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Euclid preparation LXIX. The impact of relativistic redshift-space distortions on two-point clustering statistics from the Euclid wide spectroscopic survey

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Astronomy and Astrophysics 2025年 697卷

作者： Elkhashab, M.Y. Bertacca, d. Porciani, C. Salvalaggio, J. Aghanim, N. Amara, A. Andreon, S. Auricchio, N. Baccigalupi, C. Baldi, M. Bardelli, S. Bodendorf, C. Bonino, d. Branchini, E. Brescia, M. Brinchmann, J. Camera, S. Capobianco, V. Carbone, C. Cardone, V.F. Carretero, J. Casas, r. Casas, S. Castellano, M. Castignani, G. Cavuoti, S. Cimatti, A. Colodro-Conde, C. Congedo, G. Conselice, C.J. Conversi, L. Copin, Y. Courbin, F. Courtois, H.M. da Silva, A. degaudenzi, H. di Giorgio, A.M. dinis, J. douspis, M. dubath, F. duncan, C.A.J. dupac, X. dusini, S. Farina, M. Farrens, S. Ferriol, S. Fosalba, P. Frailis, M. Franceschi, E. Galeotta, S. Gillis, B. Giocoli, C. Gómez-Alvarez, P. Grazian, A. Grupp, F. Guzzo, L. Haugan, S.V.H. Holmes, W. Hormuth, F. Hornstrup, A. Jahnke, K. Jhabvala, M. Joachimi, B. Keihänen, E. Kermiche, S. Kiessling, A. Kilbinger, M. Kitching, T. Kubik, B. Kuijken, K. Kümmel, M. Kunz, M. Kurki-Suonio, H. Ligori, S. Lilje, P.B. Lindholm, V. Lloro, I. Mainetti, G. Maiorano, E. Mansutti, O. Marggraf, O. Markovic, K. Martinet, N. Marulli, F. Massey, r. Medinaceli, E. Mei, S. Mellier, Y. Meneghetti, M. Meylan, G. Moresco, M. Moscardini, L. Niemi, S.-M. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Pettorino, V. Pires, S. Polenta, G. Poncet, M. Popa, L.A. Pozzetti, L. raison, F. rebolo, r. renzi, A. rhodes, J. riccio, G. romelli, E. roncarelli, M. Saglia, r. Sakr, Z. Sánchez, A.G. Sapone, d. Schirmer, M. Schneider, P. Schrabback, T. Scodeggio, M. Secroun, A. Sefusatti, E. Seidel, G. Serrano, S. Sirignano, C. Sirri, G. Stanco, L. Steinwagner, J. Surace, C. Tallada-Crespí, P. Taylor, A.N. Tereno, I. Toledo-Moreo, r. Torradeflot, F. Tutusaus, I. Valenziano, L. Vassallo, T. Verdoes Kleijn, G. Veropalumbo, A. Wang, Y. Weller, J. Zamorani, G. Zucca, E. Biviano, A. Boucaud, A. Bozzo, E. Burigana, C. Calabrese, M. di Ferdinando, d. Escartin Vigo, J.A. Farinelli, r. Finelli, F. Gracia-Carpio, J. Mauri, N. Pezzotta, A. Pöntinen, M. Scottez, V. Tenti, M. Viel, M. Wiesmann, M. Akrami, Y. Allevato, V. Anselmi, S INFN-Padova Via Marzolo 8 Padova 35131 Italy Dipartimento di Fisica e Astronomia “G. Galilei” Università di Padova Via Marzolo 8 Padova 35131 Italy INAF-Osservatorio Astronomico di Padova Via dell’Osservatorio 5 Padova 35122 Italy Universität Bonn Argelander-Institut für Astronomie Auf dem Hügel 71 Bonn 53121 Germany Dipartimento di Fisica – Sezione di Astronomia Università di Trieste Via Tiepolo 11 Trieste 34131 Italy INAF-Osservatorio Astronomico di Trieste Via G. B. Tiepolo 11 Trieste 34143 Italy IFPU Institute for Fundamental Physics of the Universe Via Beirut 2 Trieste 34151 Italy INFN Sezione di Trieste Via Valerio 2 TS Trieste 34127 Italy Université Paris-Saclay CNRS Institut d’astrophysique spatiale Orsay 91405 France School of Mathematics and Physics University of Surrey Guild-ford Surrey GU2 7XH United Kingdom INAF-Osservatorio Astronomico di Brera Via Brera 28 Milano 20122 Italy INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 Bologna 40129 Italy SISSA International School for Advanced Studies Via Bonomea 265 TS Trieste 34136 Italy Dipartimento di Fisica e Astronomia Università di Bologna Via Gobetti 93/2 Bologna 40129 Italy INFN-Sezione di Bologna Viale Berti Pichat 6/2 Bologna 40127 Italy Max Planck Institute for Extraterrestrial Physics Giessenbachstr. 1 Garching 85748 Germany INAF-Osservatorio Astrofisico di Torino Via Osservatorio 20 (TO) Pino Torinese 10025 Italy Dipartimento di Fisica Università di Genova Via Dodecaneso 33 Genova 16146 Italy INFN-Sezione di Genova Via Dodecaneso 33 Genova 16146 Italy Department of Physics “E. Pancini” University Federico II Via Cinthia 6 Napoli 80126 Italy INAF-Osservatorio Astronomico di Capodimonte Via Moiariello 16 Napoli 80131 Italy INFN section of Naples Via Cinthia 6 Napoli 80126 Italy Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas Porto PT4150-762 Portugal Diparti

