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Dark Energy Survey Year 3 results: Constraints on extensions to ΛCDM with weak lensing and galaxy clustering

Physical Review D 2023年第8期107卷 083504-083504页

作者： T. M. C. Abbott M. Aguena A. Alarcon O. Alves A. Amon F. Andrade-Oliveira J. Annis S. Avila D. Bacon E. Baxter K. Bechtol M. R. Becker G. M. Bernstein S. Birrer J. Blazek S. Bocquet A. Brandao-Souza S. L. Bridle D. Brooks D. L. Burke H. Camacho A. Campos A. Carnero Rosell M. Carrasco Kind J. Carretero F. J. Castander R. Cawthon C. Chang A. Chen R. Chen A. Choi C. Conselice J. Cordero M. Costanzi M. Crocce L. N. da Costa M. E. S. Pereira C. Davis T. M. Davis J. DeRose S. Desai E. Di Valentino H. T. Diehl S. Dodelson P. Doel C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole S. Everett X. Fang A. Farahi I. Ferrero A. Ferté B. Flaugher P. Fosalba D. Friedel O. Friedrich J. Frieman J. García-Bellido M. Gatti L. Giani T. Giannantonio G. Giannini D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez N. Hamaus I. Harrison W. G. Hartley K. Herner S. R. Hinton D. L. Hollowood K. Honscheid H. Huang E. M. Huff D. Huterer B. Jain D. J. James M. Jarvis N. Jeffrey T. Jeltema A. Kovacs E. Krause K. Kuehn N. Kuropatkin O. Lahav S. Lee P.-F. Leget P. Lemos C. D. Leonard A. R. Liddle M. Lima H. Lin N. MacCrann J. L. Marshall J. McCullough J. Mena-Fernández F. Menanteau R. Miquel V. Miranda J. J. Mohr J. Muir J. Myles S. Nadathur A. Navarro-Alsina R. C. Nichol R. L. C. Ogando Y. Omori A. Palmese S. Pandey Y. Park M. Paterno F. Paz-Chinchón W. J. Percival A. Pieres A. A. Plazas Malagón A. Porredon J. Prat M. Raveri M. Rodriguez-Monroy P. Rogozenski R. P. Rollins A. K. Romer A. Roodman R. Rosenfeld A. J. Ross E. S. Rykoff S. Samuroff C. Sánchez E. Sanchez J. Sanchez D. Sanchez Cid V. Scarpine D. Scolnic L. F. Secco I. Sevilla-Noarbe E. Sheldon T. Shin M. Smith M. Soares-Santos E. Suchyta M. Tabbutt G. Tarle D. Thomas C. To A. Troja M. A. Troxel I. Tutusaus T. N. Varga M. Vincenzi A. R. Walker N. Weaverdyck R. H. Wechsler J. Weller B. Yanny B. Yin Y. Zhang J. Zuntz Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Laboratório Interinstitucional de e-Astronomia-LIneA Rua General José Cristino 77 Rio de Janeiro Rio de Janeiro 20921-400 Brazil Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA Instituto de Fisica Teorica UAM/CSIC Universidad Autonoma de Madrid 28049 Madrid Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth PO1 3FX United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA SLAC National Accelerator Laboratory Menlo Park California 94025 USA Department of Physics Northeastern University Boston Massachusetts 02115 USA University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstrasse 1 81679 Munich Germany Instituto de Física Gleb Wataghin Universidade Estadual de Campinas 13083-859 Campinas São Paulo Brazil Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road Manchester M13 9PL United Kingdom Department of Physics and Astronomy University College London Gower Street London WC1E 6BT United Kingdom Instituto de Física Teórica Universidade Estadual

