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arXiv 2018年

作者： Chen, Yao Xia, Weiguo Cao, Ming Lü, Jinhu Department of Computer Science Southwestern University of Finance and Economics Chengdu611130 China School of Control Science and Engineering Dalian University of Technology Dalian116024 China Faculty of Science and Engineering ENTEG University of Groningen Groningen9747 AG Netherlands School of Automation Science and Electrical Engineering State Key Laboratory of Software Development Environment Beijing Advanced Innovation Center for Big Data and Brain Computing Beihang University Beijing100191 China Academy of Mathematics and Systems Science Chinese Academy of Sciences Beijing100190 China

Distributed coordination algorithms (DCA) carry out information processing processes among a group of networked agents without centralized information fusion. Though it is well known that DCA characterized by an SIA (stochastic, indecomposable, aperiodic) matrix generate consensus asymptotically via synchronous iterations, the dynamics of DCA with asynchronous iterations have not been studied extensively, especially when viewed as stochastic processes. This paper aims to show that for any given irreducible stochastic matrix, even non-SIA, the corresponding DCA lead to consensus successfully via random asynchronous iterations under a wide range of conditions on the transition probability. Particularly, the transition probability is neither required to be independent and identically distributed, nor characterized by a Markov chain. Copyright © 2018, The Authors. All rights reserved.

关键词： Stochastic systems

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DP-GEN: A concurrent learning platform for the generation of reliable deep learning based potential energy models

arXiv

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arXiv 2019年

作者： Wang, Haidi Chen, Weijie Zeng, Jinzhe Zhang, Linfeng Wang, Han Zhang, Yuzhi Weinan, E. Yuanpei College of Peking University Beijing100871 China School of Electronic Science and Applied Physics Hefei University of Technology Hefei230601 China Academy for Advanced Interdisciplinary Studies Peking University Beijing100871 China School of Chemistry and Molecular Engineering East China Normal University Shanghai200062 China Program in Applied and Computational Mathematics Princeton University PrincetonNJ United States Laboratory of Computational Physics Institute of Applied Physics and Computational Mathematics Huayuan Road 6 Beijing100088 China Beijing Institute of Big Data Research Beijing100871 China Program in Applied and Computational Mathematics Princeton University PrincetonNJ United States Beijing Institute of Big Data Research Beijing100871 China

In recent years, promising deep learning based interatomic potential energy surface (PES) models have been proposed that can potentially allow us to perform molecular dynamics simulations for large scale systems with quantum accuracy. However, making these models truly reliable and practically useful is still a very non-trivial task. A key component in this task is the generation of datasets used in model training. In this paper, we introduce the Deep Potential GENerator (DP-GEN), an open-source software platform that implements the recently proposed"on-the-fly" learning procedure [Phys. Rev. Materials 3, 023804] and is capable of generating uniformly accurate deep learning based PES models in a way that minimizes human intervention and the computational cost for data generation and model training. DP-GEN automatically and iteratively performs three steps: exploration, labeling, and training. It supports various popular packages for these three steps: LAMMPS for exploration, Quantum Espresso, VASP, CP2K, etc. for labeling, and DeePMD-kit for training. It also allows automatic job submission and result collection on different types of machines, such as high performance clusters and cloud machines, and is adaptive to different job management tools, including Slurm, PBS, and LSF. As a concrete example, we illustrate the details of the process for generating a general-purpose PES model for Cu using DP-GEN. Copyright © 2019, The Authors. All rights reserved.

关键词： Potential energy

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The PLATO mission

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Experimental Astronomy 2025年第3期59卷 1-111页