Measurements of galaxy clustering are affected by redshift-space distortions (rSds). Peculiar velocities, gravitational lensing, and other light-cone projection effects modify the observed redshifts, fluxes, and sky positions of distant light sources. We determined which of these effects leave a detectable imprint on several two-point clustering statistics to be extracted from the Euclid wide spectroscopic survey (EWSS) on large scales. We generated 140 mock galaxy catalogues with the survey geometry and selection function of the EWSS and made use of the LIGEr (LIght cones with GEneral relativity) method to account for a variable number of relativistic rSds to linear order in the cosmological perturbations. We estimated different two-point clustering statistics from the mocks and used the likelihood-ratio test to calculate the statistical significance with which the EWSS could reject the null hypothesis that certain relativistic projection effects can be neglected in the theoretical models. We find that the combined effects of lensing magnification and convergence imprint characteristic signatures on several clustering observables. Their signal-to-noise ratio (S/N) ranges between 2.5 and 6 (depending on the adopted summary statistic) for the highest-redshift galaxies in the EWSS. The corresponding feature due to the peculiar velocity of the Sun is measured with a S/N of order one or two. The multipoles of the power spectrum from the catalogues that include all relativistic effects reject the null hypothesis that rSds are only generated by the variation in the peculiar velocity along the line of sight with a significance of 2.9 standard deviations. As a by-product of our study, we demonstrate that the mixing-matrix formalism to model finite-volume effects in the multipole moments of the power spectrum can be robustly applied to surveys made of several disconnected patches. Our results indicate that relativistic rSds, in particular the contribution from weak gravitati

关键词： galaxies: statistics large-scale structure of Universe methods: numerical

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divertor shaping with neutral baffling as a solution to the tokamak power exhaust challenge

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Communications Physics 2025年第1期8卷 1-15页

作者： Kevin Verhaegh James Harrison david Moulton Nicola Lonigro Nick Osborne Peter ryan Cyd Cowley Stuart Henderson Andrew Thornton Lingyan Xiang S. Aleiferis S. Allan J. Allcock L. Appel W. Arter I. Balboa O. Bardsley r. Bianchetti Morales A. Bleasdale A. Boboc C. Bowman d. Brunetti I. Carvalho F. J. Casson C. d. Challis B. Chapman N. J. Conway Y. damizia S. dowson S. Elmore F. Eriksson T. Farley A. r. Field N. Fil M. Fitzgerald M. Fontana r. Futtersack L. Garzotti S. N. Gerasimov Z. Ghani S. Gibson C. Giroud V. Gopakumar C. J. Ham J. Harrison N. C. Hawkes S. Henderson r. Henriques J. C. Hillesheim L. Horvath Z. Huang P. Jacquet I. Jepu d. Keeling H. T. Kim d. B. King V. G. Kiptily K. K. Kirov F. Köchl G. Kocsis L. Kogan d. Kos K. d. Lawson M. Lennholm E. LitherlandSmith P. J. Lomas C. Lowry C. F. Maggi J. Mailloux S. Marsden M. Maslov G. F. Matthews M. L. Mayoral G. McArdle A. G. Meigs S. Menmuir H. Meyer F. Militello J. Mitchell d. Moulton C. Olde H. J. C. Oliver N. Osborne r. Otin V. V. Parail A. Parrott A. Patel B. Patel M. Poradzinski F. G. rimini C. roach P. ryan d. ryan S. Saarelma S. Scully S. E. Sharapov r. Sharma A. Shaw S. A. Silburn J. Simpson S. Smith C. Srinivasan Z. Stancar C. I. Stuart H. J. Sun G. Szepesi d. Taylor E. Tholerus B. Thomas A. Thornton A. Tookey d. F. Valcarcel M. Valovic K. Verhaegh I. Voitsekhovitch d. Weston A. Widdowson T. Wilson L. Xiang Y. Zayachuk J. r. Harrison M. Aljunid S. Y. Allan L. C. Appel A. Ash J. Ashton O. Bachmann B. Barrett d. Beckett J. Bennett J. Buchanan N. Bulmer A. Carruthers J. Clark M. Coy G. Cunningham T. da Assuncao P. davies I. E. day S. dixon T. Eagles J. Edmond H. El-Haroun S. d. Elmore I. Fitzgerald S. Gee r. Harrison S. S. Henderson C. Hickling r. Hussain P. Jepson B. Kandan I. Katramados d. King r. King A. Kirk M. Kochan M. Lees G. Liddiard C. Man-Friel F. Mansfield r. Martin r. McAdams K. G. McClements d. McConville C. McKnight P. McKnight A. McShee J. Measures N. Mehay d. Morbey O. Myatra M. Nicassio E. Parr B. Parry B. S. Patel d. Payne M. Price r. Pr United Kingdom Atomic Energy Authority Culham UK Eindhoven University of Technology Eindhoven The Netherlands York Plasma Institute University of York York UK University of Liverpool Liverpool UK ITER Organization St-Paul-lez-Durance Cedex France Nat. Inst. for Laser Plasma & Radiation Physics Măgurele Romania EUROfusion PMU Garching Germany Dutch Institute for Fundamental Energy Research DIFFER Eindhoven The Netherlands Swiss Plasma Centre École Polytechnique Fédérale de Lausanne Lausanne Switzerland Oak Ridge National Laboratory Oak Ridge TN USA Universidad de Sevilla Seville Spain Electromagnetic Engineering & Fusion Science KTH Royal Institute of Technology Stockholm Sweden UniversitÃ degli Studi della Tuscia DEIM Viterbo Italy Aix-Marseille Univ. CNRS PIIM UMR 7345 Marseille France Politecnico di Milano Milan Italy Center for Energy Research UC San Diego La Jolla CA USA V. N. Karazin Kharkiv National University Kharkiv Ukraine Max Planck Institute for Plasma Physics Garching Germany Institute of Plasma Physics of the CAS Prague 8 Czechia Dublin City University Dublin Ireland VTT Technical Research Centre of Finland Espoo Finland Consorzio RFX Padova Italy University of California Irvine Irvine CA USA Istituto per la Scienza e la Tecnologia dei Plasmi CNR Padova Italy Graz University of Technology Graz Austria Aalto University Aalto Finland Institute for Plasma Science & Technology CNR Milan Italy Dept. of Applied Physics Ghent University Ghent Belgium ENEA Fusion & Nuclear Safety Dept. C.R. Frascati Frascati (RM) Italy National Technical University of Athens Zografou Greece Dept. of Physics & Astronomy Uppsala University Uppsala Sweden Dept. of Physics Durham University Durham UK Consorzio CREATE Naples Italy Aix-Marseille Univ. CNRS PIIM F-13397 Marseille France IRFM-CEA Centre de Cadarache St-Paul-lez-Durance France Centre for Energy Research Budapest Hungary University of Milano-Bicocca Milan Italy Dept. of Ele