We constrain six possible extensions to the Λ cold dark matter (CDM) model using measurements from the Dark Energy Survey’s first three years of observations, alone and in combination with external cosmological probes. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data vectors and blind analyses of real data to validate the robustness of our results to astrophysical and modeling systematic errors. In many cases, constraining power is limited by the absence of theoretical predictions beyond the linear regime that are reliable at our required precision. The ΛCDM extensions are dark energy with a time-dependent equation of state, nonzero spatial curvature, additional relativistic degrees of freedom, sterile neutrinos with eV-scale mass, modifications of gravitational physics, and a binned σ8(z) model which serves as a phenomenological probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find (wp,wa)=(−0.99−0.17+0.28,−0.9±1.2) at 68% confidence with zp=0.24 from the DES measurements alone, and (wp,wa)=(−1.03−0.03+0.04,−0.4−0.3+0.4) with zp=0.21 for the combination of all data considered. Curvature constraints of Ωk=0.0009±0.0017 and effective relativistic species Neff=3.10−0.16+0.15 are dominated by external data, though adding DES information to external low-redshift probes tightens the Ωk constraints that can be made without cosmic microwave background observables by 20%. For massive sterile neutrinos, DES combined with external data improves the upper bound on the mass meff by a factor of 3 compared to previous analyses, giving 95% limits of (ΔNeff,meff)≤(0.28,0.20 eV) when using priors matching a comparable Planck analysis. For modified gravity, we constrain changes to the lensing and Poisson equations controlled by functions Σ(k,z)=Σ0ΩΛ(z)/ΩΛ,0 and μ(k,z)=μ0ΩΛ(z)/ΩΛ,0, respectively, to Σ0=0.6−0.5+0.4 fro

关键词： Cosmological constant Cosmological parameters Cosmology Dark energy Dark matter Galaxies Large scale structure of the Universe Telescopes

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A Component-Based 3D Garment Modeling Algorithm

A Component-Based 3D Garment Modeling Algorithm

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The 9th Textile Bioengineering and Informatics Symposium in Conjunction with the 6th Asian Protective Clothing Conference

作者： Ruo-Mei Wang Gong-Hai Xie Bing-Guang Zhou Fan Zhou National Engineering Research Center of Digital Life State-Province Joint Laboratory of Digital Home Interactive ApplicationsSchool of Data Science & Computer TechnologySun Yat-sen University

virtual garment has a wide range of application in different ***,it is difficult to construct the soft garments with rich styles,complex *** order to generate virtual garment easily,an easy-to-use 3 D garment generation method is proposed in this *** main contribution of our method is use the garment component assemble 3 D garment according to the requirement of consumer or designer.

关键词： Garment Component computer software assembly

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SPT clusters with DES and HST weak lensing. I. Cluster lensing and Bayesian population modeling of multiwavelength cluster datasets

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Physical Review D 2024年第8期110卷 083509页

作者： S. Bocquet S. Grandis L. E. Bleem M. Klein J. J. Mohr M. Aguena A. Alarcon S. Allam S. W. Allen O. Alves A. Amon B. Ansarinejad D. Bacon M. Bayliss K. Bechtol M. R. Becker B. A. Benson G. M. Bernstein M. Brodwin D. Brooks A. Campos R. E. A. Canning J. E. Carlstrom A. Carnero Rosell M. Carrasco Kind J. Carretero R. Cawthon C. Chang R. Chen A. Choi J. Cordero M. Costanzi L. N. da Costa M. E. S. Pereira C. Davis J. DeRose S. Desai T. de Haan J. De Vicente H. T. Diehl S. Dodelson P. Doel C. Doux A. Drlica-Wagner K. Eckert J. Elvin-Poole S. Everett I. Ferrero A. Ferté A. M. Flores J. Frieman J. García-Bellido M. Gatti G. Giannini M. D. Gladders D. Gruen R. A. Gruendl I. Harrison W. G. Hartley K. Herner S. R. Hinton D. L. Hollowood W. L. Holzapfel K. Honscheid N. Huang E. M. Huff D. J. James M. Jarvis G. Khullar K. Kim R. Kraft K. Kuehn N. Kuropatkin F. Kéruzoré S. Lee P.-F. Leget N. MacCrann G. Mahler A. Mantz J. L. Marshall J. McCullough M. McDonald J. Mena-Fernández R. Miquel J. Myles A. Navarro-Alsina R. L. C. Ogando A. Palmese S. Pandey A. Pieres A. A. Plazas Malagón J. Prat M. Raveri C. L. Reichardt J. Roberson R. P. Rollins A. K. Romer C. Romero A. Roodman A. J. Ross E. S. Rykoff L. Salvati C. Sánchez E. Sanchez D. Sanchez Cid A. Saro T. Schrabback M. Schubnell L. F. Secco I. Sevilla-Noarbe K. Sharon E. Sheldon T. Shin M. Smith T. Somboonpanyakul B. Stalder A. A. Stark V. Strazzullo E. Suchyta M. E. C. Swanson G. Tarle C. To M. A. Troxel I. Tutusaus T. N. Varga A. von der Linden N. Weaverdyck J. Weller P. Wiseman B. Yanny B. Yin M. Young Y. Zhang J. Zuntz University Observatory Faculty of Physics Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstr. 25/8 6020 Innsbruck Austria Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Max Planck Institute for Extraterrestrial Physics Gießenbachstr. 1 85748 Garching Germany Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ-20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall Stanford California 94305 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park California 94025 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom School of Physics University of Melbourne Parkville Victoria 3010 Australia Institute of Cosmology and Gravitation University of Portsmouth Portsmouth PO1 3FX United Kingdom Department of Physics University of Cincinnati Cincinnati Ohio 45221 USA Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Fermi National Accelerator Laboratory Batavia Illinois 60510-0500 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Department of Physics and Astronomy University of Missouri 5110 Rockhill Road Kansas City Missouri 64110 USA Department of Physics and Astronomy University Coll

