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A Robust Test of the Existence of Primordial Black Holes in Galactic Dark Matter Halos

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arXiv 2022年

作者： Abramowicz, Marek Bejger, Michal Udalski, Andrzej Wielgus, MacIek Research Center for Computational Physics and Data Processing Institute of Physics Silesian University Opava Czech Republic Nicolaus Copernicus Astronomical Centre Polish Academy of Sciences Bartycka 18 Warsaw00-716 Poland Department of Physics Göteborg University GöteborgSE-412-96 Sweden Infn Sezione di Ferrara Via Saragat 1 Ferrara44122 Italy Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany

If very low mass primordial black holes (PBH) within the asteroid/moon-mass range indeed reside in galactic dark matter halos, they must necessarily collide with galactic neutron stars (NSs). These collisions must, again necessarily, form light black holes (LBHs) with masses of typical NSs, MLBH≈ 1 - 2 Mo. LBHs may be behind events already detected by ground-based gravitational-wave detectors (GW170817, GW190425, and others such as a mixed stellar black hole-neutron star mass event GW191219-163120), and most recently by microlensing (OGLE-BLG-2011-0462). Although the status of these observations as containing LBHs is not confirmed, there is no question that gravitationalwave detectors and microlensing are in principle and in practice capable of detecting LBHs. We have calculated the creation rate of LBHs resulting from these light primordial black hole collisions with neutron stars. On this basis, we claim that if improved gravitational-wave detectors and microlensing statistics of the LBH events would indicate that the number of LBHs is significantly lower that what follows from the calculated creation rate, then this would be an unambiguous proof that there is no significant light PBH contribution to the galactic dark matter halos. Otherwise, if observed and calculated numbers of LBHs roughly agree, then the hypothesis of primordial black hole existence gets strong observational support, and in addition their collisions with neutron stars may be considered a natural creation channel for the LBHs, solving the problem of their origin, as it is known that they cannot be a product of standard stellar evolution. © 2022, CC BY.

关键词： Gravity waves

Numerical Simulation of Hot Accretion Flow around Bondi Radius

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arXiv 2022年

作者： Mosallanezhad, Amin Bu, De-Fu Čemeljić, Miljenko Zeraatgari, Fatemeh Zahra Hai, Yang Mei, Liquan School of Mathematics and Statistics Xi'an Jiaotong University Shaanxi Xi’an710049 China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Bartycka 18 Warsaw00-716 Poland Academia Sinica Institute of Astronomy and Astrophysics P.O. Box 23-141 Taipei106 Taiwan Research Centre for Computational Physics and Data Processing Institute of Physics Silesian University in Opava Bezručovo nám. 13 OpavaCZ-74601 Czech Republic

Previous numerical simulations have shown that strong winds can be produced in the hot accretion flows around black holes. Most of those studies focus only on the region close to the central black hole, therefore it is unclear whether the wind production stops at large radii around Bondi radius. Bu et al. 2016 studied the hot accretion flow around the Bondi radius in the presence of nuclear star gravity. They find that when the nuclear stars gravity is important/comparable to the black hole gravity, winds can not be produced around the Bondi radius. However, for some galaxies, the nuclear stars gravity around Bondi radius may not be strong. In this case, whether winds can be produced around Bondi radius is not clear. We study the hot accretion flow around Bondi radius with and without thermal conduction by performing hydrodynamical simulations. We use the virtual particles trajectory method to study whether winds exist based on the simulation data. Our numerical results show that in the absence of nuclear stars gravity, winds can be produced around Bondi radius, which causes the mass inflow rate decreasing inwards. We confirm the results of Yuan et al. which indicates this is due to the mass loss of gas via wind rather convectional motions. © 2022, CC BY.

