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Search for Continuous Gravitational Waves from Known Pulsars in the First Part of the Fourth LIGO-Virgo-KAGrA Observing run

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Astrophysical Journal 2025年第2期983卷 99-99页

作者： Abac, A.G. Abbott, r. Abouelfettouh, I. Acernese, F. Ackley, K. Adhicary, S. Adhikari, N. Adhikari, r.X. Adkins, V.K. Agarwal, d. Agathos, M. Aghaei Abchouyeh, M. Aguiar, O.d. Aguilar, I. Aiello, L. Ain, A. Ajith, P. Akutsu, T. Albanesi, S. Alfaidi, r.A. Al-Jodah, A. Alléné, C. Allocca, A. Al-Shammari, S. Altin, P.A. Alvarez-Lopez, S. Amato, A. Amez-droz, L. Amorosi, A. Amra, C. Ananyeva, A. Anderson, S.B. Anderson, W.G. Andia, M. Ando, M. Andrade, T. Andres, N. Andrés-Carcasona, M. Andrić, T. Anglin, J. Ansoldi, S. Antelis, J.M. Antier, S. Aoumi, M. Appavuravther, E.Z. Appert, S. Apple, S.K. Arai, K. Araya, A. Araya, M.C. Areeda, J.S. Argianas, L. Aritomi, N. Armato, F. Arnaud, N. Arogeti, M. Aronson, S.M. Ashton, G. Aso, Y. Assiduo, M. Assis de Souza Melo, S. Aston, S.M. Astone, P. Attadio, F. Aubin, F. AultONeal, K. Avallone, G. Babak, S. Badaracco, F. Badger, C. Bae, S. Bagnasco, S. Bagui, E. Baier, J.G. Baiotti, L. Bajpai, r. Baka, T. Ball, M. Ballardin, G. Ballmer, S.W. Banagiri, S. Banerjee, B. Bankar, d. Baral, P. Barayoga, J.C. Barish, B.C. Barker, d. Barneo, P. Barone, F. Barr, B. Barsotti, L. Barsuglia, M. Barta, d. Bartoletti, A.M. Barton, M.A. Bartos, I. Basak, S. Basalaev, A. Bassiri, r. Basti, A. Bates, d.E. Bawaj, M. Baxi, P. Bayley, J.C. Baylor, A.C. Baynard, P.A. Bazzan, M. Bedakihale, V.M. Beirnaert, F. Bejger, M. Belardinelli, d. Bell, A.S. Benedetto, V. Benoit, W. Bentley, J.d. Ben Yaala, M. Bera, S. Berbel, M. Bergamin, F. Berger, B.K. Bernuzzi, S. Beroiz, M. Bersanetti, d. Bertolini, A. Betzwieser, J. Beveridge, d. Bevins, N. Bhandare, r. Bhardwaj, U. Bhatt, r. Bhattacharjee, d. Bhaumik, S. Bhowmick, S. Bianchi, A. Bilenko, I.A. Billingsley, G. Binetti, A. Bini, S. Birnholtz, O. Biscoveanu, S. Bisht, A. Bitossi, M. Bizouard, M.-A. Blackburn, J.K. Blagg, L.A. Blair, C.d. Blair, d.G. Bobba, F. Bode, N. Boileau, G. Boldrini, M. Bolingbroke, G.N. Bolliand, A. Bonavena, L.d. Bondarescu, r. Bondu, F. Bonilla, E. Bonilla, M.S. Bonino, A. Bonnand, r. Booker, P. Borchers, A. Boschi, V. Bose, S. Boss Max Planck Institute for Gravitational Physics (Albert Einstein Institute) Potsdam D-14476 Germany LIGO Laboratory California Institute of Technology Pasadena 91125 CA United States LIGO Hanford Observatory Richland 99352 WA United States Dipartimento di Farmacia Università di Salerno Fisciano Salerno I-84084 Italy INFN Sezione di Napoli Napoli I-80126 Italy University of Warwick Coventry CV 47AL United Kingdom The Pennsylvania State University University Park 16802 PA United States University of Wisconsin-Milwaukee Milwaukee 53201 WI United States Louisiana State University Baton Rouge 70803 LA United States Université Catholique de Louvain Louvain-la-Neuve B-1348 Belgium Inter-University Centre for Astronomy and Astrophysics Pune 411007 India Queen Mary University of London London E1 4NS United Kingdom Department of Physics and Astronomy Sejong University 209 Neungdong-ro Gwangjin-gu Seoul 143-747 South Korea Instituto Nacional de Pesquisas Espaciais São José dos Campos São Paulo 12227-010 Brazil Stanford University Stanford 94305 CA United States Università di Roma Tor Vergata Roma I-00133 Italy INFN Sezione di Roma Tor Vergata Roma I-00133 Italy Cardiff University Cardiff CF24 3AA United Kingdom Universiteit Antwerpen Antwerpen 2000 Belgium International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India 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 Torino I-10125 Italy Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena Jena D-07743 Germany Dipartimento di Fisica Università degli Studi di Torino Torino I-10125 Italy SUPA University of Glasgow Glasgow G12 8QQ United Kingdom OzGrav University of Western Australia Crawley 6009 WA