We present a Bayesian population modeling method to analyze the abundance of galaxy clusters identified by the South Pole Telescope (SPT) with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). We discuss and validate the modeling choices with a particular focus on a robust, weak-lensing-based mass calibration using DES data. For the DES Year 3 data, we report a systematic uncertainty in weak-lensing mass calibration that increases from 1% at z=0.25 to 10% at z=0.95, to which we add 2% in quadrature to account for uncertainties in the impact of baryonic effects. We implement an analysis pipeline that joins the cluster abundance likelihood with a multiobservable likelihood for the Sunyaev-Zel’dovich effect, optical richness, and weak-lensing measurements for each individual cluster. We validate that our analysis pipeline can recover unbiased cosmological constraints by analyzing mocks that closely resemble the cluster sample extracted from the SPT-SZ, SPTpol ECS, and SPTpol 500d surveys and the DES Year 3 and HST-39 weak-lensing datasets. This work represents a crucial prerequisite for the subsequent cosmological analysis of the real dataset.

关键词： Cosmological parameters Gravitational lenses Large scale structure of the Universe

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Utilizing Cat Swarm Optimization in Allocating the Sink Node in the Wireless Sensor Network Environment 3

Utilizing Cat Swarm Optimization in Allocating the Sink Node...

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3rd International Conference on Computing Measurement Control and Sensor Network, CMCSN 2016

作者： Tsai, Pei-Wei Kong, Lingping Vaclav, Snasel Pan, Jeng-Shyang Istanda, Vaci Hu, Zhi-Yong College of Information Science and Engineering Fujian University of Technology Fuzhou China Fujian Provincial Key Laboratory of Big Data Mining and Applications Fujian University of Technology Fuzhou China Innovative Information Industry Research Center Harbin Institute of Technology Shenzhen Graduate School Shenzhen China Department of Computer Science VSB Technical University of Ostrava Ostrava Czech Republic Council of Indigenous Peoples Executive Yuan New Taipei City Taiwan

ISBN: (纸本)9781509010936

A general wireless sensor network (WSN) is a system composed of a large number of sensor nodes. In the WSN system, all sensor nodes are responsible for sensing the interested events and transmitting the related information back to the sink node. The sink node acts like the brain of the whole WSN system for processing the collected data and giving control commands. The position of the sink node directly affects the data transmission efficiency and the distance from the terminal sensor node to the sink node. Thus, choosing the correct place to place the sink node in the whole network is a delicate work. In this paper, we propose a sink node placement method by proposing a newly designed object function and utilizing Cat Swarm Optimization (CSO) to find out the near best location for placing the sink node. The simulation results indicate that our proposed method presents good performance compared with the conventional Particle Swarm Optimization (PSO) algorithm in reducing the overall energy consumption and prolongs the lifetime of network in an efficient way. © 2016 IEEE.

关键词： Sensor nodes

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Dark Energy Survey year 3 results: Constraints on cosmological parameters and galaxy-bias models from galaxy clustering and galaxy-galaxy lensing using the redMaGiC sample

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Physical Review D 2022年第4期106卷 043520-043520页