关键词： Wind

ABACUS: An Electronic Structure Analysis Package for the AI Era

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arXiv 2025年

作者： Zhou, Weiqing Zheng, Daye Liu, Qianrui Lu, Denghui Liu, Yu Lin, Peize Huang, Yike Peng, Xingliang Bao, Jie J. Cai, Chun Jin, Zuxin Wu, Jing Zhang, Haochong Jin, Gan Ji, Yuyang Shen, Zhenxiong Liu, Xiaohui Sun, Liang Cao, Yu Sun, Menglin Liu, Jianchuan Chen, Tao Liu, Renxi Li, Yuanbo Han, Haozhi Liang, Xinyuan Bao, Taoni Chen, Nuo Ren, Hongxu Zhang, Xiaoyang Liu, Zhaoqing Fu, Yiwei Liu, Maochang Li, Zhuoyuan Wen, Tongqi Tang, Zechen Xu, Yong Duan, Wenhui Wang, Xiaoyang Gu, Qiangqiang Dai, Fu-Zhi Zheng, Qijing Zhao, Jin Zhang, Yuzhi Ou, Qi Jiang, Hong Liu, Shi Xu, Ben Xu, Shenzhen Ren, Xinguo He, Lixin Zhang, Linfeng Chen, Mohan AI for Science Institute Beijing100080 China HEDPS CAPT School of Physics College of Engineering Peking University Beijing100871 China College of Engineering Peking University Beijing100871 China Institute of Artificial Intelligence Hefei Comprehensive National Science Center Hefei230026 China Key Laboratory of Quantum Information University of Science and Technology of China Hefei230026 China Supercomputing Center University of Science and Technology of China Anhui Hefei230026 China Institute of Physics Chinese Academy of Sciences Beijing100190 China School of Materials Science and Engineering Peking University Beijing100871 China School of Electrical Engineering and Electronic Information Xihua University Chengdu610039 China Academy for Advanced Interdisciplinary Studies Peking University Beijing100871 China College of Chemistry and Molecular Engineering Peking University Beijing100871 China International Research Center for Renewable Energy State Key Laboratory of Multiphase Flow Xi’an Jiaotong University Shaanxi Xi’an710049 China Suzhou Academy of Xi’an Jiaotong University Jiangsu Suzhou215123 China Center for Structural Materials Department of Mechanical Engineering The University of Hong Kong Hong Kong The University of Hong Kong Shenzhen China State Key Laboratory of Low Dimensional Quantum Physics Department of Physics Tsinghua University Beijing100084 China Frontier Science Center for Quantum Information Beijing China Saitama Wako351-0198 Japan Institute for Advanced Study Tsinghua University Beijing100084 China Laboratory of Computational Physics Institute of Applied Physics and Computational Mathematics Fenghao East Road 2 Beijing100094 China School of Artificial Intelligence and Data Science University of Science and Technology of China Hefei230026 China School of Materials Science and Engineering University of Science and Technology Beijing Beijing100083 China Department of Physics University of Science and

ABACUS (Atomic-orbital Based Ab-initio Computation at USTC) is an open-source software for first-principles electronic structure calculations and molecular dynamics simulations. It mainly features density functional theory (DFT) and is compatible with both plane-wave basis sets and numerical atomic orbital basis sets. ABACUS serves as a platform that facilitates the integration of various electronic structure methods, such as Kohn-Sham DFT, stochastic DFT, orbital-free DFT, and real-time time-dependent DFT, etc. In addition, with the aid of high-performance computing, ABACUS is designed to perform efficiently and provide massive amounts of first-principles data for generating general-purpose machine learning potentials, such as DPA models. Furthermore, ABACUS serves as an electronic structure platform that interfaces with several AI-assisted algorithms and packages, such as DeePKS-kit, DeePMD, DP-GEN, DeepH, DeePTB, etc. Copyright © 2025, The Authors. All rights reserved.

