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arXiv 2023年

作者： Bom, C.R. Annis, J. Garcia, A. Palmese, A. Sherman, N. Soares-Santos, M. Santana-Silva, L. Morgan, R. Bechtol, K. Davis, T. Diehl, H.T. Allam, S.S. Bachmann, T.G. Fraga, B.M.O. García-Bellido, J. Gill, M.S.S. Herner, K. Kilpatrick, C.D. Makler, M. Olivares, F.E. Pereira, M.E.S. Pineda, J. Santos, A. Tucker, D.L. Wiesner, M.P. Aguena, M. Alves, O. Bacon, D. Bernardinelli, P.H. Bertin, E. Bocquet, S. Brooks, D. Kind, M. Carrasco Carretero, J. Conselice, C. Costanzi, M. da Costa, L.N. De Vicente, J. Desai, S. Doel, P. Everett, S. Ferrero, I. Frieman, J. Gatti, M. Gerdes, D.W. Gruen, D. Gruendl, R.A. Gutierrez, G. Hinton, S.R. Hollowood, D.L. Honscheid, K. James, D.J. Kuehn, K. Kuropatkin, N. Melchior, P. Mena-Fernández, J. Menanteau, F. Pieres, A. Malagón, A.A. Plazas Raveri, M. Rodriguez-Monroy, M. Sanchez, E. Santiago, B. Sevilla-Noarbe, I. Smith, M. Suchyta, E. Swanson, M.E.C. Tarle, G. To, C. Weaverdyck, N. Centro Brasileiro de Pesquisas Físicas Rua Dr. Xavier Sigaud 150 RJ Rio de JaneiroCEP 22290-180 Brazil Centro Federal de Educação Tecnológica Celso Suckow da Fonseca Rodovia Mário Covas lote J2 quadra JItaguaí RJ CEP 23810-000 Brazil Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Physics University of Michigan Ann ArborMI48109 United States Department of Physics University of California Berkeley 366 LeConte Hall MC 7300 BerkeleyCA94720 United States NAT-Universidade Cruzeiro do Sul Universidade Cidade de São Paulo Rua Galvão Bueno 868 SP São Paulo01506-000 Brazil Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue MadisonWI53706-1390 United States Legacy Survey of Space and Time Corporation Data Science Fellowship Program School of Mathematics and Physics The University of Queensland BrisbaneQLD4072 Australia Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Instituto de Fisica Teorica UAM CSIC Universidad Autonoma de Madrid Madrid28049 Spain SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States International Center for Advanced Studies Instituto de Ciencias Físicas ECyT-UNSAM & CONICET Buenos Aires1650 Argentina Instituto de Astronomía y Ciencias Planetarias Universidad de Atacama Av. Copayapu 485 Copiapó Chile Hamburger Sternwarte Universität Hamburg Gojenbergsweg 112 Hamburg21029 Germany Departamento de Ciencias Fisicas Universidad Andres Bello Avda. Republica 252 Santiago Chile Nuncio Monseñor Sótero Sanz 100 Providencia Santiago Chile Benedictine University Department of Physics 5700 College Road LisleIL60532 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Institute of Cosmology and Gravitation

We address the problem of optimally identifying all kilonovae detected via gravitational wave emission in the upcoming LIGO/Virgo/KAGRA observing run, O4, which is expected to be sensitive to a factor of ∼ 7 more Binary Neutron Stars (BNS) alerts than previously. Electromagnetic follow-up of all but the brightest of these new events will require > 1 meter telescopes, for which limited time is available. We present an optimized observing strategy for the DECam during O4. We base our study on simulations of gravitational wave events expected for O4 and wide-prior kilonova simulations. We derive the detectabilities of events for realistic observing conditions. We optimize our strategy for confirming a kilonova while minimizing telescope time. For a wide range of kilonova parameters, corresponding to a fainter kilonova compared to GW170817/AT2017gfo we find that, with this optimal strategy, the discovery probability for electromagnetic counterparts with the DECam is ∼ 80% at the nominal BNS gravitational wave detection limit for O4 (190 Mpc), which corresponds to a ∼ 30% improvement compared to the strategy adopted during the previous observing run. For more distant events (∼ 330 Mpc), we reach a ∼ 60% probability of detection, a factor of ∼ 2 increase. For a brighter kilonova model dominated by the blue component that reproduces the observations of GW170817/AT2017gfo, we find that we can reach ∼ 90% probability of detection out to 330 Mpc, representing an increase of ∼ 20%, while also reducing the total telescope time required to follow-up events by ∼ 20%. Copyright © 2023, The Authors. All rights reserved.