作者： S. Pandey E. Krause J. DeRose N. MacCrann B. Jain M. Crocce J. Blazek A. Choi H. Huang C. To X. Fang J. Elvin-Poole J. Prat A. Porredon L. F. Secco M. Rodriguez-Monroy N. Weaverdyck Y. Park M. Raveri E. Rozo E. S. Rykoff G. M. Bernstein C. Sánchez M. Jarvis M. A. Troxel G. Zacharegkas C. Chang A. Alarcon O. Alves A. Amon F. Andrade-Oliveira E. Baxter K. Bechtol M. R. Becker H. Camacho A. Campos A. Carnero Rosell M. Carrasco Kind R. Cawthon R. Chen P. Chintalapati C. Davis E. Di Valentino H. T. Diehl S. Dodelson C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner S. Everett A. Farahi A. Ferté P. Fosalba O. Friedrich M. Gatti G. Giannini D. Gruen R. A. Gruendl I. Harrison W. G. Hartley E. M. Huff D. Huterer A. Kovacs P. F. Leget J. McCullough J. Muir J. Myles A. Navarro-Alsina Y. Omori R. P. Rollins A. Roodman R. Rosenfeld I. Sevilla-Noarbe E. Sheldon T. Shin A. Troja I. Tutusaus T. N. Varga 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 D. Brooks D. L. Burke J. Carretero C. Conselice M. Costanzi L. N. da Costa M. E. S. Pereira J. De Vicente J. P. Dietrich P. Doel A. E. Evrard 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 D. J. James T. Jeltema K. Kuehn N. Kuropatkin O. Lahav M. Lima H. Lin M. A. G. Maia J. L. Marshall P. Melchior F. Menanteau C. J. Miller R. Miquel J. J. Mohr R. Morgan A. Palmese F. Paz-Chinchón D. Petravick A. Pieres A. A. Plazas Malagón E. Sanchez V. Scarpine S. Serrano M. Smith M. Soares-Santos E. Suchyta G. Tarle D. Thomas J. Weller Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Department of Astronomy/Steward Observatory University of Arizona 933 North Cherry Avenue Tucson Arizona 85721-0065 USA Lawrence Berkeley National Laboratory 1 Cyclotron Road Berkeley California 94720 USA Department of Applied Mathematics and Theoretical Physics University of Cambridge Cambridge CB3 0WA United Kingdom Institut d’Estudis Espacials de Catalunya (IEEC) 08034 Barcelona Spain Institute of Space Sciences (ICE CSIC) Campus UAB Carrer de Can Magrans s/n 08193 Barcelona Spain Department of Physics Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Center for Cosmology and Astro-Particle Physics The Ohio State University Columbus Ohio 43210 USA Department of Physics University of Arizona Tucson Arizona 85721 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA Kavli Institute for Particle Astrophysics and Cosmology P.O. Box 2450 Stanford University Stanford California 94305 USA SLAC National Accelerator Laboratory Menlo Park California 94025 USA Department of Physics The Ohio State University Columbus Ohio 43210 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 Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT) Madrid Spain Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Kavli Institute for the Physics and Mathematics of the Universe (WPI) UTIAS The University of Tokyo Kashiwa Chiba 277-8583 Japan Department of Physics Duke University Durham North Carolina 27708 USA Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Instituto de Física Teórica Uni

We constrain cosmological parameters and galaxy-bias parameters using the combination of galaxy clustering and galaxy-galaxy lensing measurements from the Dark Energy Survey (DES) year-3 data. We describe our modeling framework and choice of scales analyzed, validating their robustness to theoretical uncertainties in small-scale clustering by analyzing simulated data. Using a linear galaxy-bias model and redMaGiC galaxy sample, we obtain 10% constraints on the matter density of the Universe. We also implement a nonlinear galaxy-bias model to probe smaller scales that includes parametrization based on hybrid perturbation theory and find that it leads to a 17% gain in cosmological constraining power. We perform robustness tests of our methodology pipeline and demonstrate stability of the constraints to changes in the theory model. Using the redMaGiC galaxy sample as foreground lens galaxies and adopting the best-fitting cosmological parameters from DES year-1 data, we find the galaxy clustering and galaxy-galaxy lensing measurements to exhibit significant signals akin to decorrelation between galaxies and mass on large scales, which is not expected in any current models. This likely systematic measurement error biases our constraints on galaxy bias and the S8 parameter. We find that a scale-, redshift- and sky-area-independent phenomenological decorrelation parameter can effectively capture this inconsistency between the galaxy clustering and galaxy-galaxy lensing. We trace the source of this correlation to a color-dependent photometric issue and minimize its impact on our result by changing the selection criteria of redMaGiC galaxies. Using this new sample, our constraints on the S8 parameter are consistent with previous studies and we find a small shift in the Ωm constraints compared to the fiducial redMaGiC sample. We infer the constraints on the mean host-halo mass of the redMaGiC galaxies in this new sample from the large-scale bias constraints, finding the galax