Continuous gravitational waves (CWs) emission from neutron stars carries information about their internal structure and equation of state, and it can provide tests of general relativity. We present a search for CWs from a set of 45 known pulsars in the first part of the fourth LIGO-Virgo-KAGrA observing run, known as O4a. We conducted a targeted search for each pulsar using three independent analysis methods considering single-harmonic and dual-harmonic emission models. We find no evidence of a CW signal in O4a data for both models and set upper limits on the signal amplitude and on the ellipticity, which quantifies the asymmetry in the neutron star mass distribution. For the single-harmonic emission model, 29 targets have the upper limit on the amplitude below the theoretical spin-down limit. The lowest upper limit on the amplitude is 6.4 × 10^-27 for the young energetic pulsar J0537-6910, while the lowest constraint on the ellipticity is 8.8 × 10^-9 for the bright nearby millisecond pulsar J0437-4715. Additionally, for a subset of 16 targets, we performed a narrowband search that is more robust regarding the emission model, with no evidence of a signal. We also found no evidence of nonstandard polarizations as predicted by the Brans-dicke theory. © 2025. The Author(s). Published by the American Astronomical Society.

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Quark masses using twisted-mass fermion gauge ensembles

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Physical review d 2021年第7期104卷 074515-074515页

作者： C. Alexandrou S. Bacchio G. Bergner M. Constantinou M. di Carlo P. dimopoulos J. Finkenrath E. Fiorenza r. Frezzotti M. Garofalo K. Hadjiyiannakou B. Kostrzewa G. Koutsou K. Jansen V. Lubicz M. Mangin-Brinet F. Manigrasso G. Martinelli E. Papadiofantous F. Pittler G. C. rossi F. Sanfilippo S. Simula C. Tarantino A. Todaro C. Urbach U. Wenger Department of Physics University of Cyprus 20537 Nicosia Cyprus Computation-based Science and Technology Research Center The Cyprus Institute 20 Konstantinou Kavafi Street 2121 Nicosia Cyprus University of Jena Institute for Theoretical Physics Max-Wien-Platz 1 D-07743 Jena Germany Department of Physics Temple University Philadelphia Pennsylvania 19122–1801 USA School of Physics and Astronomy The University of Edinburgh Edinburgh EH9 3FD United Kingdom Istituto Nazionale di Fisica Nucleare Sezione di Roma La Sapienza Piazzale Aldo Moro 5 I-00185 Roma Italy Dipartimento di Scienze Matematiche Fisiche e Informatiche Università di Parma and INFN Gruppo Collegato di Parma Parco Area delle Scienze 7/a (Campus) 43124 Parma Italy CP3-Origins University of Southern Denmark Campusvej 55 5230 Odense Denmark Dipartimento di Fisica and INFN Università di Roma “Tor Vergata” Via della Ricerca Scientifica 1 I-00133 Roma Italy HISKP (Theory) Rheinische Friedrich-Wilhelms-Universität Bonn Nussallee 14-16 53115 Bonn Germany High Performance Computing and Analytics Lab Rheinische Friedrich-Wilhelms-Universität Bonn Friedrich-Hirzebruch-Allee 8 53115 Bonn Germany NIC DESY Platanenallee 6 D-15738 Zeuthen Germany Dipartimento di Matematica e Fisica Università Roma Tre and INFN Sezione di Roma Tre Via della Vasca Navale 84 I-00146 Rome Italy Theory Group Laboratoire de Physique Subatomique et de Cosmologie CNRS/IN2P3 38026 Grenoble France Institut für Physik Humboldt-Universität zu Berlin Newtonstrasse 15 12489 Berlin Germany Dipartimento di Fisica and INFN Università di Roma “La Sapienza” Piazzale Aldo Moro 5 I-00185 Roma Italy Centro Fermi Museo Storico della Fisica e Centro Studi e Ricerche “Enrico Fermi” Piazza del Viminale 1 I-00184 Roma Italy Istituto Nazionale di Fisica Nucleare Sezione di Roma Tre Via della Vasca Navale 84 I-00146 Rome Italy Institute for Theoretical Physics Albert Einstein Center for Fundamental Physics University of Bern Sidlerstrasse