Exhausting power from the hot fusion core to the plasma-facing components is one fusion energy’s biggest challenges. The MAST Upgrade tokamak uniquely integrates strong containment of neutrals within the exhaust area (divertor) with extreme divertor shaping capability. By systematically altering the divertor shape, this study shows the strongest evidence to date to our knowledge that long-legged divertors with a high magnetic field gradient (total flux expansion) deliver key power exhaust benefits without adversely impacting the hot fusion core. These benefits are already achieved with relatively modest geometry adjustments that are more feasible to integrate in reactor designs. Benefits include reduced target heat loads and improved access to, and stability of, a neutral gas buffer that ‘shields’ the target and enhances power exhaust (detachment). Analysis and model comparisons shows these benefits are obtained by combining multiple shaping aspects: long-legged divertors have expanded plasma-neutral interaction volume that drive reductions in particle and power loads, while total flux expansion enhances detachment access and stability. Containing the neutrals in the exhaust area with physical structures further augments these shaping benefits. These results demonstrate strategic variation in the divertor geometry and magnetic topology is a potential solution to one of fusion’s power exhaust challenge.

关键词： Fusion reactor divertors

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Scaling properties of flow harmonics of deuterons and protons in Au+Au reactions at 1.23 AGeV

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Journal of Physics: Conference Series 2020年第1期1667卷

作者： Paula Hillmann Jan Steinheimer Tom reichert Vincent Gaebel Marcus Bleicher Sukanya Sombun Christoph Herold Ayut Limphirat Institut für Theoretische Physik Goethe Universität Frankfurt Max-von-Laue-Str. 1 D-60438 Frankfurt am Main Germany Frankfurt Institute for Advanced Studies Ruth-Moufang-Str. 1 60438 Frankfurt am Main Germany GSI Helmholtzzentrum für Schwerionenforschung GmbH Planckstr. 1 64291 Darmstadt Germany John von Neumann-Institut für Computing Forschungszentrum Jülich 52425 Jülich Germany School of Physics and Center of Excellence in High Energy Physics & Astrophysics Suranaree University of Technology Nakhon Ratchasima 30000 Thailand

We explore the scaling properties of the elliptic and quadrangular flow of deuterons and protons in Au+Au reactions at a beam energy of 1.23 AGeV within the UrQMd approach. These investigations are of great interest for the HAdES experiment at GSI that has recently studied the flow of light nuclei. In the present studies, deuterons are formed via phase-space coalescence. Our results agree well with the experimental data, if for this low energy a hard equation of state is considered. We observe that protons and deuterons show direct scaling with the mass number A. We also see scaling of higher order flow harmonics, e.g. υ4 ~ .

