 02115 USA Department of Astronomy/Steward Observatory University of Arizona 933 North Cherry Avenue Tucson Arizona 85721-0065 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) 1290 Versoix Switzerland Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 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 Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA SLAC National Accelerator Laboratory Menlo Park California 94025 USA Berkeley Center for Cosmological Physics University of California Berkeley California 94720 USA Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Dr. Pasadena California 91109 USA Department of Physics and Astronomy University College London Gower Street London WC1E 6BT United Kingdom Department of Physics Duke University Durham North Carolina 27708 USA Department of Applied Mathematics and Theoretical Physics University of Cambridge Cambridge CB3 0WA United Kingdom Instituto de Astrofísica e Ciências do Espaço Faculdade de Ciências Universidade de Lisboa 1769-016 Lisboa Portugal Institute for Astronomy University of Edinburgh Edinburgh EH9 3HJ United Kingdom Perimeter Institute for Theoretical Physics 31 Caroline Street North Waterloo Ontario N2L 2Y5 Canada Institute for Particle Physics and Astrophysic

This work and its companion paper, Amon et al. [Phys. Rev. D 105, 023514 (2022)], present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter S8≡σ8Ωm/0.3 at the 3% level in ΛCDM: S8=0.759−0.023+0.025 (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the ΛCDM analysis: S8=0.772−0.017+0.018 (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of ΛCDM is found to be in statistical agreement with Planck 2018, although favors a lower S8 than the CMB-inferred value by 2.3σ (a p-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3σ in the plane of S8×Ωm caused by uncertainties in the theoretical models.

关键词： Cosmological parameters Gravitational lenses Sky surveys