作者： Rauer, Heike Aerts, Conny Cabrera, Juan Deleuil, Magali Erikson, Anders Gizon, Laurent Goupil, Mariejo Heras, Ana Walloschek, Thomas Lorenzo-Alvarez, Jose Marliani, Filippo Martin-Garcia, César Mas-Hesse, J. Miguel O’Rourke, Laurence Osborn, Hugh Pagano, Isabella Piotto, Giampaolo Pollacco, Don Ragazzoni, Roberto Ramsay, Gavin Udry, Stéphane Appourchaux, Thierry Benz, Willy Brandeker, Alexis Güdel, Manuel Janot-Pacheco, Eduardo Kabath, Petr Kjeldsen, Hans Min, Michiel Santos, Nuno Smith, Alexis Suarez, Juan-Carlos Werner, Stephanie C. Aboudan, Alessio Abreu, Manuel Acuña, Lorena Adams, Moritz Adibekyan, Vardan Affer, Laura Agneray, François Agnor, Craig Aguirre Børsen-Koch, Victor Ahmed, Saad Aigrain, Suzanne Al-Bahlawan, Ashraf Alcacera Gil, Ma de los Angeles Alei, Eleonora Alencar, Silvia Alexander, Richard Alfonso-Garzón, Julia Alibert, Yann Allende Prieto, Carlos Almeida, Leonardo Alonso Sobrino, Roi Altavilla, Giuseppe Althaus, Christian Alvarez Trujillo, Luis Alonso Amarsi, Anish Ammler-von Eiff, Matthias Amôres, Eduardo Andrade, Laerte Antoniadis-Karnavas, Alexandros António, Carlos Aparicio del Moral, Beatriz Appolloni, Matteo Arena, Claudio Armstrong, David Aroca Aliaga, Jose Asplund, Martin Audenaert, Jeroen Auricchio, Natalia Avelino, Pedro Baeke, Ann Baillié, Kevin Balado, Ana Ballber Balagueró, Pau Balestra, Andrea Ball, Warrick Ballans, Herve Ballot, Jerome Barban, Caroline Barbary, Gaële Barbieri, Mauro Barceló Forteza, Sebastià Barker, Adrian Barklem, Paul Barnes, Sydney Barrado Navascues, David Barragan, Oscar Baruteau, Clément Basu, Sarbani Baudin, Frederic Baumeister, Philipp Bayliss, Daniel Bazot, Michael Beck, Paul G. Belkacem, Kevin Bellinger, Earl Benatti, Serena Benomar, Othman Bérard, Diane Bergemann, Maria Bergomi, Maria Bernardo, Pierre Biazzo, Katia Bignamini, Andrea Bigot, Lionel Billot, Nicolas Binet, Martin Biondi, David Biondi, Federico Birch, Aaron C. Bitsch, Bertram Bluhm Ceballos, Paz Victoria Bódi, Attila Bognár, Zsófia Boisse, Isabelle Bolmont, Emeline Bonanno, Alfio Bonavita, Institut für Planetenforschung Deutsches Zentrum für Luft- und Raumfahrt DLR Rutherfordstrasse 2 Berlin 12489 Germany Fachbereich Geowissenschaften Institut für Geologische Freie Universität Berlin Malteserstr. 74-100 Berlin 12249 Germany Institute of Astronomy KU Leuven Leuven Belgium CNRS CNES LAM Aix Marseille University Marseille France Max Planck Institute for Solar System Research Göttingen Germany LESIA Paris Observatory PSL University Sorbonne University Paris Cité University CNRS Meudon France ESTEC European Space Agency Noordwijk Netherlands ESAC European Space Agency Madrid Spain Centro de Astrobiología CSIC-INTA Campus ESAC Madrid Spain Center for Space and Habitability University of Bern Bern Switzerland INAF - Osservatorio Astrofisico di Catania Catania Italy Department of Physics and Astronomy University of Padua Padua Italy Department of Physics University of Warwick Coventry United Kingdom Astronomical Observatory of Padova INAF - Italian National Institute for Astrophysics Padua Italy Armagh Observatory and Planetarium College Hill Armagh United Kingdom Geneve Observatory University of Geneve Geneve Switzerland IAS University of Paris-Saclay Orsay France AlbaNove University Centre Stockholm University Stockholm Sweden Department of Astrophysics University of Vienna Vienna Austria Department of Astronomy University of Sao Paulo Sao Paulo Brazil Astronomical Institute of the Czech Academy of Sciences Ondřejov Czech Republic Department of Physics and Astronomy Aarhus University Aarhus Denmark Institute for Space Research SRON Leiden Netherlands Instituto de Astrofísica e Ciências do Espaço CAUP Universidade do Porto Porto Portugal Departamento de Física e Astronomia Faculdade da Ci ncias Universidade do Porto Porto Portugal Mullard Space Science Laboratory University College London Holmbury Saint Mary United Kingdom Dept. Theoretical Physics and the Cosmos University of Granada Granada Spain Centre for Plan

PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2REarth) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases. © The Author(s) 2025.

关键词： Asteroseismology Exoplanets PLATO mission

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Publisher Correction: Base editors for simultaneous introduction of C-to-T and A-to-G mutations

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Nature biotechnology 2020年第7期38卷 901页