We present a calculation of the up, down, strange, and charm quark masses performed within the lattice QCd framework. We use the twisted-mass fermion action and carry out simulations that include in the sea two light mass-degenerate quarks, as well as the strange and charm quarks. In the analysis, we use gauge ensembles simulated at three values of the lattice spacing and with light quarks that correspond to pion masses in the range from 350 MeV to the physical value, while the strange and charm quark masses are tuned approximately to their physical values. We use several quantities to set the scale in order to check for finite lattice spacing effects, and in the continuum limit, we get compatible results. The quark mass renormalization is carried out nonperturbatively using the (modified) regularization Independent Momentum Subtraction (rI′−MOM) method converted into the MS¯ scheme. For the determination of the quark masses, we use physical observables from both the meson and the baryon sectors, obtaining mud=3.636(66)( −57+60) MeV and ms=98.7(2.4)( −3.2+4.0) MeV in the MS¯(2 GeV) scheme and mc=1036(17)( −8+15) MeV in the MS¯(3 GeV) scheme, where the first errors are statistical and the second ones are combinations of systematic errors. For the quark mass ratios, we get ms/mud=27.17(32)( −38+56) and mc/ms=11.48(12)( −19+25).

关键词： Lattice field theory Quarks Mass Lattice QCd

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The AGOrA high-resolution Galaxy Simulations Comparison Project. V: Satellite Galaxy Populations In A Cosmological Zoom-in Simulation of A Milky Way-mass Halo

arXiv

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arXiv 2024年

作者： Jung, Minyong roca-Fàbrega, Santi Kim, Ji-Hoon Genina, Anna Hausammann, Loic Hyeonyong, K.I.M. Lupi, Alessandro Nagamine, Kentaro Powell, Johnny W. revaz, Yves Shimizu, Ikkoh Velázquez, Héctor Ceverino, daniel Primack, Joel r. Quinn, Thomas r. Strawn, Clayton Abel, Tom dekel, Avishai dong, Bili Oh, Boon Kiat Teyssier, romain Center for Theoretical Physics Department of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of Lund Observatory Department of Astronomy and Theoretical Physics Lund University Box 43 LundSE-221 00 Sweden Departamento de Física de la Tierra y Astrofísica Facultad de Ciencias Físicas Plaza Ciencias 1 Madrid28040 Spain Seoul National University Astronomy Research Center Seoul08826 Korea Republic of Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany ITS High Performance Computing Eidgenössische Technische Hochschule Zürich Zürich8092 Switzerland Institute of Physics Laboratoire d’Astrophysique École Polytechnique Fédérale de Lausanne LausanneCH-1015 Switzerland Department of Aerospace Engineering Seoul National University Seoul08826 Korea Republic of DiSAT Università degli Studi dell’Insubria via Valleggio 11 ComoI-22100 Italy Dipartimento di Fisica "G. Occhialini" Università degli Studi di Milano-Bicocca MilanoI-20126 Italy Department of Earth and Space Science Graduate School of Science Osaka University Osaka Toyonaka560-0043 Japan University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8583 Japan Department of Physics & Astronomy University of Nevada Las Vegas Las VegasNV89154 United States Department of Physics Reed College PortlandOR97202 United States Shikoku Gakuin University 3-2-1 Bunkyocho Zentsuji Kagawa765-8505 Japan Instituto de Astronomía Universidad Nacional Autónoma de México A.P. 70-264 D.F. Mexico04510 Mexico Universidad Autónoma de Madrid Ciudad Universitaria de Cantoblanco MadridE-28049 Spain CIAFF Facultad de Ciencias Universidad Autónoma de Madrid MadridE-28049 Spain Department of Physics University of California at Santa Cruz Santa CruzCA95064 United States Department of Astronomy University of Washington SeattleWA98195 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305 Unite

