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arXiv 2025年

作者： Mertens, F.G. Mevius, M. Koopmans, L.V.E. Offringa, A.R. Zaroubi, S. Acharya, A. Brackenhoff, S.A. Ceccotti, E. Chapman, E. Chege, K. Ciardi, B. Ghara, R. Ghosh, S. Giri, S.K. Hothi, I. Höfer, C. Iliev, I.T. Jelić, V. Ma, Q. Mellema, G. Munshi, S. Pandey, V.N. Yatawatta, S. LUX Observatoire de Paris PSL Research University CNRS Sorbonne Université ParisF-75014 France Astron PO Box 2 Dwingeloo7990 AA Netherlands Kapteyn Astronomical Institute University of Groningen PO Box 800 Groningen9700 AV Netherlands Department of Natural Sciences The Open University of Israel 1 University Road PO Box 808 Ra’anana4353701 Israel Max-Planck Institute for Astrophysics Karl-Schwarzschild-Straße 1 Garching85748 Germany INAF – Istituto di Radioastronomia Via P. Gobetti 101 Bologna40129 Italy School of Physics and Astronomy The University of Nottingham University Park NottinghamNG7 2RD United Kingdom Department of Physical Sciences Indian Institute of Science Education and Research Kolkata WB Mohanpur741 246 India Van Swinderen Institute for Particle Physics and Gravity University of Groningen Nijenborgh 4 Groningen9747 AG Netherlands Nordita KTH Royal Institute of Technology Stockholm University Hannes Alfvéns väg 12 StockholmSE-106 91 Sweden Laboratoire de Physique de l’Ecole Normale Supérieure ENS Université PSL CNRS Sorbonne Université Université de Paris ParisF-75005 France Astronomy Centre Department of Physics and Astronomy Pevensey II Building University of Sussex BrightonBN1 9QH United Kingdom Ruđer Bošković Institute Bijenička cesta 54 Zagreb10000 Croatia School of Physics and Electronic Science Guizhou Normal University Guiyang550001 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden

We present new upper limits on the 21-cm signal power spectrum from the Epoch of Reionization (EoR), at redshifts z ≈ 10.1, 9.1, and 8.3, based on reprocessed observations from the Low-Frequency Array (LOFAR). The analysis incorporates significant enhancements in calibration methods, sky model subtraction, radio-frequency interference (RFI) mitigation, and an improved signal separation technique using machine learning to develop a physically motivated covariance model for the 21-cm signal. These advancements have markedly reduced previously observed excess power due to residual systematics, bringing the measurements closer to the theoretical thermal noise limit across the entire k-space. Using comparable observational data, we achieve a 2 to 4-fold improvement over our previous LOFAR limits, with best upper limits of Δ221 2 at k = 0.076 ℎ cMpc−1, Δ221 2 at k = 0.076 ℎ cMpc−1 and Δ221 2 at k = 0.083 ℎ cMpc−1 at redshifts z ≈ 10.1, 9.1, and 8.3, respectively. These new multi-redshift upper limits provide new constraints that can be used to refine our understanding of the astrophysical processes during the EoR. Comprehensive validation tests, including signal injection, were performed to ensure the robustness of our methods. The remaining excess power is attributed to residual foreground emissions from distant sources, beam model inaccuracies, and low-level RFI. We discuss ongoing and future improvements to the data processing pipeline aimed at further reducing these residuals, thereby enhancing the sensitivity of LOFAR observations in the quest to detect the 21-cm signal from the EoR. © 2025, CC BY.