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high-precision search for dark photon dark matter with the Parkes Pulsar Timing Array

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Physical review research 2022年第1期4卷 L012022-L012022页

作者： Xiao Xue Zi-Qing Xia Xingjiang Zhu Yue Zhao Jing Shu Qiang Yuan N. d. ramesh Bhat Andrew d. Cameron Shi dai Yi Feng Boris Goncharov George Hobbs Eric Howard richard N. Manchester Aditya Parthasarathy daniel J. reardon Christopher J. russell ryan M. Shannon renée Spiewak Nithyanandan Thyagarajan Jingbo Wang Lei Zhang Songbo Zhang II. Institut für Theoretische Physik Universität Hamburg Luruper Chaussee 149 D-22761 Hamburg Germany Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing 210023 China Advanced Institute of Natural Sciences Beijing Normal University at Zhuhai 519087 China School of Physics and Astronomy Monash University Clayton Victoria 3800 Australia OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery Hawthorn Victoria 3122 Australia Department of Physics and Astronomy University of Utah Salt Lake City Utah 84112 USA CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 China School of Physical Sciences University of Chinese Academy of Sciences Beijing 100049 China CAS Center for Excellence in Particle Physics Beijing 100049 China Center for High Energy Physics Peking University Beijing 100871 China School of Fundamental Physics and Mathematical Sciences Hangzhou Institute for Advanced Study University of Chinese Academy of Sciences Hangzhou 310024 China International Centre for Theoretical Physics Asia-Pacific Beijing/Hangzhou China School of Astronomy and Space Science University of Science and Technology of China Hefei 230026 China International Centre for Radio Astronomy Research Curtin University Bentley Western Australia 6102 Australia Australia Telescope National Facility CSIRO Astronomy and Space Science Epping New South Wales 1710 Australia Centre for Astrophysics and Supercomputing Swinburne University of Technology Hawthorn Victoria 3122 Australia School of Science Western Sydney University Locked Bag 1797 Penrith South DC NSW 2751 Australia Research Institute of Artificial Intelligence Zhejiang Lab Hangzhou Zhejiang 311121 China Macquarie University Department of Physics and Astronomy Sydney New South Wales 2109 Australia Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 D-53121 Bonn Germany CSIRO Sc

The nature of dark matter remains obscure in spite of decades of experimental efforts. The mass of dark matter candidates can span a wide range, and its coupling with the Standard Model sector remains uncertain. All these unknowns make the detection of dark matter extremely challenging. Ultralight dark matter, with m∼10−22 eV, is proposed to reconcile the disagreements between observations and predictions from simulations of small-scale structures in the cold dark matter paradigm while remaining consistent with other observations. Because of its large de Broglie wavelength and large local occupation number within galaxies, ultralight dark matter behaves like a coherently oscillating background field with an oscillating frequency dependent on its mass. If the dark matter particle is a spin-1 dark photon, such as the U(1)B or U(1)B−L gauge boson, it can induce an external oscillating force and lead to displacements of test masses. Such an effect would be observable in the form of periodic variations in the arrival times of radio pulses from highly stable millisecond pulsars. In this study, we search for evidence of ultralight dark photon dark matter (dPdM) using 14-year high-precision observations of 26 pulsars collected with the Parkes Pulsar Timing Array. While no statistically significant signal is found, we place constraints on coupling constants for the U(1)B and U(1)B−L dPdM. Compared with other experiments, the limits on the dimensionless coupling constant ε achieved in our study are improved by up to two orders of magnitude when the dark photon mass is smaller than 3×10−22 eV (10−22 eV) for the U(1)B (U(1)B−L) scenario.

关键词： dark matter radio, microwave, & sub-mm astronomy Hypothetical gauge bosons Neutron stars & pulsars Electromagnetic radiation astronomy

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INTrOdUCTION

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Bulletin of the American Meteorological Society 2024年第8期105卷 S1-S11页

作者： Boyer, T. Blunden, J. dunn, r.J.H. NOAA/NESDIS National Centers for Environmental Information Silver Spring Maryland NOAA/NESDIS National Centers for Environmental Information Asheville North Carolina Met Office Hadley Centre Exeter United Kingdom European Centre for Medium-Range Weather Forecasts Reading United Kingdom University of Maryland College Park Maryland Scripps Institution of Oceanography University of California San Diego La Jolla California NOAA/NWS National Centers for Environmental Prediction Climate Prediction Center College Park Maryland Brandenburg University of Technology (BTU) Cottbus-Senftenberg Germany Servicio Meteorológico Nacional Buenos Aires Argentina NOAA/OAR Physical Sciences Laboratory Boulder Colorado European Centre for Medium-Range Weather Forecasts Bonn Germany Center for Geophysical Research and School of Physics University of Costa Rica San José Costa Rica Department of Meteorology and National Centre for Earth Observation University of Reading Reading United Kingdom Centro Nacional de Monitoramento e Alertas de Desastres Naturais CEMADEN São Paulo Brazil Université Grenoble Alpes Institut des Géosciences de l’Environnement IRD CNRS Grenoble INP Grenoble France Hampton University Hampton Virginia Seychelles Meteorological Authority Mahe Seychelles Section for Glaciers Ice and Snow Norwegian Water Resources and Energy Directorate Oslo Norway National Research Institute for Agriculture Food and Environment (INRAE) CARRTEL Université Savoie Mont Blanc Thonon les Bains France Graduate School of Agriculture Osaka Metropolitan University Sakai Japan Science Faculty Universidad Nacional de Colombia Bogotá Colombia University of Bremen Bremen Germany NOAA Global Monitoring Laboratory Boulder Colorado Servicio Nacional de Meteorología e Hidrología del Perú Lima Perú Centro de Investigaciones sobre Desertificación – Spanish National Research Council (CSIC-UV-GVA) Valencia Spain Hydro-Climate Extremes Lab (H-CEL) Ghent University Ghent Belgium Department o