作者： Rina C Sakata Soh Ishiguro Hideto Mori Mamoru Tanaka Kenji Tatsuno Hiroki Ueda Shogo Yamamoto Motoaki Seki Nanami Masuyama Keiji Nishida Hiroshi Nishimasu Kazuharu Arakawa Akihiko Kondo Osamu Nureki Masaru Tomita Hiroyuki Aburatani Nozomu Yachie Synthetic Biology Division Research Center for Advanced Science and Technology University of Tokyo Tokyo Japan. College of Arts and Sciences University of Tokyo Tokyo Japan. Institute for Advanced Biosciences Keio University Tsuruoka Japan. Graduate School of Media and Governance Keio University Fujisawa Japan. Genome Science Division Research Center for Advanced Science and Technology University of Tokyo Tokyo Japan. Biological Data Science Division Research Center for Advanced Science and Technology University of Tokyo Tokyo Japan. Engineering Biology Research Center Kobe University Kobe Japan. Graduate School of Science Technology and Innovation Kobe University Kobe Japan. Department of Biological Sciences School of Science University of Tokyo Tokyo Japan. Faculty of Environment and Information Studies Keio University Fujisawa Japan. Department of Chemical Science and Engineering Graduate School of Engineering Kobe University Kobe Japan. Synthetic Biology Division Research Center for Advanced Science and Technology University of Tokyo Tokyo Japan. yachie@synbiol.rcast.u-tokyo.ac.jp. College of Arts and Sciences University of Tokyo Tokyo Japan. yachie@synbiol.rcast.u-tokyo.ac.jp. Institute for Advanced Biosciences Keio University Tsuruoka Japan. yachie@synbiol.rcast.u-tokyo.ac.jp. Graduate School of Media and Governance Keio University Fujisawa Japan. yachie@synbiol.rcast.u-tokyo.ac.jp. Department of Biological Sciences School of Science University of Tokyo Tokyo Japan. yachie@synbiol.rcast.u-tokyo.ac.jp. PRESTO Japan Science and Technology Agency (JST) Tokyo Japan. yachie@synbiol.rcast.u-tokyo.ac.jp.

An amendment to this paper has been published and can be accessed via a link at the top of the paper.

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Global tracking of marine megafauna space use reveals how to achieve conservation targets

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science (New York, N.Y.) 2025年第6751期388卷 1086-1097页

作者： Ana M M Sequeira Jorge P Rodríguez Sarah A Marley Hannah J Calich Mirjam van der Mheen Michelle VanCompernolle Lucy M Arrowsmith Lauren R Peel Nuno Queiroz Marisa Vedor Ivo da Costa Gonzalo Mucientes Ana Couto Nicolas E Humphries Sara Abalo-Morla Francisco J Abascal Debra L Abercrombie Katya Abrantes F Alberto Abreu-Grobois André S Afonso Pedro Afonso Heidi Ahonen Susanne Åkesson Joanna Alfaro-Shigueto Russel D Andrews Frédéric Angelier Marina Antonopoulou Javier A Arata Gonzalo Araujo Randall Arauz José Manuel Arcos Igor Arregui Haritz Arrizabalaga Marie Auger-Méthé Steffen Bach Fred Bailleul Robin W Baird George H Balazs Susan G Barco Adam Barnett Warren Baverstock Alastair M M Baylis Annalea Beard Juan Bécares Eduardo J Belda Ian Bell Ashley Bennison Scott R Benson Diego Bernal Michael L Berumen Sandra Bessudo Natalia P A Bezerra Antonin V Blaison Gabriela S Blanco Barbara A Block Mark Bolton Mark E Bond Ramón Bonfil Camrin D Braun Annette C Broderick Michael de L Brooke Annabelle M L Brooks Edward J Brooks Ignacio M Bruno Jennifer M Burns Michael E Byrne Steven E Campana Hamish A Campbell Richard A Campbell Aaron Carlisle Ruth H Carmichael Gemma Carroll Paolo Casale Filipe R Ceia Demian D Chapman Taylor K Chapple Jean-Benoit Charrassin Andre Chiaradia John Chisholm Christopher R Clarke Thomas A Clay Christophe Cleguer Elizabeth Clingham Eric E G Clua Jesse E M Cochran Rochelle Constantine Robert W Cooper Estelle Crochelet Michelle Cronin Eduardo Cuevas Kayla P DaCosta Laurent Dagorn Ryan Daly Randall W Davis P J Nico de Bruyn Carlos Delgado-Trejo Thomas Dellinger Solène Derville Stella Diamant Andrew DiMatteo Kara L Dodge Philip D Doherty Michael C Double Alistair D M Dove Thomas K Doyle Michael J Drew Lindsay L Dubbs Clinton A J Duffy Peter H Dutton Ewan W J Edwards Luke D Einoder Mark V Erdmann Eduardo Espinoza Nicole Esteban Ana Isabel Fagundes Chris Feare Steven H Ferguson Luciana C Ferreira Francesco Ferretti John Filmalter Brittany Finucci G Chris Fischer Richard J Fitzpatrick Jorge Fontes Angela Formia Division of Ecology and Evolution Research School of Biology The Australian National University Canberra (Australian Capital Territory) Australia. UWA Oceans Institute and the School of Biological Sciences The University of Western Australia Perth (Western Australia) Australia. Instituto de Física Interdisciplinar y Sistemas Complejos (IFISC) CSIC-UIB Palma de Mallorca Spain. Instituto Mediterráneo de Estudios Avanzados (IMEDEA) CSIC-UIB Esporles Illes Balears Spain. C.A. Illes Balears Universidad Nacional de Educación a Distancia (UNED) Palma Spain. Delegación Territorial en Illes Balears Agencia Estatal de Meteorología (AEMET) Muelle de Poniente s/n Palma Spain. Scotland's Rural College (SRUC) Craibstone Estate Bucksburn Aberdeen UK. Oceans Graduate School and the UWA Oceans Institute The University of Western Australia Perth (Western Australia) Australia. School of Engineering and the UWA Oceans Institute The University of Western Australia Perth (Western Australia) Australia. Department of Biodiversity Conservation and Attractions Biodiversity and Conservation Science Kensington (Western Australia) Australia. Save Our Seas Foundation Geneva Switzerland. The Manta Trust Catemwood House Norwood Lane Corscombe Dorset UK. Centro de Investigação em Biodiversidade e Recursos Genéticos (CIBIO) InBIO Laboratório Associado Campus de Vairão Universidade do Porto Vairão Portugal. BIOPOLIS Program in Genomics Biodiversity and Land Planning Campus de Vairao Vairão Portugal. Instituto de Investigaciones Marinas Consejo Superior de Investigaciones Científicas (IIM-CSIC) Vigo Pontevedra Spain. School of Biological Sciences University of Aberdeen Aberdeen UK. Biomathematics and statistics Scotland The kings building Edinburgh Scotland. Marine Biological Association (MBA) The Laboratory Citadel Hill Plymouth UK. Instituto de Investigación para la Gestión Integrada de Zonas Costeras Universitat Politècnica de València Gandia València Spain. Instituto Español de O