关键词： Cosmology

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Is fixed-node diffusion quantum Monte Carlo reproducible?

arXiv

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arXiv 2025年

作者： Pia, Flaviano Della Shi, Benjamin X. Al-Hamdani, Yasmine S. Alfè, Dario Anderson, Tyler A. Barborini, Matteo Benali, Anouar Casula, Michele Drummond, Neil Dubecký, Matúš Filippi, Claudia Kent, Paul R.C. Krogel, Jaron T. Ríos, Pablo López Lüchow, Arne Luo, Ye Michaelides, Angelos Mitas, Lubos Nakano, Kousuke Needs, Richard Per, Manolo C. Scemama, Anthony Schultze, Jil Shinde, Ravindra Slootman, Emiel Sorella, Sandro Tkatchenko, Alexandre Towler, Mike Umrigar, C.J. Wagner, Lucas K. Wheeler, William A. Zhou, Haihan Zen, Andrea Yusuf Hamied Department of Chemistry University of Cambridge CambridgeCB2 1EW United Kingdom Department of Earth Sciences University College London LondonWC1E 6BT United Kingdom Dipartimento di Fisica Ettore Pancini Università di Napoli Federico II Monte S. Angelo NapoliI-80126 Italy Laboratory of Atomic and Solid State Physics Cornell University IthacaNY14853 United States HPC Platform University of Luxembourg Esch-sur-AlzetteL-4365 Luxembourg Computational Science Division Argonne National Laboratory LemontIL United States Sorbonne Université CNRS UMR 7590 MNHN 4 Place Jussieu Paris75252 France Department of Physics Lancaster University LancasterLA1 4YB United Kingdom Department of Physics Faculty of Science University of Ostrava 30. Dubna 22 Ostrava701 03 Czech Republic MESA+ Institute for Nanotechnology University of Twente Enschede7500 AE Netherlands Computational Sciences and Engineering Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Materials Science and Technology Division Oak Ridge National Laboratory Oak RidgeTN37831 United States Max Planck Institute for Solid State Research Heisenbergstr. 1 Stuttgart70569 Germany Institute of Physical Chemistry RWTH Aachen University Landoltweg 2 Aachen52074 Germany Department of Physics North Carolina State University RaleighNC27695-8202 United States 1-2-1 Sengen Tsukuba Ibaraki305-0047 Japan Theory of Condensed Matter Group Cavendish Laboratory J. J. Thomson Avenue CambridgeCB3 0HE United Kingdom CSIRO Data61 ClaytonVIC3168 Australia Université de Toulouse CNRS UPS Toulouse31062 France International School for Advanced Studies SISSA Trieste34136 Italy Department of Physics and Materials Science University of Luxembourg Luxembourg CityL-1511 Luxembourg The Apuan Alps Centre for Physics Vallico Sotto Italy Department of Physics University of Illinois at Urbana-Champaign UrbanaIL61801 United States Department of Materials Science and Engi

Fixed-node diffusion quantum Monte Carlo (FN-DMC) is a widely-trusted manybody method for solving the Schrödinger equation, known for its reliable predictions of material and molecular properties. Furthermore, its excellent scalabilitywith system complexity and near-perfect utilization of computational power makes FN-DMC ideally positioned to leverage new advances in computing to address increasingly complex scientific problems. Even though the method is widely used as a computational gold standard, reproducibility across the numerous FN-DMC code implementations has yet to be demonstrated. This difficulty stems from the diverse array of DMC algorithms and trial wave functions, compounded by the method's inherent stochastic nature. This study represents a community-wide effort to address the titular question, affirming that: Yes, FN-DMC is reproducible (when handled with care). Using the water-methane dimer as the canonical test case, we compare results from eleven different FN-DMC codes and show that the approximations to treat the non-locality of pseudopotentials are the primary source of the discrepancies between them. In particular, we demonstrate that, for the same choice of determinantal component in the trial wave function, reliable and reproducible predictions can be achieved by employing the T-move (TM), the determinant locality approximation (DLA), or the determinant T-move (DTM) schemes, while the older locality approximation (LA) leads to considerable variability in results. This work lays the foundation to establish accurate and reproducible FN-DMC estimates for all future studies across applications in materials science, physics, chemistry, and biology. © 2025, CC BY.

关键词： Wave functions

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Graph-cut based antialiasing for Doppler ultrasound color flow medical imaging

Graph-cut based antialiasing for Doppler ultrasound color fl...