We analyze and compare the satellite halo populations at z ∼ 2 in the high-resolution cosmological zoom-in simulations of a 1012 M☉ target halo (z = 0 mass) carried out on eight widely-used astrophysical simulation codes (ArT-I, ENZO, rAMSES, CHANGA, GAdGET-3, GEAr, ArEPO-T, and GIZMO) for the AGOrA high-resolution Galaxy Simulations Comparison Project. We use slightly different redshift epochs near z = 2 for each code (hereafter "z ∼ 2’) at which the eight simulations are in the same stage in the target halo’s merger history. After identifying the matched pairs of halos between the Cosmorun simulations and the dMO simulations, we discover that each Cosmorun halo tends to be less massive than its dMO counterpart. When we consider only the halos containing stellar particles at z ∼ 2, the number of satellite galaxies is significantly fewer than that of dark matter halos in all participating AGOrA simulations, and is comparable to the number of present-day satellites near the Milky Way or M31. The so-called "missing satellite problem’ is fully resolved across all participating codes simply by implementing the common baryonic physics adopted in AGOrA and the stellar feedback prescription commonly used in each code, with sufficient numerical resolution ( 100 proper pc at z = 2). We also compare other properties such as the stellar mass−halo mass relation and the mass−metallicity relation. Our work highlights the value of comparison studies such as AGOrA, where outstanding problems in galaxy formation theory are studied simultaneously on multiple numerical platforms. © 2024, CC BY.

关键词： Satellites

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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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Quark masses using twisted mass fermion gauge ensembles

arXiv

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arXiv 2021年

作者： Alexandrou, C. Bacchio, S. Bergner, G. Constantinou, M. di Carlo, M. dimopoulos, P. Finkenrath, J. Fiorenza, E. Frezzotti, r. Garofalo, M. Hadjiyiannakou, K. Kostrzewa, B. Koutsou, G. Jansen, K. Lubicz, V. Mangin-Brinet, M. Manigrasso, F. Martinelli, G. Papadiofantous, E. Pittler, F. rossi, G.C. Sanfilippo, F. Simula, Silvano Tarantino, C. Todaro, A. Urbach, C. Wenger, U. Department of Physics University of Cyprus Nicosia20537 Cyprus Computation-based Science and Technology Research Center The Cyprus Institute 20 Konstantinou Kavafi Street Nicosia2121 Cyprus University of Jena Institute for Theoretical Physics Max-Wien-Platz 1 JenaD-07743 Germany Department of Physics Temple University PhiladelphiaPA19122 - 1801 United States School of Physics and Astronomy The University of Edinburgh EdinburghEH9 3FD United Kingdom Istituto Nazionale di Fisica Nucleare Sezione di Roma La Sapienza Piazzale Aldo Moro 5 RomaI-00185 Italy Parma43124 Italy CP3-Origins University of Southern Denmark Campusvej 55 Odense5230 Denmark Dipartimento di Fisica INFN Università di Roma Tor Vergata Via della Ricerca Scientifica 1 RomaI-00133 Italy Rheinische Friedrich-Wilhelms-Universität Bonn Nussallee 14-16 Bonn53115 Germany High Performance Computing and Analytics Lab Rheinische Friedrich-Wilhelms-Universität Bonn Friedrich-Hirzebruch-Allee 8 Bonn53115 Germany NIC DESY Platanenallee 6 ZeuthenD-15738 Germany Dipartimento di Matematica e Fisica Università Roma Tre INFN Sezione di Roma Tre Via della Vasca Navale 84 RomeI-00146 Italy Theory Group Laboratoire de Physique Subatomique et de Cosmologie CNRS IN2P3 Grenoble38026 France Institut für Physik Humboldt-Universität zu Berlin Newtonstrasse 15 Berlin12489 Germany Dipartimento di Fisica INFN Università di Roma La Sapienza Piazzale Aldo Moro 5 RomaI-00185 Italy Centro Fermi Museo Storico della Fisica Centro Studi e Ricerche Enrico Fermi Piazza del Viminale 1 RomaI-00184 Italy Istituto Nazionale di Fisica Nucleare Sezione di Roma Tre Via della Vasca Navale 84 RomeI-00146 Italy Institute for Theoretical Physics Albert Einstein Center for Fundamental Physics University of Bern Sidlerstrasse 5 BernCH-3012 Switzerland