The recent Kunming-Montreal Global Biodiversity Framework (GBF) sets ambitious goals but no clear pathway for how zero loss of important biodiversity areas and halting human-induced extinction of threatened species will be achieved. We assembled a multi-taxa tracking dataset (11 million geopositions from 15,845 tracked individuals across 121 species) to provide a global assessment of space use of highly mobile marine megafauna, showing that 63% of the area that they cover is used 80% of the time as important migratory corridors or residence areas. The GBF 30% threshold (Target 3) will be insufficient for marine megafauna's effective conservation, leaving important areas exposed to major anthropogenic threats. Coupling area protection with mitigation strategies (e.g., fishing regulation, wildlife-traffic separation) will be essential to reach international goals and conserve biodiversity.

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Strikingly high fraction of fast rotators in Magellanic Cloud star clusters

arXiv

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arXiv 2025年

作者： Ettorre, Greta Mazzi, Alessandro Girardi, Léo Marigo, Paola Pastorelli, Giada Goudfrooij, Paul Williams, Benjamin F. Bellini, Andrea Bressan, Alessandro Chen, Yang Correnti, Matteo Costa, Guglielmo Dalcanton, Julianne J. Facchini, Pietro Fouesneau, Morgan Nguyen, Chi Thanh Volpato, Guglielmo Dipartimento di Fisica e Astronomia "Galileo Galilei" Università di Padova Vicolo dell’Osservatorio 3 PadovaI-35122 Italy Dipartimento di Fisica e Astronomia "Augusto Righi" Alma Mater Studiorum Università di Bologna Via Gobetti 93/2 BolognaI-40129 Italy INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Gobetti 93/3 Bologna40129 Italy INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Space Telescope Science Institute 3700 San Martin drive BaltimoreMD21218 United States Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States SISSA International School for Advanced Studies Trieste Italy School of Physics and optoelectronic engineering Anhui University Hefei230601 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone Rome00078 Italy ASI - Space Science Data Center Via del Politecnico RomeI-00133 Italy Université de Lyon Univ Lyon1 ENS de Lyon CNRS Centre de Recherche Astrophysique de Lyon UMR5574 Saint-Genis-LavalF-69230 France Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Mönchhofstr. 12-14 HeidelbergD-69120 Germany Königstuhl 17 Heidelberg69117 Germany INAF - Osservatorio Astronomico di Trieste via Tiepolo 11 Trieste34143 Italy

There has been growing evidence that the rich star clusters in the Magellanic Clouds contain significant fractions of rapidly rotating stars. In this work, we aim to constrain these fractions by studying the colour-magnitude diagrams of four star clusters, selected among those with the most striking signatures of fast rotators. Using isochrones derived from parsec v2.0 stellar tracks, we generate distinct stellar populations, each covering a limited interval of initial rotation rates ωi, referred to as ‘Partial Models’ (PMs). Using optimization algorithms and Monte Carlo Markov Chains, PMs are combined to create the final best-fitting model. In our analysis, we adopt two key assumptions: a uniform age and an isotropic distribution of stellar spin axes within each cluster. The solutions are allowed to explore the entire range of ωi, and different values of age, metallicity, distance and foreground extinction. We find that the rotational velocity distributions in all four clusters reveal a high fraction of stars with ωi close to the break-up value, in all cases. Specifically, the fraction of stars with ωi > 0.7 exceeds 80% in the clusters NGC 419 of the Small Magellanic Cloud (SMC) and NGC 1831 and NGC 1866 of the Large Magellanic Cloud (LMC). For NGC 2203 of the LMC, this fraction is smaller, although it still exceeds 50%, confirming that also this cluster is mainly populated by fast-rotating stars. Copyright © 2025, The Authors. All rights reserved.