关键词： Cosmological constant Cosmological parameters Dark energy Dark matter Evolution of the Universe General relativity Gravitational lenses Large scale structure of the Universe Optical, UV, & IR astronomy

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Dark energy survey year 3 results: High-precision measurement and modeling of galaxy-galaxy lensing

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Physical Review D 2022年第8期105卷 083528-083528页

作者： J. Prat J. Blazek C. Sánchez I. Tutusaus S. Pandey J. Elvin-Poole E. Krause M. A. Troxel L. F. Secco A. Amon J. DeRose G. Zacharegkas C. Chang B. Jain N. MacCrann Y. Park E. Sheldon G. Giannini S. Bocquet C. To A. Alarcon O. Alves F. Andrade-Oliveira E. Baxter K. Bechtol M. R. Becker G. M. Bernstein H. Camacho A. Campos A. Carnero Rosell M. Carrasco Kind R. Cawthon R. Chen A. Choi J. Cordero M. Crocce C. Davis J. De Vicente H. T. Diehl S. Dodelson C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner S. Everett X. Fang A. Farahi A. Ferté P. Fosalba O. Friedrich M. Gatti D. Gruen R. A. Gruendl I. Harrison W. G. Hartley K. Herner H. Huang E. M. Huff D. Huterer M. Jarvis N. Kuropatkin P.-F. Leget P. Lemos A. R. Liddle J. McCullough J. Muir J. Myles A. Navarro-Alsina A. Porredon M. Raveri M. Rodriguez-Monroy R. P. Rollins A. Roodman R. Rosenfeld A. J. Ross E. S. Rykoff J. Sanchez I. Sevilla-Noarbe T. Shin A. Troja T. N. Varga N. Weaverdyck R. H. Wechsler B. Yanny B. Yin J. Zuntz T. M. C. Abbott M. Aguena S. Allam J. Annis D. Bacon D. Brooks D. L. Burke J. Carretero C. Conselice M. Costanzi L. N. da Costa M. E. S. Pereira S. Desai J. P. Dietrich P. Doel A. E. Evrard 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 D. J. James K. Kuehn O. Lahav H. Lin M. A. G. Maia J. L. Marshall P. Martini P. Melchior F. Menanteau C. J. Miller R. Miquel J. J. Mohr R. Morgan R. L. C. Ogando A. Palmese F. Paz-Chinchón D. Petravick A. A. Plazas Malagón E. Sanchez S. Serrano M. Smith M. Soares-Santos E. Suchyta G. Tarle D. Thomas J. Weller 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 Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Institut d’Estudis Espacials de Catalunya (IEEC) 08034 Barcelona Spain Institute of Space Sciences (ICE CSIC) Campus UAB Carrer de Can Magrans Sin número 08193 Barcelona Spain 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 Astronomy/Steward Observatory University of Arizona 933 North Cherry Avenue Tucson Arizona 85721-0065 USA Department of Physics Duke University Durham North Carolina 27708 USA Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Lawrence Berkeley National Laboratory 1 Cyclotron Road Berkeley California 94720 USA Department of Applied Mathematics and Theoretical Physics University of Cambridge Cambridge CB3 0WA United Kingdom Kavli Institute for the Physics and Mathematics of the Universe (WPI) UTIAS The University of Tokyo Kashiwa Chiba 277-8583 Japan Brookhaven National Laboratory Building 510 Upton New York 11973 USA Institut de Física d’Altes Energies (IFAE) The Barcelona Institute of Science and Technology Campus UAB 08193 Bellaterra (Barcelona) Spain Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 81679 Munich Germany Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA SLAC National Accelerator Laboratory Menlo Park California 94025 USA Argonne National Laboratory 9700 South Cass A