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2011 IEEE Visual Communications and Image processing, VCIP 2011

作者： Yatchenko, Artem M. Krylov, Andrey S. Gavrilov, Andrey V. Arkhipov, Ivan V. Laboratory of Mathematical Methods of Image Processing Faculty of Computational Mathematics and Cybernetics Lomonosov Moscow State University Russia D.V. Skobeltsyn Institute of Nuclear Physics Lomonosov Moscow State University Russia B.V. Petrovsky National Research Centre of Surgery Moscow Russia

An unwrapping method for Doppler ultrasound color flow medical images has been developed. It is based on a image digitizing procedure to construct the areas graph. The minimization unwrapping procedure of the velocity... 详细信息

ISBN: (纸本)9781457713200

关键词： Medical imaging

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Theoretical and experimental investigation of the near field under ordered silica spheres on substrate

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Applied physics A: Materials Science and processing 2009年第2期96卷 459-466页

作者： Huang, S.M. Wang, Z.A. Sun, Z. Wang, Z.B. Luk'yanchuk, Boris Department of physics East China Normal University Ministry of Education North Zhongshan Rd. 3663 Shanghai 200062 China Laser Processing Research Centre School of Mechanical Aerospace and Civil Engineering University of Manchester Sackville Street Manchester M60 1QD United Kingdom Data Storage Institute DSI Building 5 Engineering Drive 1 Singapore 117608 Singapore

Investigation on the optical resonance and near field effects of a 2D periodic dielectric spheres on metallic surfaces by combining theoretical calculations with experimental studies were carried out. The light scattering and coupling was numerically studied. Nanostructures were fabricated on the metallic surfaces using these arrays of micro- and nano-spheres with a single laser pulse (KrF, λ=248 nm). The occurrence of such nanostructures is well explained by the theoretical calculations. The results can be useful in investigation and development of spheres-assisted nano-patterning. © 2009 Springer-Verlag.

关键词： Light scattering

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Timescale of twin-peak quasi-periodic oscillations and mass of accreting neutron stars

arXiv

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arXiv 2019年

作者： Török, Gabriel Goluchová, Kateřina Šrámková, Eva Urbanec, Martin Straub, Odele Institute of Physics and Research Centre for Computational Physics and Data Processing Silesian University in Opava Bezručovo nám. 13 OpavaCZ-74601 Czech Republic Max Planck Institute for extraterrestrial Physics Gießenbachstraße 1 Garching85748 Germany

Einstein’s general relativity predicts that orbital motion of accreted gas approaching a neutron star (NS) in a NS low-mass X-ray binary (LMXB) system occurs on a time scale proportional to the NS mass. Radiation of the gas accounts for most of the observed LMXBs variability. In more than a dozen of sources twin-peak quasi-periodic oscillations (QPOs) have been observed. Inspired by the expected proportionality between periods of orbital motion and NS mass we present a straightforward comparison among these sources. We investigate relations between QPO periods and their ratios and identify characteristic time scales of QPOs associated to individual sources. These timescales are likely determined by the relative mass of each NS. We show that the characteristic time scale of the millisecond pulsar XTE J1807.4-294 is longer than for most other NS LMXBs. Consequently, models of QPOs that consider geodesic orbital frequencies imply that the X-ray pulsars’ mass has to be about 50% higher than the average mass of other sources. Consideration of other X-ray pulsars indicates that the exceptionality of XTE J1807.4-294 cannot be related to NS magnetic field in any simple manner. We suggest that QPOs observed in this source can help to discriminate between the proposed versions of the NS equation of state. Copyright © 2019, The Authors. All rights reserved.