关键词： Gravity waves

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Improvement of an Anonymous and Lightweight Authentication Scheme for TMIS

引用

Journal of Applied Mathematics and Physics 2018年第1期6卷 18-28页

作者： Chien-Ming Chen Bin Xiang Eric Wang Ke Tsu-Yang Wu Jerry Chun-Wei Lin Department of Computer Science and Technology Harbin Institute of Technology Shenzhen Graduate School Shenzhen China Fujian University of Technology Fujian Provincial Key Laboratory of Big Data Mining and Applications Fujian University of Technology Fuzhou China National Demonstration Center for Experimental Electronic Information and Electrical Technology Education Fujian University of Technology Fuzhou China

Telecare Medicine Information Systems (TMIS) provides flexible and convenient healthcare for patients. However, the medical data transmitted between patients and doctors are exposed to unsecure public networks. To protect the patient’s personal information, many authentication schemes are designed. Recently, Kang et al. proposed a hash based authentication schemes for TMIS and claimed that it could resist various attacks. However, we find that their proposed scheme is unsecure to traceability attack and user impersonation attack. In order to enhance the security and preserve the efficiency of Kang et al.’s, we proposed a new anonymous and lightweight scheme. The analysis demonstrates that our proposed scheme is superior to Kang et al.’s and the related schemes in security.

关键词： Authentication TMIS Smart Card

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The XMM Cluster Survey: Exploring scaling relations and completeness of the Dark Energy Survey Year 3 redMaPPer cluster catalogue

arXiv

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arXiv 2023年

作者： Upsdell, E.W. Giles, P.A. Romer, A.K. Wilkinson, R. Turner, D.J. Hilton, M. Rykoff, E. Farahi, A. Bhargava, S. Jeltema, T. Klein, M. Bermeo, A. Collins, C.A. Ebrahimpour, L. Hollowood, D. Mann, R.G. Manolopoulou, M. Miller, C.J. Rooney, P.J. Sahlén, Martin Stott, J.P. Viana, P.T.P. Allam, S. Alves, O. Bacon, D. Bertin, E. Bocquet, S. Brooks, D. Burke, D.L. Kind, M. Carrasco Carretero, J. Costanzi, M. da Costa, L.N. Pereira, M.E.S. De Vicente, J. Desai, S. Diehl, H.T. Dietrich, J.P. Everett, S. Ferrero, I. Frieman, J. García-Bellido, J. Gerdes, D.W. Gutierrez, G. Hinton, S.R. Honscheid, K. James, D.J. Kuehn, K. Kuropatkin, N. Lima, M. Marshall, J.L. Mena-Fernández, J. Menanteau, F. Miquel, R. Mohr, J.J. Ogando, R.L.C. Pieres, A. Raveri, M. Rodriguez-Monroy, M. Sanchez, E. Scarpine, V. Sevilla-Noarbe, I. Smith, M. Suchyta, E. Swanson, M.E.C. Tarle, G. To, C. Weaverdyck, N. Weller, J. Wiseman, P. Department of Physics and Astronomy University of Sussex BrightonBN1 9QH United Kingdom Astrophysics Research Centre University of KwaZulu-Natal Westville Campus Durban4041 South Africa School of Mathematics Statistics and Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 Stanford CA94305 United States Department of Statistics and Data Sciences The University of Texas at Austin AustinTX78712 United States AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France Santa Cruz Institute for Particle Physics University of California Santa Cruz 1156 High St Santa CruzCA95064 United States Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Astrophysics Research Institute Liverpool John Moores University Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas Porto4150-762 Portugal Departamento de Física e Astronomia Faculdade de Ciências Universidade do Porto Rua do Campo Alegre 687 Porto4169-007 Portugal Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Astronomy Department University of Michigan Ann ArborMI48109 United States Department of Physics and Astronomy Uppsala University UppsalaSE-751 20 Sweden Department of Physics Lancaster University LancasterLA1 4YB United Kingdom Department of Physics University of Michigan Ann ArborMI48109 United States Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich

We cross-match and compare characteristics of galaxy clusters identified in observations from two sky surveys using two completely different techniques. One sample is optically selected from the analysis of three years of Dark Energy Survey observations using the redMaPPer cluster detection algorithm. The second is X-ray selected from XMM observations analysed by the XMM Cluster Survey. The samples comprise a total area of 57.4 deg2, bounded by the area of 4 contiguous XMM survey regions that overlap the DES footprint. We find that the X-ray selected sample is fully matched with entries in the redMaPPer catalogue, above λ >20 and within 0.1X − TX), luminosity-richness (LX − λ) and temperature-richness (TX − λ) scaling relations. We find that the fitted forms of the LX − TX relations are consistent between the two selection methods and also with other studies in the literature. However, we find tentative evidence for a steepening of the slope of the relation for low richness systems in the X-ray selected sample. When considering the scaling of richness with X-ray properties, we again find consistency in the relations (i.e., LX − λ and TX − λ) between the optical and X-ray selected samples. This is contrary to previous similar works that find a significant increase in the scatter of the luminosity scaling relation for X-ray selected samples compared to optically selected samples. © 2023, CC BY.

关键词： Luminance

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Robust frequent directions with application in online learning

The Journal of Machine Learning Research

引用

The Journal of Machine Learning Research 2019年第1期20卷

作者： Luo Luo Cheng Chen Zhihua Zhang Wu-Jun Li Tong Zhang Department of Computer Science and Engineering Shanghai Jiao Tong University Shanghai China National Engineering Lab for Big Data Analysis and Applications School of Mathematical Sciences Peking University Beijing China National Key Laboratory for Novel Software Technology Collaborative Innovation Center of Novel Software Technology and Industrialization Department of Computer Science and Technology Nanjing University Nanjing China Computer Science & Mathematics Hong Kong University of Science and Technology Hong Kong

The frequent directions (FD) technique is a deterministic approach for online sketching that has many applications in machine learning. The conventional FD is a heuristic procedure that often outputs rank deficient matrices. To overcome the rank deficiency problem, we propose a new sketching strategy called robust frequent directions (RFD) by introducing a regularization term. RFD can be derived from an optimization problem. It updates the sketch matrix and the regularization term adaptively and jointly. RFD reduces the approximation error of FD without increasing the computational cost. We also apply RFD to online learning and propose an effective hyperparameter-free online Newton algorithm. We derive a regret bound for our online Newton algorithm based on RFD, which guarantees the robustness of the algorithm. The experimental studies demonstrate that the proposed method outperforms state-of-the-art second order online learning algorithms.

关键词： frequent directions matrix approximation online Newton algorithm online convex optimization sketching

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Collaborative Experience between Scientific Software Projects using Agile Scrum Development