We present and characterize the galaxy-galaxy lensing signal measured using the first three years of data from the Dark Energy Survey (DES Y3) covering 4132 deg2. These galaxy-galaxy measurements are used in the DES Y3 3×2 pt cosmological analysis, which combines weak lensing and galaxy clustering information. We use two lens samples: a magnitude-limited sample and the redmagic sample, which span the redshift range ∼0.2–1 with 10.7 and 2.6 M galaxies, respectively. For the source catalog, we use the metacalibration shape sample, consisting of ≃100 M galaxies separated into four tomographic bins. Our galaxy-galaxy lensing estimator is the mean tangential shear, for which we obtain a total SNR of ∼148 for maglim (∼120 for redmagic), and ∼67 (∼55) after applying the scale cuts of 6 Mpc/h. Thus we reach percent-level statistical precision, which requires that our modeling and systematic-error control be of comparable accuracy. The tangential shear model used in the 3×2 pt cosmological analysis includes lens magnification, a five-parameter intrinsic alignment model, marginalization over a point mass to remove information from small scales and a linear galaxy bias model validated with higher-order terms. We explore the impact of these choices on the tangential shear observable and study the significance of effects not included in our model, such as reduced shear, source magnification, and source clustering. We also test the robustness of our measurements to various observational and systematics effects, such as the impact of observing conditions, lens-source clustering, random-point subtraction, scale-dependent metacalibration responses, point spread function residuals, and B modes.

关键词： Cosmological parameters Dark energy Dark matter Gravitational lenses Large scale structure of the Universe Optical, UV, & IR astronomy

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Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing

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Physical Review D 2022年第2期105卷 023520-023520页

作者： T. M. C. Abbott M. Aguena A. Alarcon S. Allam O. Alves A. Amon F. Andrade-Oliveira J. Annis S. Avila D. Bacon E. Baxter K. Bechtol M. R. Becker G. M. Bernstein S. Bhargava S. Birrer J. Blazek A. Brandao-Souza S. L. Bridle D. Brooks E. Buckley-Geer D. L. Burke H. Camacho A. Campos A. Carnero Rosell M. Carrasco Kind J. Carretero F. J. Castander R. Cawthon C. Chang A. Chen R. Chen A. Choi C. Conselice J. Cordero M. Costanzi M. Crocce L. N. da Costa M. E. da Silva Pereira C. Davis T. M. Davis J. De Vicente J. DeRose S. Desai E. Di Valentino H. T. Diehl J. P. Dietrich S. Dodelson P. Doel C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole S. Everett A. E. Evrard X. Fang A. Farahi E. Fernandez I. Ferrero A. Ferté P. Fosalba O. Friedrich J. Frieman J. García-Bellido M. Gatti E. Gaztanaga D. W. Gerdes T. Giannantonio G. Giannini D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez I. Harrison W. G. Hartley K. Herner S. R. Hinton D. L. Hollowood K. Honscheid B. Hoyle E. M. Huff D. Huterer B. Jain D. J. James M. Jarvis N. Jeffrey T. Jeltema A. Kovacs E. Krause R. Kron K. Kuehn N. Kuropatkin O. Lahav P.-F. Leget P. Lemos A. R. Liddle C. Lidman M. Lima H. Lin N. MacCrann M. A. G. Maia J. L. Marshall P. Martini J. McCullough P. Melchior J. Mena-Fernández F. Menanteau R. Miquel J. J. Mohr R. Morgan J. Muir J. Myles S. Nadathur A. Navarro-Alsina R. C. Nichol R. L. C. Ogando Y. Omori A. Palmese S. Pandey Y. Park F. Paz-Chinchón D. Petravick A. Pieres A. A. Plazas Malagón A. Porredon J. Prat M. Raveri M. Rodriguez-Monroy R. P. Rollins A. K. Romer A. Roodman R. Rosenfeld A. J. Ross E. S. Rykoff S. Samuroff C. Sánchez E. Sanchez J. Sanchez D. Sanchez Cid V. Scarpine M. Schubnell D. Scolnic L. F. Secco S. Serrano I. Sevilla-Noarbe E. Sheldon T. Shin M. Smith M. Soares-Santos E. Suchyta M. E. C. Swanson M. Tabbutt G. Tarle D. Thomas C. To A. Troja M. A. Troxel D. L. Tucker I. Tutusaus T. N. Varga A. R. Walker N. Weaverdyck R. Wechsler J. Weller B. Yanny B. Yin Y. Zhang J. Zuntz Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Laboratório Interinstitucional de e-Astronomia—LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ—20921-400 Brazil Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Instituto de Física Teórica Universidade Estadual Paulista São Paulo 01140-070 Brazil Kavli Institute for Particle Astrophysics and Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Instituto de Fisica Teorica UAM/CSIC Universidad Autonoma de Madrid 28049 Madrid Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth PO1 3FX United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Department of Physics and Astronomy Pevensey Building University of Sussex Brighton BN1 9QH United Kingdom Graduate School of Education Stanford University 160 450 Serra Mall Stanford California 94305 USA Department of Physics Northeastern University Boston Massachusetts 02115 USA Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Instituto de Física Gleb Wataghin Universidade Estadual de Campinas 13083-859 Campinas SP Brazil Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road Manchester M13 9PL United Kingdom Department of Physics and Astronomy University College London Gower Street London WC1E 6BT United Kingdom Department of Astronomy and Astroph