We present a calculation of the up, down, strange and charm quark masses performed within the lattice QCd framework. We use the twisted mass fermion action and carry out simulations that include in the sea two light mass-degenerate quarks, as well as the strange and charm quarks. In the analysis we use gauge ensembles simulated at three values of the lattice spacing and with light quarks that correspond to pion masses in the range from 350 MeV to the physical value, while the strange and charm quark masses are tuned approximately to their physical values. We use several quantities to set the scale in order to check for finite lattice spacing effects and in the continuum limit we get compatible results. The quark mass renormalization is carried out nonperturbatively using the rI'-MOM method converted into the MS scheme. For the determination of the quark masses we use physical observables from both the meson and the baryon sectors, obtaining mud = 3.636(66)(+60−57) MeV and ms = 98.7(2.4)(+4.0−3.2) MeV in the MS(2 GeV) scheme and mc = 1036(17)(+15−8 ) MeV in the MS(3 GeV) scheme, where the first errors are statistical and the second ones are combinations of systematic errors. For the quark mass ratios we get ms/mud = 27.17(32)(+56−38) and mc/ms = 11.48(12)(+25−19). Copyright © 2021, The Authors. All rights reserved.

关键词： Hadrons

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A persistent excess of galaxy-galaxy strong lensing observed in galaxy clusters

arXiv

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arXiv 2023年

作者： Meneghetti, Massimo Cui, Weiguang rasia, Elena Yepes, Gustavo Acebron, Ana Angora, Giuseppe Bergamini, Pietro Borgani, Stefano Calura, Francesco despali, Giulia Giocoli, Carlo Granata, Giovanni Grillo, Claudio Knebe, Alexander Macciò, Andrea V. Mercurio, Amata Moscardini, Lauro Natarajan, Priyamvada ragagnin, Antonio rosati, Piero Vanzella, Eros INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 BolognaI-40129 Italy INFN-Sezione di Bologna Viale Berti Pichat 6/2 BolognaI-40127 Italy Departamento de Física Teórica Facultad de Ciencias Universidad Autónoma de Madrid Módulo 8 MadridE-28049 Spain Facultad de Ciencias Universidad Autónoma de Madrid MadridE-28049 Spain Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom INAF – Osservatorio Astronomico di Trieste via Tiepolo 11 TriesteI-34131 Italy IFPU Institute for Fundamental Physics of the Universe via Beirut 2 Trieste34151 Italy INFN Istituto Nazionale di Fisica Nucleare Via Valerio 2 TriesteI-34127 Italy Dipartimento di Fisica Università degli Studi di Milano Via Celoria 16 MilanoI-20133 Italy Dipartimento di Fisica e Scienze della Terra Università degli Studi di Ferrara Via Saragat 1 FerraraI-44122 Italy INAF-Osservatorio Astronomico di Capodimonte Via Moiariello 16 Napoli80131 Italy Astronomy Unit Department of Physics University of Trieste via Tiepolo 11 TriesteI-34131 Italy Dipartimento di Fisica e Astronomia "Augusto Righi" Alma Mater Studiorum Università di Bologna via Gobetti 93/2 BolognaI-40129 Italy INAF - IASF Milano via A. Corti 12 MilanoI-20133 Italy International Centre for Radio Astronomy Research University of Western Australia 35 Stirling Highway CrawleyWA6009 Australia New York University Abu Dhabi PO Box Abu Dhabi129188 United Arab Emirates New York University Abu Dhabi United Arab Emirates Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany FiscianoI–84084 Italy Department of Astronomy Yale University New HavenCT06511 United States Department of Physics Yale University New HavenCT06520 United States ICSC - Italian Research Center on High Performance Computing Big Data and Quantum Computing Italy

Context. Previous studies have revealed that the estimated probability of galaxy-galaxy strong lensing in observed galaxy clusters exceeds the expectations from the Λ Cold dark Matter cosmological model by one order of magnitude. Aims. We aim to understand the origin of this excess by analyzing a larger set of simulated galaxy clusters, and investigating how the theoretical expectations vary under different adopted prescriptions and numerical implementations of star formation and feedback in simulations. Methods. We performed a ray-tracing analysis of 324 galaxy clusters from the Three Hundred project, comparing the Gadget-X and Gizmo-Simba runs. These simulations, which start from the same initial conditions, were performed with different implementations of hydrodynamics and galaxy formation models tailored to match different observational properties of the intracluster medium and cluster galaxies. results. We find that galaxies in the Gizmo-Simba simulations develop denser stellar cores than their Gadget-X counterparts. Consequently, their probability for galaxy-galaxy strong lensing is higher by a factor of ∼ 3. This increment is still insufficient to fill the gap with observations as a discrepancy by a factor ∼ 4 still persists. In addition, we find that several simulated galaxies have Einstein radii that are too large compared to observations. Conclusions. We conclude that a persistent excess of galaxy-galaxy strong lensing exists in observed galaxy clusters. The origin of this discrepancy with theoretical predictions is still unexplained in the framework of the cosmological hydrodynamical simulations. This might signal a hitherto unknown issue with either the simulation methods or our assumptions regarding the standard cosmological model. Copyright © 2023, The Authors. All rights reserved.