In 2023, La Niña conditions that generally prevailed in the eastern Pacific Ocean from mid-2020 into early 2023 gave way to a strong El Niño by October. Atmospheric concentrations of Earth’s major greenhouse gases—carbon dioxide, methane, and nitrous oxide—all increased to record-high levels. The annual global average carbon dioxide concentration in the atmosphere rose to 419.3±0.1 ppm, which is 50% greater than the pre-industrial level. The growth from 2022 to 2023 was 2.8 ppm, the fourth highest in the record since the 1960s. The combined short-term effects of El Niño and the long-term effects of increasing levels of heat-trapping gases in the atmosphere contributed to new records for many essential climate variables reported here. The annual global temperature across land and oceans was the highest in records dating as far back as 1850, with the last seven months (June–december) having each been record warm. Over land, the globally averaged temperature was also record high. dozens of countries reported record or near-record warmth for the year, including China and continental Europe as a whole (warmest on record), India and russia (second warmest), and Canada (third warmest). Intense and widespread heatwaves were reported around the world. In Vietnam, an all-time national maximum temperature record of 44.2°C was observed at Tuong duong on 7 May, surpassing the previous record of 43.4°C at Huong Khe on 20 April 2019. In Brazil, the air temperature reached 44.8°C in Araçuaí in Minas Gerais on 20 November, potentially a new national record and 12.8°C above normal. The effect of rising temperatures was apparent in the cryosphere, where snow cover extent by June 2023 was the smallest in the 56-year record for North America and seventh smallest for the Northern Hemisphere overall. Heatwaves contributed to the greatest average mass balance loss for Alpine glaciers around the world since the start of the record in 1970. due to rapid volume loss beginning in 2021, St. A

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Calculation of heavy meson light-cone distribution amplitudes from lattice QCd

arXiv

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arXiv 2024年

作者： Han, Xue-Ying Hua, Jun Ji, Xiangdong Lü, Cai-dian Schäfer, Andreas Su, Yushan Wang, Wei Xu, Ji Yang, Yibo Zhang, Jian-Hui Zhang, Qi-An Zhao, Shuai Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China School of Physical Sciences University of Chinese Academy of Sciences Beijing100049 China Guangdong Basic Research Center of Excellence for Structure and Fundamental Interactions of Matter Institute of Quantum Matter South China Normal University Guangzhou510006 China Guangdong-Hong Kong Joint Laboratory of Quantum Matter Guangdong Provincial Key Laboratory of Nuclear Science Southern Nuclear Science Computing Center South China Normal University Guangzhou510006 China Maryland Center for Fundamental Physics Department of Physics University of Maryland 4296 Stadium Dr. College ParkMD20742 United States Institut für Theoretische Physik University Regensburg RegensburgD-93040 Germany School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Institute of Modern Physics Chinese Academy of Sciences Guangdong Province Huizhou516000 China School of Nuclear Science and Technology Lanzhou University Lanzhou730000 China School of Physics and Microelectronics Zhengzhou University Henan Zhengzhou450001 China CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing100190 China School of Fundamental Physics and Mathematical Sciences Hangzhou Institute for Advanced Study UCAS Hangzhou310024 China International Centre for Theoretical Physics Asia-Pacific Hangzhou Beijing China School of Science and Engineering The Chinese University of Hong Kong Shenzhen518172 China School of Physics Beihang University Beijing102206 China School of Science Tianjin University Tianjin300072 China

We develop an approach for calculating heavy quark effective theory (HQET) light-cone distribution amplitudes (LCdAs) by employing a sequential effective theory methodology. The theoretical foundation of the framework is established, elucidating how the quasi distribution amplitudes (quasi dAs) with three scales can be utilized to compute HQET LCdAs. We provide theoretical support for this approach by demonstrating the rationale behind devising a hierarchical ordering for the three involved scales, discussing the factorization at each step, clarifying the underlying reason for obtaining HQET LCdAs in the final phase, and addressing potential theoretical challenges. The lattice QCd simulation aspect is explored in detail, and the computations of quasi dAs are presented. We employ three fitting strategies to handle contributions from excited states and extract the bare matrix elements. For renormalization purposes, we apply hybrid renormalization schemes at short and long distance separations. To mitigate long-distance perturbations, we perform an extrapolation in λ = z · Pz and assess the stability against various parameters. After two-step matching, our results for HQET LCdAs are found in agreement with existing model parametrizations. The potential phenomenological implications of the results are discussed, shedding light on how these findings could impact our understanding of the strong interaction dynamics and physics beyond the standard model. It should be noted, however, that systematic uncertainties have not been accounted for yet. © 2024, CC BY.

关键词： Bosons

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The MeerKAT Absorption Line Survey (MALS)