关键词： Time measurement

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DeePMD-kit v3: A Multiple-Backend Framework for Machine Learning Potentials

arXiv

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arXiv 2025年

作者： Zeng, Jinzhe Zhang, Duo Peng, Anyang Zhang, Xiangyu He, Sensen Wang, Yan Liu, Xinzijian Bi, Hangrui Li, Yifan Cai, Chun Zhang, Chengqian Du, Yiming Zhu, Jia-Xin Mo, Pinghui Huang, Zhengtao Zeng, Qiyu Shi, Shaochen Qin, Xuejian Yu, Zhaoxi Luo, Chenxing Ding, Ye Liu, Yun-Pei Shi, Ruosong Wang, Zhenyu Bore, Sigbjørn Løland Chang, Junhan Deng, Zhe Ding, Zhaohan Han, Siyuan Jiang, Wanrun Ke, Guolin Liu, Zhaoqing Lu, Denghui Muraoka, Koki Oliaei, Hananeh Singh, Anurag Kumar Que, Haohui Xu, Weihong Xu, Zhangmancang Zhuang, Yong-Bin Dai, Jiayu Giese, Timothy J. Jia, Weile Xu, Ben York, Darrin M. Zhang, Linfeng Wang, Han School of Artificial Intelligence and Data Science Unversity of Science and Technology of China Hefei China AI for Science Institute Beijing100080 China DP Technology Beijing100080 China Academy for Advanced Interdisciplinary Studies Peking University Beijing100871 China State Key Lab of Processors Institute of Computing Technology Chinese Academy of Sciences Beijing100871 China University of Chinese Academy of Sciences Beijing China Baidu Inc. Beijing China Department of Computer Science University of Toronto TorontoON Canada Department of Chemistry Princeton University PrincetonNJ08540 United States University of Chinese Academy of Sciences Beijing100871 China State Key Laboratory of Physical Chemistry of Solid Surfaces iChEM College of Chemistry and Chemical Engineering Xiamen University Xiamen361005 China College of Integrated Circuits Hunan University Changsha410082 China State Key Laboratory of Advanced Technology for Materials Synthesis and Processing Center for Smart Materials and Device Integration School of Material Science and Engineering Wuhan University of Technology Wuhan430070 China College of Science National University of Defense Technology Changsha410073 China Hunan Key Laboratory of Extreme Matter and Applications National University of Defense Technology Changsha410073 China ByteDance Research Beijing100098 China Ningbo Institute of Materials Technology and Engineering Chinese Academy of Sciences Ningbo315201 China College of Materials Science and Opto-Electronic Technology University of Chinese Academy of Sciences Beijing100049 China Key Laboratory of Theoretical and Computational Photochemistry of Ministry of Education College of Chemistry Beijing Normal University Beijing100875 China Department of Geosciences Princeton University PrincetonNJ08544 United States Department of Applied Physics and Applied Mathematics Columbia University New YorkNY10027 United States IKKEM Fujian Xiamen361005 China Graduate

In recent years, machine learning potentials (MLPs) have become indispensable tools in physics, chemistry, and materials science, driving the development of software packages for molecular dynamics (MD) simulations and related applications. These packages, typically built on specific machine learning frameworks such as TensorFlow, PyTorch, or JAX, face integration challenges when advanced applications demand communication across different frameworks. The previous TensorFlow-based implementation of DeePMD-kit exemplified these limitations. In this work, we introduce DeePMD-kit version 3, a significant update featuring a multi-backend framework that supports TensorFlow, PyTorch, JAX, and PaddlePaddle backends, and demonstrate the versatility of this architecture through the integration of other MLPs packages and of Differentiable Molecular Force Field. This architecture allows seamless backend switching with minimal modifications, enabling users and developers to integrate DeePMD-kit with other packages using different machine learning frameworks. This innovation facilitates the development of more complex and interoperable workflows, paving the way for broader applications of MLPs in scientific research. Copyright © 2025, The Authors. All rights reserved.