关键词： Galaxies

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Insight-HXMT and GECAM-C observations of the brightest-of-all-time GrB 221009A

arXiv

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arXiv 2023年

作者： An, Zheng-Hua Antier, S. Bi, Xing-Zi Bu, Qing-Cui Cai, Ce Cao, Xue-Lei Camisasca, Anna-Elisa Chang, Zhi Chen, Gang Chen, Li Chen, Tian-Xiang Chen, Wen Chen, Yi-Bao Chen, Yong Chen, Yu-Peng Coughlin, Michael W. Cui, Wei-Wei dai, Zi-Gao Hussenot-desenonges, T. du, Yan-Qi du, Yuan-Yuan du, Yun-Fei Fan, Cheng-Cheng Frontera, Filippo Gao, He Gao, Min Ge, Ming-Yu Gong, Ke Gu, Yu-dong Guan, Ju Guo, dong-Ya Guo, Zhi-Wei Guidorzi, Cristiano Han, da-Wei He, Jian-Jian He, Jun-Wang Hou, dong-Jie Huang, Yue Huo, Jia Ji, Zhen Jia, Shu-Mei Jiang, Wei-Chun Kann, david Alexander Klotz, A. Kong, Ling-da Lan, Lin Li, An Li, Bing Li, Chao-Yang Li, Cheng-Kui Li, Gang Li, Mao-Shun Li, Ti-Pei Li, Wei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Yan-Guo Li, Zheng-Wei Liang, Jing Liang, Xiao-Hua Liao, Jin-Yuan Lin, Lin Liu, Cong-Zhan Liu, He-Xin Liu, Hong-Wei Liu, Jia-Cong Liu, Xiao-Jing Liu, Ya-Qing Liu, Yu-rong Lu, Fang-Jun Lu, Hong Lu, Xue-Feng Luo, Qi Luo, Tao Ma, Bin-Yuan Ma, Fu-Li Ma, rui-Can Ma, Xiang Maccary, romain Mao, Ji-rong Meng, Bin Nie, Jian-Yin Orlandini, Mauro Ou, Ge Peng, Jing-Qiang Peng, Wen-Xi Qiao, rui Qu, Jin-Lu ren, Xiao-Qin Shi, Jing-Yan Shi, Qi Song, Li-Ming Song, Xin-Ying Su, Ju Sun, Gong-Xing Sun, Liang Sun, Xi-Lei Tan, Wen-Jun Tan, Ying Tao, Lian Tuo, You-Li Turpin, damien Wang, Jin-Zhou Wang, Chen Wang, Chen-Wei Wang, Hong-Jun Wang, Hui Wang, Jin Wang, Ling-Jun Wang, Peng-Ju Wang, Ping Wang, Wen-Shuai Wang, Xiang-Yu Wang, Xi-Lu Wang, Yu-Sa Wang, Yue Wen, Xiang-Yang Wu, Bo-Bing Wu, Bai-Yang Wu, Hong Xiao, Sheng-Hui Xiao, Shuo Xiao, Yun-Xiang Xie, Sheng-Lun Xiong, Shao-Lin Xiong, Sen-Lin Xu, dong Xu, He Xu, Yan-Jun Xu, Yan-Bing Xu, Ying-Chen Xu, Yu-Peng Xue, Wang-Chen Yang, Sheng Yang, Yan-Ji Yang, Zi-Xu Ye, Wen-Tao Yi, Qi-Bin Yi, Shu-Xu Yin, Qian-Qing You, Yuan Yu, Yun-Wei Yu, Wei Yu, Wen-Hui Zeng, Ming Zhang, Bing Zhang, Bin-Bin Zhang, da-Li Zhang, Fan Zhang, Hong-Mei Zhang, Juan Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China Institut für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Eberhard Karls Universität Sand 1 Tübingen72076 Germany College of Physics Hebei Key Laboratory of Photophysics Research and Application Hebei Normal University Hebei Shijiazhuang050024 China Department of Physics and Earth Science University of Ferrara Via Saragat 1 Ferrara44122 Italy Department of Astronomy Beijing Normal University Beijing100875 China CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China Department of Astronomy Tsinghua University Beijing100084 China Southwest Jiaotong University Chengdu610092 China INAF Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 101 Bologna40129 Italy University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100049 China College of physics Sciences Technology Hebei University No. 180 Wusi Dong Road Lian Chi District Hebei Baoding071002 China INFN - Sezione di Ferrara Via Saragat 1 Ferrara44122 Italy Physics and Space Science College China West Normal University China Yunnan Observatories Chinese Academy of Sciences Yunnan Province Kunming650011 China Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science Nanjing University Nanjing210093 China School of Physics and Optoelectronics Xiangtan University Yuhu District Hunan Xiangtan411105 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China Institute of Astrophysics Central China Normal University Wuhan430079 China Nevada Center for Astrophysics Department of Physics and Astronomy University of