arXiv

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arXiv 2017年

作者： Gupta, N. Srianand, r. Baan, W. Baker, A. Beswick, r. Bhatnagar, S. Bhattacharya, d. Bosma, A. Carilli, C. Cluver, M. Combes, F. Cress, C. dutta, r. Fynbo, J. Heald, G. Hilton, M. Hussain, T. Jarvis, M. Jozsa, G. Kamphuis, P. Kembhavi, A. Kerp, J. Klöckner, H.-r. Krogager, J. Kulkarni, V. Ledoux, C. Mahabal, A. Mauch, T. Moodley, K. Momjian, E. Morganti, r. Noterdaeme, P. Oosterloo, T. Petitjean, P. Schröder, A. Serra, P. Sievers, J. Spekkens, K. Vaïsänen, P. Hulst, T. Van der Vivek, M. Wang, J. Wong, O.I. Zungu, A.r. Inter-University Centre for Astronomy and Astrophysics India The Netherlands Institute for Radio Astronomy Astron Netherlands The State University of New Jersey Rutgers United States University of 14 Mals N. Gupta Manchester United Kingdom National Radio Astronomy Observatory United States Laboratoire d'Astrophysique de Marseille France Physics and Astronomy Department University of Western Cape South Africa Observatoire de Paris France Centre for High Performance Computing South Africa Dark Cosmology Center Niels Bohr Institute Denmark Csiro Astronomy and Space Science Australia Astrophysics and Cosmology Research Unit University of KwaZulu Natal South Africa University of Oxford Astrophysics United Kingdom Square Kilometre Array South Africa South Africa National Centre for Radio Astrophysics India Universität Bonn Germany Max-Planck-Institut für Radioastronomie Germany Institut d'Astrophysique de Paris France Department of Physics and Astronomy University of South Carolina United States European Southern Observatory Chile Astronomy Department California Institute of Technology United States South African Astronomical Observatory South Africa INAF-Osservatorio Astronomico di Cagliari Italy Department of Physics Royal Military College of Canada Canada Kapteyn Astronomical Institute University of Groningen Netherlands University of Utah United States International Centre for Radio Astronomy Research University of Western Australia Australia

deep galaxy surveys have revealed that the global star formation rate (SFr) density in the Universe peaks at 1 z 2 and sharply declines towards z = 0. But a clear picture of the underlying processes, in particular the evolution of cold atomic (100 K) and molecular gas phases, that drive such a strong evolution is yet to emerge. MALS is designed to use MeerKAT's L- A nd UHF-band receivers to carry out the most sensitive (N(H I)>1019 cm2) dust-unbiased search of intervening H I 21-cm and OH 18-cm absorption lines at 0 1024WHz1) at 0 Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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The global spectrum of tree crown architecture

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Nature communications 2025年第1期16卷 4876页

作者： Tommaso Jucker Fabian Jörg Fischer Jérôme Chave david A Coomes John Caspersen Arshad Ali Grace Jopaul Loubota Panzou Ted r Feldpausch daniel Falster Vladimir A Usoltsev Toby d Jackson Stephen Adu-Bredu Luciana F Alves Mohammad Aminpour Bhely Angoboy Ilondea Niels P r Anten Cécile Antin Yousef Askari Narayanan Ayyappan Lindsay F Banin Nicolas Barbier John J Battles Hans Beeckman Yannick E Bocko Ben Bond-Lamberty Frans Bongers Samuel Bowers Michiel van Breugel Arthur Chantrain rajeev Chaudhary Jingyu dai Michele dalponte Kangbéni dimobe Jean-Christophe domec Jean-Louis doucet Juan Manuel dupuy rada remko A duursma Moisés Enríquez Karin Y van Ewijk William Farfán-rios Adeline Fayolle Marco Ferretti Eric Forni david I Forrester Hammad Gilani John L Godlee Matthias Haeni Jefferson S Hall Jie-Kun He Andreas Hemp José L Hernández-Stefanoni Steven I Higgins robert J Holdaway Kiramat Hussain Lindsay B Hutley Tomoaki Ichie Yoshiko Iida Hai-Sheng Jiang Puspa raj Joshi Hasan Kaboli Maryam Kazempour Larsary Tanaka Kenzo Brian d Kloeppel Takashi S Kohyama Suwash Kunwar Shem Kuyah Jakub Kvasnica Siliang Lin Emily r Lines Hongyan Liu Craig Lorimer Jean-Joël Loumeto Yadvinder Malhi Peter L Marshall Eskil Mattsson radim Matula Jorge A Meave Sylvanus Mensah Xiangcheng Mi Stéphane T Momo Glenn r Moncrieff Francisco Mora rodrigo Muñoz Sarath P Nissanka Zamah Shari Nur Hajar Kevin L O'Hara Steven Pearce raphaël Pelissier Pablo L Peri Pierre Ploton Lourens Poorter Mohsen Javanmiri Pour Hassan Pourbabaei Sabina C ribeiro Casey ryan Anvar Sanaei Jennifer Sanger Michael Schlund Giacomo Sellan Alexander Shenkin Bonaventure Sonké Frank J Sterck Martin Svátek Kentaro Takagi Anna T Trugman Matthew A Vadeboncoeur Ahmad Valipour Mark C Vanderwel Alejandra G Vovides Peter Waldner Weiwei Wang Li-Qiu Wang Christian Wirth Murray Woods Wenhua Xiang Fabiano de Aquino Ximenes Yaozhan Xu Toshihiro Yamada Miguel A Zavala Niklaus E Zimmermann School of Biological Sciences University of Bristol Bristol BS8 1TQ UK. t.jucker@bristol.ac.uk. School of Biological Sciences University of Bristol Bristol BS8 1TQ UK. UMR5300 Centre de Recherche sur la Biodiversité et l'Environnement CNRS INPT IRD Université de Toulouse Bât 4R1 118 route de Narbonne 31062 Toulouse France. Conservation Research Institute University of Cambridge Cambridge CB2 3EA UK. Institute of Forestry and Conservation University of Toronto 33 Willcocks Street Toronto ON M5S 3B3 Canada. Forest Ecology Research Group College of Life Sciences Hebei University Baoding 071002 Hebei China. Institut Supérieur des Sciences Géographiques Environnementales et de l'Aménagement (ISSGEA) Université DENIS SASSOU-N'GUESSO Kintélé République du Congo. Laboratoire de Biodiversité de Gestion des Ecosystèmes et de l'Environnement (LBGE) Faculté des Sciences et Techniques Université Marien NGOUABI BP 69 Brazzaville Brazzaville République du Congo. Faculty of Environment Science and Economy University of Exeter Exeter EX4 4QE UK. Evolution & Ecology Research Centre University of New South Wales Sydney NSW Sydney Australia. Department of Forest Mensuration and Management Ural State Forest Engineering and Economic University Yekaterinburg Russia. Forestry Research Institute of Ghana Council for Scientific and Industrial Research University Kumasi Ghana. Center for Tropical Research Institute of the Environment and Sustainability University of California Los Angeles Los Angeles CA USA. Natural Recourses and Watershed Management Office West Azerbaijan Province Urmia Iran. Institut National pour l'Etude et la Recherche Agronomiques BP 2037 Kinshasa Democratic Republic of the Congo. Université Pédagogique Nationale BP 8815 Kinshasa-Ngaliema Democratic Republic of the Congo. Center for Crop Systems Analysis Wageningen University & Research Wageningen Netherlands. AMAP lab Montpellier University IRD CIRAD CNRS INRAE Montpellier France. Rese