We present the first cosmology results from large-scale structure using the full 5000 deg2 of imaging data from the Dark Energy Survey (DES) data Release 1. We perform an analysis of large-scale structure combining three two-point correlation functions (3×2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions, galaxy–galaxy lensing. To achieve the cosmological precision enabled by these measurements has required updates to nearly every part of the analysis from DES Year 1, including the use of two independent galaxy clustering samples, modeling advances, and several novel improvements in the calibration of gravitational shear and photometric redshift inference. The analysis was performed under strict conditions to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results and tests of the robustness of our results to this decision. We model the data within the flat ΛCDM and wCDM cosmological models, marginalizing over 25 nuisance parameters. We find consistent cosmological results between the three two-point correlation functions; their combination yields clustering amplitude S8=0.776−0.017+0.017 and matter density Ωm=0.339−0.031+0.032 in ΛCDM, mean with 68% confidence limits; S8=0.775−0.024+0.026, Ωm=0.352−0.041+0.035, and dark energy equation-of-state parameter w=−0.98−0.20+0.32 in wCDM. These constraints correspond to an improvement in signal-to-noise of the DES Year 3 3×2pt data relative to DES Year 1 by a factor of 2.1, about 20% more than expected from the increase in observing area alone. This combination of DES data is consistent with the prediction of the model favored by the Planck 2018 cosmic microwave background (CMB) primary anisotropy data, which is quantified with a probability-to-exceed p=0.13–0.48. We find better agreement between DES 3×2pt and Planck than in DES Y1

关键词： Cosmological parameters Cosmology Dark energy Dark matter Large scale structure of the Universe

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Security improvement on a three party password based authenticated key exchange scheme using chaotic maps

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Journal of Information Hiding and Multimedia Signal Processing 2016年第6期7卷 1365-1372页

作者： Chen, Yu Chen, Chien-Ming Pan, Jeng-Shyang Wu, Tsu-Yang Liu, Shuai Fujian Provincial Key Laboratory of Big Data Mining and Applications Fujian University of Technology Fuzhou350118 China Innovative Information Industry Research Center School of Computer Science and Technology Shenzhen Graduate School Harbin Institute of Technology Shenzhen518055 China

Recently, password based authenticated key exchange (or called PAKE for short) with chaotic maps has been received much attention for researchers. In 2013, Xie et al. proposed a three party PAKE scheme (based on chaotic maps). However, their scheme had been proved insecure by Lee et al. in 2015. In this paper, we first show that Xie et al.’s scheme is also vulnerable to a replay attack. To overcome this attack, we further propose an improvement based on their scheme. Finally, we demonstrate the security of our improvement with the BAN logic. © 2016.

关键词： Authentication

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C/2014 UN271(Bernardinelli-Bernstein): The nearly spherical cow of comets

arXiv

引用

arXiv 2021年

作者： Bernardinelli, Pedro H. Bernstein, Gary M. Montet, Benjamin T. Weryk, Robert Wainscoat, Richard Aguena, M. Allam, S. Andrade-Oliveira, F. Annis, J. Avila, S. Bertin, E. Brooks, D. Burke, D.L. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Cawthon, R. Conselice, C. Costanzi, M. Da Costa, L.N. Pereira, M.E.S. De Vicente, J. Diehl, H.T. Everett, S. Ferrero, I. Flaugher, B. Frieman, J. García-Bellido, J. Gaztanaga, E. Gerdes, D.W. Gruen, D. Gruendl, R.A. Gschwend, J. Gutierrez, G. Hinton, S.R. Hollowood, D.L. Honscheid, K. James, D.J. Kuehn, K. Kuropatkin, N. Lahav, O. Maia, M.A.G. Marshall, J.L. Menanteau, F. Miquel, R. Morgan, R. Ogando, R.L.C. Paz-Chinchón, F. Pieres, A. Plazas Malagón, A.A. Rodriguez-Monroy, M. Romer, A.K. Roodman, A. Sanchez, E. Schubnell, M. Serrano, S. Sevilla-Noarbe, I. Smith, M. Soares-Santos, M. Suchyta, E. Swanson, M.E.C. Tarle, G. To, C. Troxel, M.A. Varga, T.N. Walker, A.R. Zhang, Y. Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States School of Physics University of New South Wales SydneyNSW2052 Australia UNSW Data Science Hub University of New South Wales SydneyNSW2052 Australia Dept. of Physics & Astronomy University of Western Ontario 1151 Richmond Street LondonONN6A 3K7 Canada Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Instituto de Fisica Teorica CSIC Universidad Autonoma de Madrid Madrid28049 Spain CNRS UMR 7095 Institut d'Astrophysique de Paris ParisF-75014 France Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d'Astrophysique de Paris ParisF-75014 France Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Center for Astrophysical Surveys National Center for Supercomputing Applications 1205 West Clark St. UrbanaIL61801 United States Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street UrbanaIL61801 United States The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Physics Department University of Wisconsin-Madison 2320 Chamberlin Hall 1150 University Avenue MadisonWI53706-1390 United States Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom University of Nottingham School of Physics and Astronomy NottinghamNG7 2RD U