关键词： Stochastic systems

Evolutionary dynamics of any multiplayer game on regular graphs

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arXiv 2024年

作者： Wang, Chaoqian Perc, Matjaž Szolnoki, Attila Department of Computational and Data Sciences George Mason University FairfaxVA22030 United States Faculty of Natural Sciences and Mathematics University of Maribor Koroška cesta 160 Maribor2000 Slovenia Community Healthcare Center Dr. Adolf Drolc Maribor Vošnjakova ulica 2 Maribor2000 Slovenia Complexity Science Hub Vienna Josefstädterstraße 39 Vienna1080 Austria Department of Physics Kyung Hee University 26 Kyungheedae-ro Dongdaemun-gu Seoul Korea Republic of Institute of Technical Physics and Materials Science Centre for Energy Research P.O. Box 49 BudapestH-1525 Hungary

Multiplayer games on graphs are at the heart of theoretical descriptions of key evolutionary processes that govern vital social and natural systems. However, a comprehensive theoretical framework for solving multiplayer games with an arbitrary number of strategies on graphs is still missing. Here, we solve this by drawing an analogy with the Balls-and-Boxes problem, based on which we show that the local configuration of multiplayer games on graphs is equivalent to distributing k identical co-players among n distinct strategies. We use this to derive the replicator equation for any n-strategy multiplayer game under weak selection, which can be solved in polynomial time. As an example, we revisit the second-order free-riding problem, where costly punishment cannot truly resolve social dilemmas in a well-mixed population. Yet, in structured populations, we derive an accurate threshold for the punishment strength, beyond which punishment can either lead to the extinction of defection or transform the system into a rock-paper-scissors-like cycle. The analytical solution also qualitatively agrees with the phase diagrams that were previously obtained for non-marginal selection strengths. Our framework thus allows an exploration of any multi-strategy multiplayer game on regular graphs. © 2024, CC BY.

关键词： Graphic methods

Measurement of the 2νββ Decay Rate and Spectral Shape of Mo100 from the CUPID-Mo Experiment

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Physical Review Letters 2023年第16期131卷 162501-162501页

作者： C. Augier A. S. Barabash F. Bellini G. Benato M. Beretta L. Bergé J. Billard Yu. A. Borovlev L. Cardani N. Casali A. Cazes E. Celi M. Chapellier D. Chiesa I. Dafinei F. A. Danevich M. De Jesus T. Dixon L. Dumoulin K. Eitel F. Ferri B. K. Fujikawa J. Gascon L. Gironi A. Giuliani V. D. Grigorieva M. Gros D. L. Helis H. Z. Huang R. Huang L. Imbert J. Johnston A. Juillard H. Khalife M. Kleifges V. V. Kobychev Yu. G. Kolomensky S. I. Konovalov J. Kotila P. Loaiza L. Ma E. P. Makarov P. de Marcillac R. Mariam L. Marini S. Marnieros X.-F. Navick C. Nones E. B. Norman E. Olivieri J. L. Ouellet L. Pagnanini L. Pattavina B. Paul M. Pavan H. Peng G. Pessina S. Pirro D. V. Poda O. G. Polischuk S. Pozzi E. Previtali Th. Redon A. Rojas S. Rozov V. Sanglard J. A. Scarpaci B. Schmidt Y. Shen V. N. Shlegel F. Šimkovic V. Singh C. Tomei V. I. Tretyak V. I. Umatov L. Vagneron M. Velázquez B. Ware B. Welliver L. Winslow M. Xue E. Yakushev M. Zarytskyy A. S. Zolotarova Univ Lyon Université Lyon 1 CNRS/IN2P3 IP2I-Lyon F-69622 Villeurbanne France National Research Centre “Kurchatov Institute ” Kurchatov Complex of Theoretical and Experimental Physics 117218 Moscow Russia Dipartimento di Fisica Sapienza Università di Roma Piazzale Aldo Moro 2 I-00185 Rome Italy INFN Sezione di Roma P.le Aldo Moro 2 I-00185 Rome Italy INFN Laboratori Nazionali del Gran Sasso I-67100 Assergi (AQ) Italy INFN Gran Sasso Science Institute I-67100 L’Aquila Italy University of California Berkeley California 94720 USA Université Paris-Saclay CNRS/IN2P3 IJCLab 91405 Orsay France Nikolaev Institute of Inorganic Chemistry 630090 Novosibirsk Russia Dipartimento di Fisica Università di Milano-Bicocca I-20126 Milano Italy INFN Sezione di Milano-Bicocca I-20126 Milano Italy Institute for Nuclear Research of NASU 03028 Kyiv Ukraine INFN Sezione di Roma Tor Vergata Via della Ricerca Scientifica 1 I-00133 Rome Italy IRFU CEA Université Paris-Saclay F-91191 Gif-sur-Yvette France Karlsruhe Institute of Technology Institute for Astroparticle Physics 76021 Karlsruhe Germany Lawrence Berkeley National Laboratory Berkeley California 94720 USA Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) Fudan University Shanghai 200433 People’s Republic of China Massachusetts Institute of Technology Cambridge Massachusetts 02139 USA Karlsruhe Institute of Technology Institute for Data Processing and Electronics 76021 Karlsruhe Germany National Research Centre Kurchatov Institute Institute of Theoretical and Experimental Physics 117218 Moscow Russia Department of Physics University of Jyväskylä P.O. Box 35 FI-40014 Jyväskylä Finland Finnish Institute for Educational Research University of Jyväskylä P.O. Box 35 FI-40014 Jyvaäskylä Finland Center for Theoretical Physics Sloane Physics Laboratory Yale University New Haven Connecticut 06520-8120 USA Physik Department Technische Universität München Garching D-85748 Germany Department of Modern P