arXiv

引用

arXiv 2021年

作者： Baxter, A.L. BenZvi, S.Y. Bonivento, W. Brazier, A. Clark, M. Coleiro, A. Collom, D. Colomer-Molla, M. Cousins, Bryce Orellana, A. Delgado Dornic, D. Ekimtcov, V. ElSayed, S. Rosso, A. Gallo Godwin, P. Griswold, S. Habig, A. Hill, R. Horiuchi, S. Howell, D.A. Johnson, M.W.G. Jurić, M. Kneller, J.P. Kopec, A. Kopper, C. Kulikovskiy, V. Lamoureux, M. Lang, R.F. Li, S. Lincetto, M. Lindstrom, W. Linvill, M.W. McCully, C. Migenda, J. Milisavljevic, D. Nelson, S. Novoseltseva, R. O'Sullivan, E. Petravick, D. Pointon, B.W. Raj, N. Renshaw, A. Rumleskie, J. Sonley, T. Tapia, R. Tseng, J.C.L. Tunnell, C.D. Vannoye, G. Vigorito, C.F. Virtue, C.J. Weaver, C. Weil, K.E. Winslow, L. Wolski, R. Xu, X.J. Xu, Y. Department of Physics and Astronomy Purdue University West LafayetteIN47907 United States Department of Physics and Astronomy University of Rochester RochesterNY14627 United States INFN sezione di Cagliari Istituto Nazionale Complesso Universitario di Monserrato - S.P. per Sestu Km 0.700 Monserrato CagliariI-09042 Italy Center for Advanced Computing Cornell University IthacaNY14853 United States Université de Paris CNRS AstroParticule et Cosmologie ParisF-75013 France Las Cumbres Observatory GoletaCA93117 United States c/ Catedrático José Beltrán Paterna Valencia2 E-46980 Spain Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Department of Physics The Pennsylvania State University University ParkPA16802 United States Pontificia Universidad Catolica de Chile Región Metropolitana Santiago Chile Aix Marseille Univ CNRS IN2P3 CPPM Marseille France National Center for Supercomputing Applications University of Illinois at Urbana-Champaign UrbanaIL61801 United States Department of Computer Science University of California Santa BarbaraCA93106 United States Department of Physics Laurentian University SudburyONP3E 2C6 Canada Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics and Astronomy University of Minnesota Duluth DuluthMN55812 United States Center for Neutrino Physics Department of Physics Virginia Tech BlacksburgVA24061 United States University of California Santa BarbaraCA93106 United States DiRAC Institute and the Department of Astronomy University of Washington SeattleWA98195 United States Department of Physics NC State University RaleighNC27695 United States Department of Physics and Astronomy Michigan State University East LansingMI48824 United States INFN Sezione di Genova Via Dodecaneso 33 Genova16146 Italy INFN Sezione di Padova Università di Padova D

Developing sustainable software for the scientific community requires expertise in software engineering and domain science. This can be challenging due to the unique needs of scientific software, the insufficient resources for software engineering practices in the scientific community, and the complexity of developing for evolving scientific contexts. While open-source software can partially address these concerns, it can introduce complicating dependencies and delay development. These issues can be reduced if scientists and software developers collaborate. We present a case study wherein scientists from the SuperNova Early Warning System collaborated with software developers from the Scalable Cyberinfrastructure for Multi-Messenger Astrophysics project. The collaboration addressed the difficulties of open-source software development, but presented additional risks to each team. For the scientists, there was a concern of relying on external systems and lacking control in the development process. For the developers, there was a risk in supporting a user-group while maintaining core development. These issues were mitigated by creating a second Agile Scrum framework in parallel with the developers’ ongoing Agile Scrum process. This Agile collaboration promoted communication, ensured that the scientists had an active role in development, and allowed the developers to evaluate and implement the scientists’ software requirements. The collaboration provided benefits for each group: the scientists actuated their development by using an existing platform, and the developers utilized the scientists’ use-case to improve their systems. This case study suggests that scientists and software developers can avoid scientific computing issues by collaborating and that Agile Scrum methods can address emergent concerns. Copyright © 2021, The Authors. All rights reserved.

关键词： Open source software

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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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Dark Energy Survey Year 3 Results: Mis-centering calibration and X-ray-richness scaling relations in redMaPPer clusters