C/2014 UN271(Bernardinelli-Bernstein) is a comet incoming from the Oort cloud which is remarkable in having the brightest (and presumably largest) nucleus of any well-measured comet, and having been discovered at heliocentric distance rh≈29 au farther than any Oort-cloud member. We describe the properties that can be inferred from images recorded until the first reports of activity in June 2021. The orbit has i=95°, with perihelion of 10.97 au to be reached in 2031, and previous aphelion at 40,400±260 au. Backwards integration of the orbit under a standard Galactic tidal model and known stellar encounters suggests this is a pristine new comet, with a perihelion of q≈18 au on its previous perihelion passage 3.5 Myr ago. The photometric data show an unresolved nucleus with absolute magnitude Hr=8.0, colors that are typical of comet nuclei or Damocloids, and no secular trend as it traversed the range 34-23 au. For r-band geometric albedo pr, this implies a diameter of 150 (pr/0.04)-0.5km. There is strong evidence of brightness fluctuations at ±0.2 mag level, but no rotation period can be discerned. A coma consistent with a "stationary" 1/ρ surface-brightness distribution grew in scattering cross-section at an exponential rate from Afρ ≈ 1 m to ≈ 150 m as the comet approached from 28 to 20 au. The activity is consistent with a simple model of sublimation of a surface species in radiative equilibrium with the Sun. The inferred enthalpy of sublimation matches those of CO2and NH3. More-volatile species - N2, CH4, and CO - must be far less abundant on the sublimating surfaces. © 2021, CC BY-NC-ND.

关键词： Comets

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A Competitive QUasi-Affine TRansformation Evolutionary (C-QUATRE) Algorithm for Global Optimization

A Competitive QUasi-Affine TRansformation Evolutionary (C-QU...

引用

IEEE International Conference on Systems, Man, and Cybernetics

作者： Zhenyu Meng Jeng-Shyang Pan Department of Computer Science and Technology Harbin Institute of Technology Shenzhen Graduate School Shenzhen China 518055 Department of Computer Science and Technology Harbin Institute of Technology Shenzhen Graduate School Shenzhen China 518055 Fujian Provincial Key Laboratory of Data Mining and Applications Fujian University of Technology Fuzhou China 350000

ISBN: (纸本)9781509018987

In this paper, we proposed a Competitive QUasi-Affine TRansformation Evolutionary (C-QUATRE) algorithm. This algorithm is an advancement of a preciously proposed QUATRE algorithm. The QUATRE algorithm is arguably a very powerful stochastic optimization algorithm, and it will appear in CEC2016 conference proceedings with the paper title "QUasi-Affine TRansformation Evolutionary (QUATRE) Algorithm: A Parameter-reduced Differential Evolution Algorithm for Optimization Problem". It conquers some weaknesses of Differential Evolution (DE) algorithm and it has excellent performance even on multi-modal optimization problem. Here in the paper, we advance a C-QUATRE algorithm which uses a pairwise competition mechanism to enhance the performance of the former proposed QUATRE algorithm. The C-QUATRE algorithm is verified both on CEC2013 test suite for realparameter optimization and BBOB2009 framework for blackbox optimization, and experiment results show that the pairwise competition mechanism is very useful for the enhancement of the QUATRE performance over all these benchmarks.

关键词： mechanism enhancement advancement Global optimization algorithms Evolutionary Refractive surgery enhancement BENCHMARKS Optimization algorithms paper Pairwise

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