Neutrinoless double beta decay (0νββ) is a yet unobserved nuclear process that would demonstrate Lepton number violation, a clear evidence of beyond standard model physics. The process two neutrino double beta decay (2νββ) is allowed by the standard model and has been measured in numerous experiments. In this Letter, we report a measurement of 2νββ decay half-life of Mo100 to the ground state of Ru100 of [7.07±0.02(stat)±0.11(syst)]×1018 yr by the CUPID-Mo experiment. With a relative precision of ±1.6% this is the most precise measurement to date of a 2νββ decay rate in Mo100. In addition, we constrain higher-order corrections to the spectral shape, which provides complementary nuclear structure information. We report a novel measurement of the shape factor ξ3,1=0.45±0.03(stat)±0.05(syst) based on a constraint on the ratio of higher-order terms from theory, which can be reliably calculated. This is compared to theoretical predictions for different nuclear models. We also extract the first value for the effective axial vector coupling constant obtained from a spectral shape study of 2νββ decay.

关键词： Double beta decay Neutrinoless double beta decay Nuclear structure & decays

Model-independent searches of new physics in DARWIN with a semi-supervised deep learning pipeline

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arXiv 2024年

作者： Aalbers, J. Abe, K. Adrover, M. Ahmed Maouloud, S. Althueser, L. Amaral, D.W.P. Andrieu, B. Angelino, E. Antón Martin, D. Antunovic, B. Aprile, E. Babicz, M. Bajpai, D. Balzer, M. Barberio, E. Baudis, L. Bazyk, M. Bell, N.F. Bellagamba, L. Biondi, R. Biondi, Y. Bismark, A. Boehm, C. Boese, K. Braun, R. Breskin, A. Brommer, S. Brown, A. Bruni, G. Budnik, R. Cai, C. Capelli, C. Chauvin, A. Cimental Chavez, A.P. Colijn, A.P. Conrad, J. Cuenca-García, J.J. D'Andrea, V. Daniel Garcia, L.C. Decowski, M.P. Deisting, A. Di Donato, C. Di Gangi, P. Diglio, S. Doerenkamp, M. Drexlin, G. Eitel, K. Elykov, A. Engel, R. Ferella, A.D. Ferrari, C. Fischer, H. Flehmke, T. Flierman, M. Fujikawa, K. Fulgione, W. Fuselli, C. Gaemers, P. Gaior, R. Galloway, M. Gao, F. Garroum, N. Giacomobono, R. Girard, F. Glade-Beucke, R. Glück, F. Grandi, L. Grigat, J. Größle, R. Guan, H. Guida, M. Gyorgy, P. Hammann, R. Hannen, V. Hansmann-Menzemer, S. Hargittai, N. Higuera, A. Hils, C. Hiraoka, K. Hoetzsch, L. Hoferichter, M. Hood, N.F. Iacovacci, M. Itow, Y. Jakob, J. James, R.S. Joerg, F. Kahlert, F. Kaminaga, Y. Kara, M. Kavrigin, P. Kazama, S. Keller, M. Kharbanda, P. Kilminster, B. Kleifges, M. Klute, M. Kobayashi, M. Koke, D. Kopec, A. von Krosigk, B. Kuger, F. LaCascio, L. Landsman, H. Lang, R.F. Levinson, L. Li, I. Li, A. Li, S. Liang, S. Liang, Z. Lin, Y.