关键词： Molecular dynamics

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ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -XXI. A Large-sample Observational Study of Ethanol and Dimethyl Ether in Hot Cores

arXiv

引用

arXiv 2025年

作者： Kou, Zhiping Li, Xiaohu Qin, Sheng-Li Liu, Tie Mannfors, E. Tang, Xindi Gorai, Prasanta Garay, Guido Das, Swagat R. García, Pablo Bronfman, Leonardo Juvela, M. Chen, Li Liu, Xunchuan Sanhueza, Patricio Peng, Yaping Chen, Long-Fei Zou, Jiahang Yang, Dongting Tóth, L. Viktor Dewangan, Lokesh Liu, Hong-Li Chibueze, James O. Li, Ziyang Xinjiang Astronomical Observatory Chinese Academy of Sciences 150 Science 1-Stree Urumqi Xinjiang830011 China University of Chinese Academy of Sciences Beijing100049 China School of Physics and Astronomy Yunnan University Kunming650091 China Xinjiang Key Laboratory of Radio Astrophysics 150 Science 1-Street Urumqi Xinjiang830011 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Physics University of Helsinki PO Box 64 Helsinki00014 Finland Rosseland Centre for Solar Physics University of Oslo PO Box 1029 Blindern Oslo0315 Norway Institute of Theoretical Astrophysics University of Oslo PO Box 1029 Blindern Oslo0315 Norway Departamento de Astronomía Universidad de Chile Las Condes Santiago7591245 Chile Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Department of Earth and Planetary Sciences Institute of Science Tokyo Meguro Tokyo152-8551 Japan National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Astronomical Science SOKENDAI The Graduate University for Advanced Studies 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Physics Faculty of Science Kunming University of Science and Technology Kunming650500 China School of Physics and Electronic Science Guizhou Normal University Guiyang550025 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guiyang550025 China Department of Astronomy Eötvös Loránd University Pázmány Péter sétány 1/A BudapestH-1117 Hungary University of Debrecen Faculty of Science and Technology Egyetemtér 1 DebrecenH-4032 Hungary Physical Research Laboratory Navrangpura Ahmedabad380 009 India Department of Mathematical Sciences University of South Africa Cnr Christian de Wet Rd and Pioneer Avenue Florida Park Roodepoort1709 South Africa Centre for Sp

Hot cores, as a stage of massive star formation, exhibit abundant line emissions of COMs. We present a deep line survey of two isomers of C2H6O: ethanol (C2H5OH;EA), and dimethyl ether (CH3OCH3;DE) as well as their possible precursor CH3OH towards 60 hot cores by using the ALMA 3 mm line observations. EA is detected in 40 hot cores and DE is detected in 59 hot cores. Of these, EA and DE are simultaneously detected in 39 hot cores. We calculate rotation temperatures and column densities of EA and DE by using the XCLASS software. The average rotation temperature of EA is higher than that of DE, whereas the average column density of EA is lower than that of DE. Combined with previous studies of hot cores and hot corinos, we find strong column density correlations among EA and DE (ρ = 0.92), EA and CH3OH (ρ = 0.82), as well as DE and CH3OH (ρ = 0.80). The column density ratios of EA/DE versus the column densities of CH3OH remain nearly constant with values within ~1 order of magnitude. These strong correlations and the stable ratios, suggest that EA, DE, and CH3OH could be chemically linked, with CH3OH potentially serving as a precursor for EA and DE. Compared with chemical models, the three different warm-up timescale models result in the systematic overproduction of EA and the systematic underproduction of DE. Therefore, our large sample observations can provide crucial constraints on chemical models. Copyright © 2025, The Authors. All rights reserved.