关键词： Monte Carlo methods

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Varying the Stiffness and Diffusivity of Rod-Shaped Microgels Independently through Their Molecular Building Blocks

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Angewandte Chemie 2023年第44期135卷

作者： Yonca Kittel Luis P. B. Guerzoni Carolina Itzin Dirk Rommel Matthias Mork Céline Bastard Bernhard Häßel Abdolrahman Omidinia-Anarkoli Silvia P. Centeno Tamás Haraszti Kyoohyun Kim Jochen Guck Alexander J. C. Kuehne Laura De Laporte DWI-Leibniz Institute for Interactive Materials e. V. Forckenbeckstraße 50 52074 Aachen Germany Institute of Technical and Macromolecular Chemistry RWTH Aachen University Worringerweg 1–2 52074 Aachen Germany Institute of Organic and Macromolecular Chemistry Ulm University Albert-Einstein Allee 11 89081 Ulm Germany Contribution: Conceptualization (equal) Data curation (lead) Formal analysis (lead) Investigation (lead) Project administration (lead) Visualization (lead) Writing - original draft (lead) Contribution: Conceptualization (equal) Investigation (supporting) Supervision (supporting) Writing - review & editing (supporting) Contribution: Investigation (supporting) Validation (supporting) Visualization (supporting) Writing - review & editing (equal) Contribution: Conceptualization (supporting) Investigation (supporting) Validation (supporting) Writing - review & editing (equal) Contribution: Conceptualization (supporting) Formal analysis (supporting) Investigation (supporting) Visualization (supporting) Writing - review & editing (equal) Center for Biohybrid Medical Systems (CBMS) Advanced Materials for Biomedicine (AMB) Institute of Applied Medical Engineering (AME) Forckenbeckstraße 55 52074 Aachen Germany Contribution: Conceptualization (supporting) Validation (supporting) Visualization (supporting) Writing - original draft (supporting) Writing - review & editing (equal) Contribution: Formal analysis (equal) Software (lead) Validation (supporting) Visualization (supporting) Writing - original draft (supporting) Writing - review & editing (equal) Max Planck Institute for the Science of Light and Max-Planck-Zentrum für Physik und Medizin Staudtstraße 2 91058 Erlangen Germany Contribution: Conceptualization (supporting) Investigation (supporting) Software (supporting) Validation (supporting) Visualization (supporting) Writing - original draft (supporting) Writing - review & editing (equal) Contribution: Conceptualization (supporting) Writing - review

Microgels are water-swollen, crosslinked polymers that are widely used as colloidal building blocks in scaffold materials for tissue engineering and regenerative medicine. Microgels can be controlled in their stiffness, degree of swelling, and mesh size depending on their polymer architecture, crosslink density, and fabrication method—all of which influence their function and interaction with the environment. Currently, there is a lack of understanding of how the polymer composition influences the internal structure of soft microgels and how this morphology affects specific biomedical applications. In this report, we systematically vary the architecture and molar mass of polyethylene glycol-acrylate (PEG-Ac) precursors, as well as their concentration and combination, to gain insight in the different parameters that affect the internal structure of rod-shaped microgels. We characterize the mechanical properties and diffusivity, as well as the conversion of acrylate groups during photopolymerization, in both bulk hydrogels and microgels produced from the PEG-Ac precursors. Furthermore, we investigate cell-microgel interaction, and we observe improved cell spreading on microgels with more accessible RGD peptide and with a stiffness in a range of 20 kPa to 50 kPa lead to better cell growth.