-T. Lindemann, S. Lindner, M. Liu, K. Loizeau, J. Lombardi, F. Long, J. Lopes, J.A.M. Lucchetti, G.M. Luce, T. Ma, Y. Macolino, C. Mahlstedt, J. Maier, B. Mancuso, A. Manenti, L. Marignetti, F. Martens, K. Masbou, J. Masson, E. Mastroianni, S. Melchiorre, A. Menéndez, J. Messina, M. Milosovic, B. Milutinovic, S. Miuchi, K. Miyata, R. Molinario, A. Monteiro, C.M.B. Morå, K. Moriyama, S. Morteau, E. Mosbacher, Y. Müller, J. Murra, M. Newstead, J.L. Ni, K. O'Hare, C. Oberlack, U. Obradovic, M. Ostrowskiy, I. Ouahada, S. Paetsch, B. Pan, Y. Pandurovic, M. Pellegrini, Q. Nikhef The University of Groningen Van Swinderen Institute Groningen9747AG Netherlands University of Tokyo Higashi-Mozumi Kamioka Gifu Hida506-1205 Japan Physik-Institut University of Zürich Zürich8057 Switzerland LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France Institute for Nuclear Physics University of Münster Münster48149 Germany Department of Physics and Astronomy Rice University HoustonTX77005 United States INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy INFN-Laboratori Nazionali del Gran Sasso Gran Sasso Science Institute L'Aquila67100 Italy Department of Physics Enrico Fermi Institute Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Physics Department Columbia University New YorkNY10027 United States Department of Physics & Astronomy University of Alabama TuscaloosaAL34587-0324 United States Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany ARC Centre of Excellence for Dark Matter Particle Physics School of Physics The University of Melbourne VIC3010 Australia SUBATECH IMT Atlantique CNRS IN2P3 Nantes Université Nantes44307 France Department of Physics and Astronomy University of Bologna INFN-Bologna Bologna40126 Italy Max-Planck-Institut für Kernphysik Heidelberg69117 Germany Institute for Astroparticle Physics Karlsruhe Institute of Technology Karlsruhe76021 Germany School of Physics The University of Sydney Camperdown SydneyNSW2006 Australia Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot7610001 Israel Institute of Experimental Particle Physics Karlsruhe Institute of Technology Karlsruhe76021 Germany Physikalisches Institut Universität Freiburg Freiburg79104 Germany Department of Physics and

We present a novel deep learning pipeline to perform a model-independent, likelihood-free search for anomalous (i.e., non-background) events in the proposed next generation multi-ton scale liquid Xenon-based direct detection experiment, DARWIN. We train an anomaly detector comprising a variational autoencoder and a classifier on extensive, high-dimensional simulated detector response data and construct a one-dimensional anomaly score optimised to reject the background only hypothesis in the presence of an excess of non-background-like events. We benchmark the procedure with a sensitivity study that determines its power to reject the background-only hypothesis in the presence of an injected WIMP dark matter signal, outperforming the classical, likelihood-based background rejection test. We show that our neural networks learn relevant energy features of the events from low-level, high-dimensional detector outputs, without the need to compress this data into lower-dimensional observables, thus reducing computational effort and information loss. For the future, our approach lays the foundation for an efficient end-to-end pipeline that eliminates the need for many of the corrections and cuts that are traditionally part of the analysis chain, with the potential of achieving higher accuracy and significant reduction of analysis time. Copyright © 2024, The Authors. All rights reserved.