arXiv

引用

arXiv 2023年

作者： Kelly, P. Jobel, J. Eiger, O. Abd, A. Jeltema, T.E. Giles, P. Hollowood, D.L. Wilkinson, R.D. Turner, D.J. Bhargava, S. Everett, S. Farahi, A. Romer, A.K. Rykoff, E.S. Wang, F. Bocquet, S. Cross, D. Faridjoo, R. Franco, J. Gardner, G. Kwiecien, M. Laubner, D. McDaniel, A. O’Donnell, J.H. Sanchez, L. Schmidt, E. Sripada, S. Swart, A. Upsdell, E. Webber, A. Aguena, M. Allam, S. Alves, O. Bacon, D. Brooks, D. Burke, D.L. Rosell, A. Carnero Carretero, J. Collins, C.A. Costanzi, M. da Costa, L.N. Pereira, M.E.S. Davis, T.M. Doel, P. Ferrero, I. Frieman, J. García-Bellido, J. Giannini, G. Gruen, D. Gruendl, R.A. Hilton, M. Hinton, S.R. Honscheid, K. James, D.J. Kuehn, K. Mann, R.G. Marshall, J.L. Mena-Fernández, J. Miller, C.J. Miquel, R. Myles, J. Palmese, A. Pieres, A. Malagón, A.A. Plazas Rooney, P.J. Sahlen, M. Sanchez, E. Cid, D. Sanchez Schubnell, M. Sevilla-Noarbe, I. Smith, M. Stott, J.P. Suchyta, E. Swanson, M.E.C. Tarle, G. To, C. Viana, P.T.P. Weaverdyck, N. Wiseman, P. University of California Santa Cruz Santa CruzCA95064 United States University of California Davis 1 Shields Ave DavisCA95616 United States Santa Cruz Institute for Particle Physics Santa CruzCA95064 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Swinburne University of Technology John St HawthornVIC3122 Australia Department of Physics and Astronomy Pevensey Building University of Sussex BrightonBN1 9QH United Kingdom 2 place Maurice-Quentin Paris France Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Dr. PasadenaCA91109 United States Departments of Statistics and Data Science University of Texas at Austin AustinTX78757 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Los Altos High School United States University of California Berkeley University Avenue and Oxford St BerkeleyCA94720 United States University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Homestead High School United States De Anza College 21250 Stevens Creek Blvd CupertinoCA United States Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States California State University San Marcos 333 S Twin Oaks Valley Rd San MarcosCA92096 United States Dougherty Valley High School United States University of New Hampshire 105 Main St DurhamNH03824 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 Department of Physics University of Michigan Ann ArborMI48109 United States Institute of Cosmology and G

We use Dark Energy Survey Year 3 (DES Y3) clusters with archival X-ray data from XMM-Newton and Chandra to assess the centering performance of the redMaPPer cluster finder and to measure key richness observable scaling relations. In terms of centering, we find that 10-20% of redMaPPer clusters are miscentered with no significant difference in bins of low versus high richness (20 40) or redshift (0.2 X-λ scatter of 0.21 ± 0.01. While the scatter in TX-λ is consistent in bins of redshift, we do find modestly different slopes with high-redshift clusters displaying a somewhat shallower relation. Splitting based on richness, we find a marginally larger scatter for our lowest richness bin, 20 © 2023, CC BY.

关键词： Galaxies

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Improvement of an Anonymous and Lightweight Authentication Scheme for TMIS

Improvement of an Anonymous and Lightweight Authentication S...

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作者： Chien-Ming Chen Bin Xiang Eric Wang Ke Tsu-Yang Wu Jerry Chun-Wei Lin Department of Computer Science and Technology Harbin Institute of Technology Shenzhen Graduate School Fujian University of Technology Fujian Provincial Key Laboratory of Big Data Mining and Applications Fujian University of Technology National Demonstration Center for Experimental Electronic Information and Electrical Technology Education Fujian University of Technology

Telecare Medicine Information Systems(TMIS) provides flexible and convenient healthcare for patients. However, the medical data transmitted between patients and doctors are exposed to unsecure public networks. To protect the patient's personal information, many authentication schemes are designed. Recently, Kang et al. proposed a hash based authentication schemes for TMIS and claimed that it could resist various attacks. However, we find that their proposed scheme is unsecure to traceability attack and user impersonation attack. In order to enhance the security and preserve the efficiency of Kang et al.'s, we proposed a new anonymous and lightweight scheme. The analysis demonstrates that our proposed scheme is superior to Kang et al.'s and the related schemes in security.

关键词： Authentication TMIS Smart Card

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A matrix-based implementation of DE algorithm: The compensation and deficiency 30th

A matrix-based implementation of DE algorithm: The compensat...

引用

30th International Conference on Industrial, Engineering, and Other applications of Applied Intelligent Systems, IEA/AIE 2017

作者： Pan, Jeng-Shyang Meng, Zhenyu Xu, Huarong Li, Xiaoqing Fujian Provincial Key Lab of Big Data Mining and Applications Fujian University of Technology Fuzhou China Department of Computer Science and Technology Harbin Institute of Technology Shenzhen Graduate School Shenzhen China Department of Computer Science and Technology Xiamen University of Technology Xiamen China Shenzhen Institute of Advanced Technology Chinese Academy of Sciences Shenzhen China