GrB 221009A is the brightest gamma-ray burst ever detected since the discovery of this kind of energetic explosions. However, an accurate measurement of the prompt emission properties of this burst is very challenging due to its exceptional brightness. With joint observations of Insight-HXMT and GECAM-C, we made an unprecedentedly accurate measurement of the emission during the first ∼1800 s of GrB 221009A, including its precursor, main emission (ME, which dominates the burst in flux), flaring emission and early afterglow, in the hard X-ray to soft gamma-ray band from ∼ 10 keV to ∼ 6 MeV. Based on the GECAM-C unsaturated data of the ME, we measure a record-breaking isotropic equivalent energy (Eiso) of ∼ 1.5 × 1055 erg, which is about eight times the total rest-mass energy of the Sun. The early afterglow data require a significant jet break between 650 s and 1100 s, most likely at ∼ 950 s from the afterglow starting time TAG, which corresponds to a jet opening angle of ∼ 0.7◦ (ηγn)1/8, where n is the ambient medium density in units of cm−3 and ηγ is the ratio between γ-ray energy and afterglow kinetic energy. The beaming-corrected total γ-ray energy Eγ is ∼ 1.15 × 1051 (ηγn)1/4 erg, which is typical for long GrBs. These results suggest that this GrB may have a special central engine, which could launch and collimate a very narrowly beamed jet with an ordinary energy budget, leading to exceptionally luminous gamma-ray radiation per unit solid angle. Alternatively, more GrBs might have such a narrow and bright beam, which are missed by an unfavorable viewing angle or have been detected without distance measurement. Copyright © 2023, The Authors. All rights reserved.

关键词： Gamma rays

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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Sup1期18卷 1-79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 Bra

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Search for heavy resonances decaying to a Z boson and a photon in pp collisions at s=13 TeV with the ATLAS detector

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Physics Letters, Section B: Nuclear, Elementary Particle and high-Energy Physics 2017年 764卷 11-30页