关键词： Diffusion Internal Structure Mechanical Properties Microfluidics PEG Microgels

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Mysterious odd radio circle near the large magellanic cloud - An intergalactic supernova remnant?

arXiv

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arXiv 2022年

作者： Filipovic, Miroslav D. Payne, J.L. Alsaberi, R.Z.E. Norris, R.P. MacGregor, P.J. Rudnick, L. Koribalski, B.S. Leahy, D. Ducci, L. Kothes, R. Andernach, H. Barnes, L. Bojicic, I.S. Bozzetto, L.M. Brose, R. Collier, J.D. Crawford, Evan J. Crocker, R.M. Dai, S. Galvin, T.J. Haberl, F. Heber, U. Hill, T. Hopkins, A.M. Hurley-Walker, N. Ingallinera, A. Jarrett, T. Kavanagh, P.J. Lenc, E. Luken, K.J. MacKey, D. Manojlovic, P. Maggi, P. Maitra, C. Pennock, C.M. Points, S. Riggi, S. Rowell, G. Safi-Harb, S. Sano, H. Sasaki, M. Shabala, S. Stevens, J. Van Loon, J.Th. Tothill, N.F.H. Umana, G. Uroševic, D. Velovic, V. Vernstrom, T. West, J.L. Wan, Z. School of Science Western Sydney University Locked Bag 1797 Penrith South DC NSW2751 Australia CSIRO Space & Astronomy PO Box 76 EppingNSW1710 Australia Minnesota Institute For Astrophysics School of Physics & Astronomy University of Minnesota 116 Church Street SE MinneapolisMN55455 United States Department of Physics & Astronomy University of Calgary University of Calgary CalgaryABT2N 1N4 Canada Institut Für Astronomie Und Astrophysik Kepler Center For Astro & Particle Physics Universität Tübingen Sand 1 Tübingen72076 Germany ISDC Data Center For Astrophysics Université De Genève 16 Chemin d'Écogia Versoix1290 Switzerland Dominion Radio Astrophysical Observatory Herzberg Astronomy & Astrophysics National Research Council Canada PO Box 248 PentictonBCV2A 6J9 Canada Departamento De Astronomía DCNE Universidad De Guanajuato Cjón. de Jalisco s/n Col. Valenciana Gto. GuanajuatoCP 36023 Mexico Dublin Institute For Advanced Studies Astronomy & Astrophysics Section 31 Fitzwilliam Place Dublin 2D02 XF86 Ireland University of Potsdam Institute of Physics & Astronomy Potsdam14476 Germany Department of Astronomy University of Cape Town Rondebosch7701 South Africa Research School of Astronomy & Astrophysics Australian National University CanberraACT2611 Australia International Centre For Radio Astronomy Research Curtin University BentleyWA6102 Australia Max-Planck-Institut Für Extraterrestrische Physik Gießenbachstraße 1 GarchingD-85748 Germany Remeis Observatory ECAP Universität Erlangen-Nürnberg Sternwartstraße 7 BambergD-96049 Germany Australian Astronomical Optics AAO-Macquarie Faculty of Science & Engineering Macquarie University 105 Delhi Rd North RydeNSW2113 Australia INAF - Osservatorio Astrofisico Di Catania via Santa Sofia 78 CataniaI-95123 Italy Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa School of Cosmic Physics Dublin Institute For Advanced Studies 31 Fitzwilliam

We report the discovery of J0624-6948, a low-surface brightness radio ring, lying between the Galactic Plane and the Large Magellanic Cloud (LMC). It was first detected at 888 MHz with the Australian Square Kilometre Array Pathfinder (ASKAP), and with a diameter of ∼196 arcsec. This source has phenomenological similarities to Odd Radio Circles (ORCs). Significant differences to the known ORCs - a flatter radio spectral index, the lack of a prominent central galaxy as a possible host, and larger apparent size - suggest that J0624-6948 may be a different type of object. We argue that the most plausible explanation for J0624-6948 is an intergalactic supernova remnant due to a star that resided in the LMC outskirts that had undergone a single-degenerate type Ia supernova, and we are seeing its remnant expand into a rarefied, intergalactic environment. We also examine if a massive star or a white dwarf binary ejected from either galaxy could be the supernova progenitor. Finally, we consider several other hypotheses for the nature of the object, including the jets of an active galactic nucleus (AGN) or the remnant of a nearby stellar super-flare. Copyright © 2022, The Authors. All rights reserved.

关键词： Supernovae

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Measurement of ω meson production in pp collisions at = 13 TeV

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Journal of High Energy Physics 2025年第4期2025卷 1-30页