ISBN: (纸本)9783319600413

Differential Evolution has become a very popular continuous optimization algorithm since its inception as its simplicity, easy coding and good performance over kinds of optimization problems. Difference operator in donor vector calculation is the key feature of DE algorithm. Usually, base vector and difference vectors selection in calculating a donor usually cost extra lines of condition judgement. Moreover, these vectors are not equally selected from the individual population. These lead to more perturbation in optimization performance. To tackling this disadvantage of DE implementation, a matrix-based implementation of DE algorithm is advanced herein this paper. Three commonly used DE implementation approaches in literature are also presented and contrasted. CEC2013 test suites for real-parameter optimization are used as the test-beds for these comparison. Experiment results show that the proposed matrix-based implementation of DE algorithm performs better on optimization performance than the common implementation schemes of DE algorithm with similar time complexity. © Springer International Publishing AG 2017.

关键词： Global optimization

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Cosmological constraints from the tomography of DES-Y3 galaxies with CMB lensing from ACT DR4

arXiv

引用

arXiv 2023年

作者： Marques, G.A. Madhavacheril, M.S. Darwish, O. Shaikh, S. Aguena, M. Alves, O. Avila, S. Bacon, D. Baxter, E.J. Bechtol, K. Becker, M.R. Bertin, E. Blazek, J. Bond, J. Richard Brooks, D. Cai, H. Calabrese, E. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Cawthon, R. Crocce, M. da Costa, L.N. Pereira, M.E.S. De Vicente, J. Desai, S. Diehl, H.T. Doel, P. Doux, C. Drlica-Wagner, A. Dunkley, J. Elvin-Poole, J. Everett, S. Ferraro, Simone Ferrero, I. Flaugher, B. Fosalba, P. García-Bellido, J. Gatti, M. Giannini, G. Gluscevic, V. Gruen, D. Gruendl, R.A. Gutierrez, G. Harrison, I. Hill, J. Colin Hinton, S.R. Hollowood, D.L. Honscheid, K. Huterer, D. Jeffrey, N. Kim, J. Kuehn, K. Lahav, O. Lemos, P. Lima, M. Huffenberger, K.M. MacCrann, N. Marshall, J.L. Mena-Fernández, J. Miquel, R. Mohr, J.J. Moodley, K. Muir, J. Naess, S. Nati, F. Page, L.A. Palmese, A. Malagón, A.A. Plazas Porredon, A. Prat, J. Qu, F.J. Raveri, M. Ross, A.J. Rykoff, E.S. Farren, G.S. Samuroff, S. Sanchez, E. Schubnell, M. Sehgal, N. Sevilla-Noarbe, I. Sheldon, E. Sherwin, B.D. Sifón, C. Smith, M. Spergel, D.N. Staggs, S.T. Suchyta, E. Tarle, G. To, C. Van Engelen, A. Weaverdyck, N. Weller, J. Wenzl, L. Wiseman, P. Wollack, E.J. Yanny, B. Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Physics Florida State University TallahasseeFL32306 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Centre for the Universe Perimeter Institute WaterlooONN2L 2Y5 Canada Université de Genève Département de Physique Théorique Centre for Astroparticle Physics 24 quai Ernest-Ansermet Genève 4CH-1211 Switzerland School of Earth and Space Exploration Arizona State University TempeAZ85287 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Department of Physics University of Michigan Ann ArborMI48109 United States The Barcelona Institute of Science and Technology Campus UAB Barcelona Bellaterra08193 Spain Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive HonoluluHI96822 United States Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue MadisonWI53706-1390 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States 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 CITA University of Toronto TorontoONM5S 3H8 Canada Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Physics and Astronomy University of Pittsburgh PittsburghPA15260 United States School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Instituto de Astrofisica de Canarias Tenerife La LagunaE-38205 Spain Universidad de La Laguna

We present a measurement of the cross-correlation between the MAGLIM galaxies selected from the Dark Energy Survey (DES) first three years of observations (Y3) and cosmic microwave background (CMB) lensing from the Atacama Cosmology Telescope (ACT) data Release 4 (DR4), reconstructed over ∼ 436 deg2 of the sky. Our galaxy sample, which covers ∼ 4143 deg2, is divided into six redshift bins spanning the redshift range of 0.20 8 compared to results from measurements of CMB anisotropies by the Planck satellite, although at a mild level ( Copyright © 2023, The Authors. All rights reserved.

关键词： Galaxies

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