关键词： Giant stars

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Investigating photometric and spectroscopic variability in the multiply-imaged ‘Little Red Dot’ A2744-QSO1

arXiv

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arXiv 2025年

作者： Furtak, Lukas J. Secunda, Amy R. Greene, Jenny E. Zitrin, Adi Labbé, Ivo Golubchik, Miriam Bezanson, Rachel Kokorev, Vasily Atek, Hakim Brammer, Gabriel B. Chemerynska, Iryna Cutler, Sam E. Dayal, Pratika Feldmann, Robert Fujimoto, Seiji Leja, Joel Ma, Yilun Matthee, Jorryt Naidu, Rohan P. Nelson, Erica J. Oesch, Pascal A. Pan, Richard Price, Sedona H. Suess, Katherine A. Wang, Bingjie Weaver, John R. Whitaker, Katherine E. Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Physics & Astronomy and PITT PACC University of Pittsburgh PittsburghPA15260 United States Department of Astronomy The University of Texas at Austin AustinTX78712 United States Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Copenhagen Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen Denmark Department of Astronomy University of Massachusetts AmherstMA01003 United States Kapteyn Astronomical Institute University of Groningen PO Box 800 Groningen9700 AV Netherlands Department of Astrophysics Universität Zürich Winterthurerstrasse 190 ZurichCH-8044 Switzerland Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Am Campus 1 Klosterneuburg3400 Austria MIT Kavli Institute for Astrophysics and Space Research 70 Vassar Street CambridgeMA02139 United States Department for Astrophysical and Planetary Science University of Colorado BoulderCO80309 United States Département d’Astronomie Université de Genève Chemin Pegasi 51 Versoix1290 Switzerland Department of Physics and Astronomy Tufts University 574 Boston Ave. MedfordMA02155 United States

JWST observations have uncovered a new population of red, compact objects at high redshifts dubbed ‘Little Red Dots’ (LRDs), which typically show broad emission lines and are thought to be dusty Active Galactic Nuclei (AGN). Some of their other features, however, challenge the AGN explanation, such as prominent Balmer breaks and extremely faint or even missing metal high-ionization lines, X-ray, or radio emission, including in deep stacks. Time variability is a unique test of AGN activity. Here, we exploit the z = 7.045 multiply-imaged LRD A2744-QSO1, which offers a unique test of variability due to lensing-induced time delays between the three images spanning 22 yr (2.7 yr in the rest-frame), to investigate its photometric and spectroscopic variability. We find the equivalent widths (EWs) of the broad Hα and Hβ lines, which are independent of magnification and other systematics, to exhibit significant variations, up to 18 ± 3 % for Hα and up to 22 ± 8 % in Hβ, on a timescale of 875 d (2.4 yr) in the rest-frame. This suggests that A2744-QSO1 is indeed an AGN. We find no significant photometric variability beyond the limiting systematic uncertainties, so it currently cannot be determined whether the EW variations are due to line-flux or continuum variability. These results are consistent with a typical damped random walk (DRW) variability model for an AGN like A2744-QSO1 (MBH = 4 × 107 M☉) given the sparse sampling of the light-curve with the available data. Our results therefore support the AGN interpretation of this LRD, and highlight the need for further photometric and spectroscopic monitoring in order to build a detailed and reliable light-curve. Copyright © 2025, The Authors. All rights reserved.

关键词： Active Galactic Nuclei

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TOI-2005b: An Eccentric Warm Jupiter in Spin-Orbit Alignment