作者： Acharya, S. Adamová, D. Agarwal, A. Aglieri Rinella, G. Aglietta, L. Agnello, M. Agrawal, N. Ahammed, Z. Ahmad, S. Ahn, S. U. Ahuja, I. Akindinov, A. Akishina, V. Al-Turany, M. Aleksandrov, D. Alessandro, B. Alfanda, H. M. Alfaro Molina, R. Ali, B. Alici, A. Alizadehvandchali, N. Alkin, A. Alme, J. Alocco, G. Alt, T. Altamura, A. R. Altsybeev, I. Alvarado, J. R. Anaam, M. N. Andrei, C. Andreou, N. Andronic, A. Andronov, E. Anguelov, V. Antinori, F. Antonioli, P. Apadula, N. Aphecetche, L. Appelshäuser, H. Arata, C. Arcelli, S. Aresti, M. Arnaldi, R. Arneiro, J. G. M. C. A. Arsene, I. C. Arslandok, M. Augustinus, A. Averbeck, R. Azmi, M. D. Baba, H. Badalà, A. Bae, J. Baek, Y. W. Bai, X. Bailhache, R. Bailung, Y. Bala, R. Balbino, A. Baldisseri, A. Balis, B. Banerjee, D. Banoo, Z. Barbasova, V. Barile, F. Barioglio, L. Barlou, M. Barman, B. Barnaföldi, G. G. Barnby, L. S. Barreau, E. Barret, V. Barreto, L. Bartels, C. Barth, K. Bartsch, E. Bastid, N. Basu, S. Batigne, G. Battistini, D. Batyunya, B. Bauri, D. Bazo Alba, J. L. Bearden, I. G. Beattie, C. Becht, P. Behera, D. Belikov, I. Bell Hechavarria, A. D. C. Bellini, F. Bellwied, R. Belokurova, S. Beltran, L. G. E. Beltran, Y. A. V. Bencedi, G. Bensaoula, A. Beole, S. Berdnikov, Y. Berdnikova, A. Bergmann, L. Besoiu, M. G. Betev, L. Bhaduri, P. P. Bhasin, A. Bhat, M. A. Bhattacharjee, B. Bianchi, L. Bianchi, N. Bielčík, J. Bielčíková, J. Bigot, A. P. Bilandzic, A. Biro, G. Biswas, S. Bize, N. Blair, J. T. Blau, D. Blidaru, M. B. Bluhme, N. Blume, C. Boca, G. Bock, F. Bodova, T. Bok, J. Boldizsár, L. Bombara, M. Bond, P. M. Bonomi, G. Borel, H. Borissov, A. Borquez Carcamo, A. G. Bossi, H. Botta, E. Bouziani, Y. E. M. Bratrud, L. Braun-Munzinger, P. Bregant, M. Broz, M. Bruno, G. E. Buckland, M. D. Budnikov, D. Buesching, H. Bufalino, S. Buhler, P. Burmasov, N. Buthelezi, Z. Bylinkin, A. Bysiak, S. A. Cabanillas Noris, J. C. Cabrera, M. F. T. Cai, M. Caines, H. Caliva, A. Calvo Villar, E. Camacho, J. M. M. Camerini, P. Canedo, F. D. M. Cantway, S. L. Carabas, M. Université Clermont Auvergne CNRS/IN2P3 LPC Clermont-Ferrand France Nuclear Physics Institute of the Czech Academy of Sciences Husinec-Řež Czech Republic Variable Energy Cyclotron Centre Homi Bhabha National Institute Kolkata India European Organization for Nuclear Research (CERN) Geneva Switzerland Dipartimento di Fisica dell’Università and Sezione INFN Turin Italy Dipartimento DISAT del Politecnico and Sezione INFN Turin Italy Dipartimento di Fisica e Astronomia dell’Università and Sezione INFN Bologna Italy Department of Physics Aligarh Muslim University Aligarh India Korea Institute of Science and Technology Information Daejeon Republic of Korea Faculty of Science P.J. Šafárik University Košice Slovak Republic Frankfurt Institute for Advanced Studies Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany Research Division and ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Darmstadt Germany INFN Sezione di Torino Turin Italy Central China Normal University Wuhan China Instituto de Física Universidad Nacional Autónoma de México Mexico City Mexico University of Houston Houston United States Sungkyunkwan University Suwon City Republic of Korea Department of Physics and Technology University of Bergen Bergen Norway INFN Sezione di Cagliari Cagliari Italy Institut für Kernphysik Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany INFN Sezione di Bari Bari Italy Physik Department Technische Universität München Munich Germany High Energy Physics Group Universidad Autónoma de Puebla Puebla Mexico Horia Hulubei National Institute of Physics and Nuclear Engineering Bucharest Romania University of Derby Derby United Kingdom Universität Münster Institut für Kernphysik Münster Germany Physikalisches Institut Ruprecht-Karls-Universität Heidelberg Heidelberg Germany INFN Sezione di Padova Padova Italy INFN Sezione di Bologna Bologna Italy Lawrence Berkeley National Laboratory Berkeley United Sta

The pT-differential cross section of ω meson production in pp collisions at $$ \sqrt{s} $$ = 13 TeV at midrapidity (|y| < 0.5) was measured with the ALICE detector at the LHC, covering an unprecedented transverse-momentum range of 1.6 < pT < 50 GeV/c. The meson is reconstructed via the ω → π+π−π0 decay channel. The results are compared with various theoretical calculations: PYTHIA8.2 with the Monash 2013 tune overestimates the data by up to 50%, whereas good agreement is observed with Next-to-Leading Order (NLO) calculations incorporating ω fragmentation using a broken SU(3) model. The ω/π0 ratio is presented and compared with theoretical calculations and the available measurements at lower collision energies. The presented data triples the pT ranges of previously available measurements. A constant ratio of Cω/π0 = 0.578 ± 0.006 (stat.) ± 0.013 (syst.) is found above a transverse momentum of 4 GeV/c, which is in agreement with previous findings at lower collision energies within the systematic and statistical uncertainties.