Trees can differ enormously in their crown architectural traits, such as the scaling relationships between tree height, crown width and stem diameter. Yet despite the importance of crown architecture in shaping the structure and function of terrestrial ecosystems, we lack a complete picture of what drives this incredible diversity in crown shapes. Using data from 374,888 globally distributed trees, we explore how climate, disturbance, competition, functional traits, and evolutionary history constrain the height and crown width scaling relationships of 1914 tree species. We find that variation in height-diameter scaling relationships is primarily controlled by water availability and light competition. Conversely, crown width is predominantly shaped by exposure to wind and fire, while also covarying with functional traits related to mechanical stability and photosynthesis. Additionally, we identify several plant lineages with highly distinctive stem and crown forms, such as the exceedingly slender dipterocarps of Southeast Asia, or the extremely wide crowns of legume trees in African savannas. Our study charts the global spectrum of tree crown architecture and pinpoints the processes that shape the 3d structure of woody ecosystems.

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26th Annual Computational Neuroscience Meeting (CNS*2017) of the Organization for Computational Neuroscience Antwerp, Belgium, July 15-20, 2017

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BMC NEUrOSCIENCE 2017年第SUPPL 1期18卷 59-59页

作者： [Anonymous] Indiana University Purdue University Indianapolis Indianapolis IN 46032 USA Stark Neurosciences Research Institute Indiana University School of Medicine Indianapolis IN 46032 USA Department of Mathematics East Carolina University Greenville NC 27858 USA Jülich Supercomputing Centre Forschungszentrum Jülich 52425 Jülich Germany Future Systems Swiss National Supercomputing Centre 8092 Zurich Switzerland User Engagement and Support Swiss National Supercomputing Centre 6900 Lugano Switzerland Institut de Neurosciences des Systèmes Aix Marseille Univ 13005 Marseille France Simulation Lab Neuroscience Forschungszentrum Jülich Jülich Germany Department of Experimental Psychology Ghent University 9000 Ghent Belgium Donders Center for Cognitive Neuroimaging Radboud University 6525HR Nijmegen The Netherlands Department of Electrical Computer and Energy Engineering University of Colorado Boulder CO 80309 USA Department of Neurosurgery Johns Hopkins School of Medicine Baltimore MD 21287 USA Department of Neurology Johns Hopkins School of Medicine Baltimore MD 21287 USA Department of Otolaryngology Johns Hopkins School of Medicine Baltimore MD 21287 USA INSERM U968 Paris France Sorbonne Universités UPMC University Paris 06 UMR_S 968 Institut de la Vision Paris France CNRS UMR_7210 Paris France Department of Computer Architecture and Technology University of Granada (CITIC) Granada Spain Sorbonne Universités UPMC Univ Paris 06 INSERM CNRS Institut de la Vision Paris France Department of Adaptive Machine Systems Osaka University Osaka Japan Department of Computer Science University of Cergy-Pontoise Cergy-Pontoise France Department of Physics and Astronomy College of Charleston Charleston SC 29424 USA School of Physics Faculty of Science University of Sydney Sydney NSW 2006 Australia Center of Excellence for Integrative Brain Function Australian Research Council Sydney Australia Max Planck Institute for Human Cognitive and Brain Sciences Saxony Lei

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Search for Gravitational Waves Emitted from SN 2023ixf

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The Astrophysical Journal 2025年第2期985卷 183-183页