作者： Aaboud, M. Aad, G. Abbott, B. Abdallah, J. Abdinov, O. Abeloos, B. Aben, r. AbouZeid, O.S. Abraham, N.L. Abramowicz, H. Abreu, H. Abreu, r. Abulaiti, Y. Acharya, B.S. Adachi, S. Adamczyk, L. Adams, d.L. Adelman, J. Adomeit, S. Adye, T. Affolder, A.A. Agatonovic-Jovin, T. Agricola, J. Aguilar-Saavedra, J.A. Ahlen, S.P. Ahmadov, F. Aielli, G. Akerstedt, H. Åkesson, T.P.A. Akimov, A.V. Alberghi, G.L. Albert, J. Albrand, S. Alconada Verzini, M.J. Aleksa, M. Aleksandrov, I.N. Alexa, C. Alexander, G. Alexopoulos, T. Alhroob, M. Ali, B. Aliev, M. Alimonti, G. Alison, J. Alkire, S.P. Allbrooke, B.M.M. Allen, B.W. Allport, P.P. Aloisio, A. Alonso, A. Alonso, F. Alpigiani, C. Alshehri, A.A. Alstaty, M. Alvarez Gonzalez, B. Álvarez Piqueras, d. Alviggi, M.G. Amadio, B.T. Amako, K. Amaral Coutinho, Y. Amelung, C. Amidei, d. Amor dos Santos, S.P. Amorim, A. Amoroso, S. Amundsen, G. Anastopoulos, C. Ancu, L.S. Andari, N. Andeen, T. Anders, C.F. Anders, G. Anders, J.K. Anderson, K.J. Andreazza, A. Andrei, V. Angelidakis, S. Angelozzi, I. Anger, P. Angerami, A. Anghinolfi, F. Anisenkov, A.V. Anjos, N. Annovi, A. Antel, C. Antonelli, M. Antonov, A. Anulli, F. Aoki, M. Aperio Bella, L. Arabidze, G. Arai, Y. Araque, J.P. Arce, A.T.H. Arduh, F.A. Arguin, J-F. Argyropoulos, S. Arik, M. Armbruster, A.J. Armitage, L.J. Arnaez, O. Arnold, H. Arratia, M. Arslan, O. Artamonov, A. Artoni, G. Artz, S. Asai, S. Asbah, N. Ashkenazi, A. Åsman, B. Asquith, L. Assamagan, K. Astalos, r. Atkinson, M. Atlay, N.B. Augsten, K. Avolio, G. Axen, B. Ayoub, M.K. Azuelos, G. Baak, M.A. Baas, A.E. Baca, M.J. Bachacou, H. Bachas, K. Backes, M. Backhaus, M. Bagiacchi, P. Bagnaia, P. Bai, Y. Baines, J.T. Baker, O.K. Baldin, E.M. Balek, P. Balestri, T. Balli, F. Balunas, W.K. Banas, E. Banerjee, Sw. Bannoura, A.A.E. Barak, L. Barberio, E.L. Barberis, d. Barbero, M. Barillari, T. Barisits, M-S Barklow, T. Barlow, N. Barnes, S.L. Barnett, B.M. Barnett, r.M. Barnovska-Blenessy, Z. Baroncelli, A. Barone, G. Barr, A.J. Barranco Navarro, L. Barreiro, F. Barreiro Gui Department of Physics University of Adelaide Adelaide Australia Physics Department SUNY Albany Albany NY United States Department of Physics University of Alberta Edmonton AB Canada Department of Physics Ankara University Ankara Turkey Istanbul Aydin University Istanbul Turkey Division of Physics TOBB University of Economics and Technology Ankara Turkey LAPP CNRS/IN2P3 Université Savoie Mont Blanc Annecy-le-Vieux France High Energy Physics Division Argonne National Laboratory Argonne IL United States Department of Physics University of Arizona Tucson AZ United States Department of Physics The University of Texas at Arlington Arlington TX United States Physics Department University of Athens Athens Greece Physics Department National Technical University of Athens Zografou Greece Department of Physics The University of Texas at Austin Austin TX United States Institute of Physics Azerbaijan Academy of Sciences Baku Azerbaijan Institut de Física d'Altes Energies (IFAE) The Barcelona Institute of Science and Technology Barcelona Spain Institute of Physics University of Belgrade Belgrade Serbia Department for Physics and Technology University of Bergen Bergen Norway Physics Division Lawrence Berkeley National Laboratory University of California Berkeley CA United States Department of Physics Humboldt University Berlin Germany Albert Einstein Center for Fundamental Physics Laboratory for High Energy Physics University of Bern Bern Switzerland School of Physics and Astronomy University of Birmingham Birmingham United Kingdom Department of Physics Bogazici University Istanbul Turkey Department of Physics Engineering Gaziantep University Gaziantep Turkey Istanbul Bilgi University Faculty of Engineering and Natural Sciences Istanbul Turkey Bahcesehir University Faculty of Engineering and Natural Sciences Istanbul Turkey Centro de Investigaciones Universidad Antonio Narino Bogota Colombia INFN Sezione di Bologna Italy Dipartimento di Fis

This Letter presents a search for new resonances with mass larger than 250 GeV, decaying to a Z boson and a photon. The dataset consists of an integrated luminosity of 3.2 fb−1 of pp collisions collected at s=13 TeV w... 详细信息

This Letter presents a search for new resonances with mass larger than 250 GeV, decaying to a Z boson and a photon. The dataset consists of an integrated luminosity of 3.2 fb⁻¹ of pp collisions collected at s=13 TeV with the ATLAS detector at the Large Hadron Collider. The Z bosons are identified through their decays either to charged, light, lepton pairs (e⁺e⁻, μ⁺μ⁻) or to hadrons. The data are found to be consistent with the expected background in the whole mass range investigated and upper limits are set on the production cross section times decay branching ratio to Zγ of a narrow scalar boson with mass between 250 GeV and 2.75 TeV. © 2016 The Author(s)

关键词： Z bosons CrOSS sections (Nuclear physics) PHOTON-photon interactions LArGE Hadron Collider (France & Switzerland) dILEPTON production NUCLEAr counters

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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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