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Dense matter with eXTP

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science China(Physics,Mechanics & Astronomy) 2019年第2期62卷 28-44页

作者： Anna L.Watts WenFei Yu Juri Poutanen Shu Zhang Sudip Bhattacharyya Slavko Bogdanov Long Ji Alessandro Patruno Thomas E.Riley Pavel Bakala Altan Baykal Federico Bernardini Ignazio Bombaci Edward Brown Yuri Cavecchi Deepto Chakrabarty Jér?me Chenevez Nathalie Degenaar Melania Del Santo Tiziana Di Salvo Victor Doroshenko Maurizio Falanga Robert D.Ferdman Marco Feroci Angelo F.Gambino MingYu Ge Svenja K.Greif Sebastien Guillot Can Gungor Dieter H.Hartmann Kai Hebeler Alexander Heger Jeroen Homan Rosario Iaria Jean in 't Zand Oleg Kargaltsev Aleksi KurkelaTheoretical Physics Department CERN XiaoYu Lai Ang Li XiangDong Li ZhaoSheng Li Manuel Linares FangJun Lu Simin Mahmoodifar Mariano Méndez M.Coleman Miller Sharon Morsink Joonas N?ttil? Andrea Possenti Chanda Prescod-Weinstein JinLu Qu Alessandro Riggio Tuomo Salmi Andrea Sanna Andrea Santangelo Hendrik Schatz Achim Schwenk LiMing Song Eva?rámková Benjamin Stappers Holger Stiele Tod Strohmayer Ingo Tews Laura Tolos Gabriel T?r?k David Tsang Martin Urbanec Andrea Vacchi RenXin Xu YuPeng Xu Silvia Zane GuoBao Zhang ShuangNan Zhang WenDa Zhang ShiJie Zheng Xia Zhou Anton Pannekoek Institute for Astronomy University of Amsterdam Shanghai Astronomical Observatory Tuorla Observatory Department of Physics and Astronomy University of Turku Nordita KTH Royal Institute of Technology and Stockholm University Institute of High Energy Physics Chinese Academy Sciences Tata Institute of Fundamental Research Columbia Astrophysics Laboratory Columbia University Institut für Astronomie und Astrophysik Tübingen Universit?t Tübingen Leiden Observatory Leiden University Research Center for Computational Physics and Data Processing Silesian University in Opava Physics Department Middle East Technical University INAF Osservatorio Astronomico di Roma New York University Abu Dhabi Dipartimento di Fisica Enrico Fermi University of Pisa INFN Italian National Institute for Nuclear Physics Department of Physics and Astronomy Michigan State University Department of Astrophysical Sciences Princeton University Mathematical Sciences and STAG Research Centre University of Southampton MIT Kavli Institute for Astrophysics and Space Research DTU Space Technical University of Denmark INAF/IASF Palermo via Ugo La Malfa 153 Universita degli Studi di Palermo Dipartimento di Fisica e Chimica International Space Science Institute (ISSI) Faculty of Science University of East Anglia INAF Istituto di Astrofisica e Planetologie Spaziali Institut für Kernphysik Technische Universit?t Darmstadt ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Instituto de Astrof'?sica Pontificia Universidad Católica de Chile Department of Physics & Astronomy Kinard Lab of Physics Clemson University School of Physics and Astronomy Monash University SRON Netherlands Institute for Space Research Department of Physics The George Washington University Faculty of Science and Technology University of Stavanger School of Physics and Mechanical & Electrical Engineering Hubei University of Education Department of Astronomy Xiamen University (Haiyun Campus) School of Astronomy and Space

In this White Paper we present the potential of the Enhanced X-ray Timing and Polarimetry(eXTP) mission for determining the nature of dense matter; neutron star cores host an extreme density regime which cannot be replicated in a terrestrial laboratory. The tightest statistical constraints on the dense matter equation of state will come from pulse profile modelling of accretion-powered pulsars, burst oscillation sources, and rotation-powered pulsars. Additional constraints will derive from spin measurements, burst spectra, and properties of the accretion flows in the vicinity of the neutron star. Under development by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of sciences, the eXTP mission is expected to be launched in the mid 2020 s.

关键词： neutron X-rays dense matter equation of state

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