作者： A. G. Abac r. Abbott I. Abouelfettouh F. Acernese K. Ackley S. Adhicary N. Adhikari r. X. Adhikari V. K. Adkins d. Agarwal M. Agathos M. Aghaei Abchouyeh O. d. Aguiar I. Aguilar L. Aiello A. Ain T. Akutsu S. Albanesi r. A. Alfaidi A. Al-Jodah C. Alléné A. Allocca S. Al-Shammari P. A. Altin S. Alvarez-Lopez A. Amato L. Amez-droz A. Amorosi C. Amra A. Ananyeva S. B. Anderson W. G. Anderson M. Andia M. Ando T. Andrade N. Andres M. Andrés-Carcasona T. Andrić J. Anglin S. Ansoldi J. M. Antelis S. Antier M. Aoumi E. Z. Appavuravther S. Appert S. K. Apple K. Arai A. Araya M. C. Araya J. S. Areeda L. Argianas N. Aritomi F. Armato N. Arnaud M. Arogeti S. M. Aronson G. Ashton Y. Aso M. Assiduo S. Assis de Souza Melo S. M. Aston P. Astone F. Attadio F. Aubin K. AultONeal G. Avallone S. Babak F. Badaracco C. Badger S. Bae S. Bagnasco E. Bagui J. G. Baier L. Baiotti r. Bajpai T. Baka M. Ball G. Ballardin S. W. Ballmer S. Banagiri B. Banerjee d. Bankar P. Baral J. C. Barayoga B. C. Barish d. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia d. Barta A. M. Bartoletti M. A. Barton I. Bartos S. Basak A. Basalaev r. Bassiri A. Basti d. E. Bates M. Bawaj P. Baxi J. C. Bayley A. C. Baylor P. A. Baynard II M. Bazzan V. M. Bedakihale F. Beirnaert M. Bejger d. Belardinelli A. S. Bell V. Benedetto W. Benoit J. d. Bentley M. Ben Yaala S. Bera M. Berbel F. Bergamin B. K. Berger S. Bernuzzi M. Beroiz d. Bersanetti A. Bertolini J. Betzwieser d. Beveridge N. Bevins r. Bhandare U. Bhardwaj r. Bhatt d. Bhattacharjee S. Bhaumik S. Bhowmick A. Bianchi I. A. Bilenko G. Billingsley A. Binetti S. Bini O. Birnholtz S. Biscoveanu A. Bisht M. Bitossi M.-A. Bizouard J. K. Blackburn L. A. Blagg C. d. Blair d. G. Blair F. Bobba N. Bode G. Boileau M. Boldrini G. N. Bolingbroke A. Bolliand L. d. Bonavena r. Bondarescu F. Bondu E. Bonilla M. S. Bonilla A. Bonino r. Bonnand P. Booker A. Borchers V. Boschi S. Bose V. Bossilkov V. Boudart A. Boudon A. Bozzi C. Bradaschia P. r. Brady M. Braglia A. Branch M. Branchesi J. Brandt I. Braun M. Breschi T. B Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-14476 Potsdam Germany LIGO Laboratory California Institute of Technology Pasadena CA 91125 USA LIGO Hanford Observatory Richland WA 99352 USA Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli I-80126 Napoli Italy University of Warwick Coventry CV4 7AL UK The Pennsylvania State University University Park PA 16802 USA University of Wisconsin-Milwaukee Milwaukee WI 53201 USA Louisiana State University Baton Rouge LA 70803 USA Université catholique de Louvain B-1348 Louvain-la-Neuve Belgium Inter-University Centre for Astronomy and Astrophysics Pune 411007 India Queen Mary University of London London E1 4NS UK Department of Physics and Astronomy Sejong University 209 Neungdong-ro Gwangjin-gu Seoul 143-747 Republic of Korea Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Stanford University Stanford CA 94305 USA Università di Roma Tor Vergata I-00133 Roma Italy INFN Sezione di Roma Tor Vergata I-00133 Roma Italy Cardiff University Cardiff CF24 3AA UK Universiteit Antwerpen 2000 Antwerpen Belgium Gravitational Wave Science Project National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino I-10125 Torino Italy Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany Dipartimento di Fisica Università degli Studi di Torino I-10125 Torino Italy SUPA University of Glasgow Glasgow G12 8QQ UK OzGrav University of Western Australia Crawley Western Australia 6009 Australia University Savoie Mont Blanc CNRS Laboratoire d’Annecy de Physique des Particules - IN2P3 F-74000 Annecy France Università di Napoli “Federico II ” I-80126 Napoli Italy OzGrav Australian National University C

We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19, during the LIGO–Virgo–KAGrA 15th Engineering run. We define a five-day on-source window during which an accompanying gravitational-wave signal may have occurred. No gravitational waves have been identified in data when at least two gravitational-wave observatories were operating, which covered ∼14% of this five-day window. We report the search detection efficiency for various possible gravitational-wave emission models. Considering the distance to M101 (6.7 Mpc), we derive constraints on the gravitational-wave emission mechanism of core-collapse supernovae across a broad frequency spectrum, ranging from 50 Hz to 2 kHz, where we assume the gravitational-wave emission occurred when coincident data are available in the on-source window. Considering an ellipsoid model for a rotating proto-neutron star, our search is sensitive to gravitational-wave energy 1 × 10⁻⁴ M_⊙c² and luminosity 2.6 × 10⁻⁴ M_⊙c² s⁻¹ for a source emitting at 82 Hz. These constraints are around an order of magnitude more stringent than those obtained so far with gravitational-wave data. The constraint on the ellipticity of the proto-neutron star that is formed is as low as 1.08, at frequencies above 1200 Hz, surpassing past results.

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