arXiv

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arXiv 2025年

作者： Bieryla, Allyson Dong, Jiayin Zhou, George Eastman, Jason D. Mayorga, L.C. Latham, David W. Carter, Brad Huang, Chelsea X. Quinn, Samuel N. Collins, Karen A. Abe, Lyu Beletsky, Yuri Brahm, Rafael Colón, Knicole D. Essack, Zahra Guillot, Tristan Henning, Thomas Hobson, Melissa J. Horne, Keith Jenkins, Jon M. Jones, Matías I. Jordán, Andrés Osip, David Ricker, George R. Rodriguez, Joseph E. Schulte, Jack Schwarz, Richard P. Seager, Sara Shporer, Avi Suarez, Olga Tan, Thiam-Guan Ting, Eric B. Triaud, Amaury Vanderburg, Andrew Villaseñor, Jesus Noel Vowell, Noah Watkins, Cristilyn N. Winn, Joshua N. Ziegler, Carl Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States University of Southern Queensland Centre for Astrophysics West Street ToowoombaQLD4350 Australia Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Department of Astronomy University of Illinois at Urbana-Champaign UrbanaIL61801 United States The Johns Hopkins University Applied Physics Laboratory 11100 Johns Hopkins Rd LaurelMD20723 United States Observatoire de la Côte d’Azur UniCA Laboratoire Lagrange CNRS UMR 7293 CS 34229 06304 Nice cedex 4 France Las Campanas Observatory Carnegie Institution for Science Colina El Pino Casilla La Serena601 Chile Facultad de Ingeniería y Ciencias Universidad Adolfo Ibáñez Av. Diagonal las Torres 2640 Santiago Peñalolén Chile Millennium Institute for Astrophysics Chile Data Observatory Foundation Chile GreenbeltMD20771 United States Department of Physics and Astronomy The University of New Mexico 210 Yale Blvd NE AlbuquerqueNM87106 United States Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany SUPA Physics and Astronomy University of St. Andrews Fife ScotlandKY16 9SS United Kingdom NASA Ames Research Center Moffett FieldCA94035 United States European Southern Observatory Alonso de Córdova 3107 Vitacura Casilla Santiago19001 Chile Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Center for Data Intensive and Time Domain Astronomy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Earth Atmospheric and Planetary Sciences Massachusetts Institute of Technology CambridgeMA02139 United States Department of Aeronautics and Astronautics MIT 77 Massachusetts Avenue CambridgeMA02139 United States Observatoire de la Côte d’Azur UniCA CNRS CS 34229 Nice06304 cedex 4

We report the discovery and characterization of TOI-2005 b, a warm Jupiter on an eccentric (e ∼ 0.59), 17.3-day orbit around a Vmag = 9.867 rapidly rotating F-star. The object was detected as a candidate by TESS and the planetary nature of TOI-2005 b was then confirmed via a series of ground-based photometric, spectroscopic, and diffraction-limited imaging observations. The planet was found to reside in a low sky-projected stellar obliquity orbit (λ =4.8+2−235 degrees) via a transit spectroscopic observation using the Magellan MIKE spectrograph. TOI-2005 b is one of a few planets known to have a low-obliquity, high-eccentricity orbit, which may be the result of high-eccentricity coplanar migration. The planet has a periastron equilibrium temperature of ∼ 2100 K, similar to some highly irradiated hot Jupiters where atomic metal species have been detected in transmission spectroscopy, and varies by almost 1000 K during its orbit. Future observations of the atmosphere of TOI-2005b can inform us about its radiative timescales thanks to the rapid heating and cooling of the planet. © 2025, CC BY.

关键词： Photometry

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Evolution of cooperation under a generalized death-birth process

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Physical Review E 2023年第2期107卷 024303-024303页

作者： Chaoqian Wang Attila Szolnoki Department of Computational and Data Sciences George Mason University Fairfax Virginia 22030 USA Institute of Technical Physics and Materials Science Centre for Energy Research P.O. Box 49 H-1525 Budapest Hungary

According to the evolutionary death-birth protocol, a player is chosen randomly to die and neighbors compete for the available position proportional to their fitness. Hence, the status of the focal player is completely ignored and has no impact on the strategy update. In this paper, we revisit and generalize this rule by introducing a weight factor to compare the payoff values of the focal and invading neighbors. By means of evolutionary graph theory, we analyze the model on joint transitive graphs to explore the possible consequences of the presence of a weight factor. We find that focal weight always hinders cooperation under weak selection strength. Surprisingly, the results show a nontrivial tipping point of the weight factor where the threshold of cooperation success shifts from positive to negative infinity. Once focal weight exceeds this tipping point, cooperation becomes unreachable. Our theoretical predictions are confirmed by Monte Carlo simulations on a square lattice of different sizes. We also verify the robustness of the conclusions to arbitrary two-player prisoner's dilemmas, to dispersal graphs with arbitrary edge weights, and to interaction and dispersal graphs overlapping arbitrarily.

关键词： Complex systems

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