关键词： Self-supervised learning

High precision calculation of the hadronic vacuum polarisation contribution to the muon anomaly

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arXiv 2024年

作者： Boccaletti, A. Borsanyi, Sz. Davier, M. Fodor, Z. Frech, F. Gérardin, A. Giusti, D. Kotov, A.Yu. Lellouch, L. Lippert, Th. Lupo, A. Malaescu, B. Mutzel, S. Portelli, A. Risch, A. Sjö, M. Stokes, F. Szabo, K.K. Toth, B.C. Wang, G. Zhang, Z. Department of Physics University of Wuppertal WuppertalD-42119 Germany Jülich Supercomputing Centre Forschungszentrum Jülich JülichD-52428 Germany IJCLab Université Paris-Saclay CNRS IN2P3 Orsay91405 France Physics Department Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences Pennsylvania State University University ParkPA16802 United States Institute for Theoretical Physics Eötvös University BudapestH-1117 Hungary University of California 9500 Gilman Drive La Jolla San DiegoCA92093 United States Aix Marseille Univ Université de Toulon CNRS CPT IPhU Marseille France Fakultät für Physik Universität Regensburg Regensburg93040 Germany LPNHE Sorbonne Université Université Paris Cité CNRS IN2P3 Paris75252 France Laboratoire de Physique de l'Ecole Normale Supérieure Mines Paris - PSL CNRS Inria PSL Research University Paris France School of Physics and Astronomy University of Edinburgh EdinburghEH9 3JZ United Kingdom RIKEN Center for Computational Science Kobe650-0047 Japan Special Research Centre for the Subatomic Structure of Matter Department of Physics University of Adelaide SA5005 Australia

For fifty years, the standard model of particle physics has been hugely successful in describing subatomic phenomena. Recently, this statement appeared to be contradicted by the strong disagreement between measurements of the anomalous magnetic moment of the muon [1], aµ, and the reference standard-model prediction [2]. Such a large discrepancy should signal the discovery of interactions or particles not present in the standard model. However, two independent determinations [3, 4] of the most uncertain contribution to the standard-model prediction display significantly less tension with the measurement. Here we present a new first-principle calculation of this contribution. We reduce uncertainties compared to our earlier computation [3] by 40%. To reach this unprecedented level of precision we improve on many aspects of the calculation. Namely, we perform large-scale lattice QCD simulations on finer lattices than in Ref. [3], allowing for an even more accurate continuum extrapolation. We also include a small, long-distance contribution obtained using input from experiments in a low-energy regime where they all agree. Combined with the extensive calculations of other standard model contributions summarised in Ref. [2], our result leads to a prediction that differs from the measurement of aµ by only 0.9 standard deviations. This provides a remarkable validation of the standard model to 0.37ppm. Copyright © 2024, The Authors. All rights reserved.

关键词： Forecasting

Analysis of GWTC-3 with fully precessing numerical relativity surrogate models

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arXiv 2023年

作者： Islam, Tousif Vajpeyi, Avi Shaik, Feroz H. Haster, Carl-Johan Varma, Vijay Field, Scott E. Lange, Jacob O’Shaughnessy, Richard Smith, Rory Department of Mathematics University of Massachusetts DartmouthMA02747 United States Center for Scientific Computing and Data Science Research University of Massachusetts DartmouthMA02747 United States Department of Statistics The University of Auckland New Zealand School of Physics and Astronomy Monash University VIC3800 Australia OzGrav The ARC Centre of Excellence for Gravitational Wave Discovery ClaytonVIC3800 Australia Department of Physics and Astronomy University of Nevada Las Vegas 4505 South Maryland Parkway Las VegasNV89154 United States Nevada Center for Astrophysics University of Nevada Las VegasNV89154 United States LIGO Laboratory Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 77 Massachusetts Ave CambridgeMA02139 United States Max Planck Institute for Gravitational Physics Albert Einstein Institute PotsdamD-14476 Germany Center for Computational Relativity and Gravitation Rochester Institute of Technology RochesterNY14623 United States University of Texas AustinTX78712 United States

The third Gravitational-Wave Transient Catalog (GWTC-3) contains 90 binary coalescence candidates detected by the LIGO-Virgo-KAGRA Collaboration (LVK). We provide a re-analysis of binary black hole (BBH) events using a recently developed numerical relativity (NR) waveform surrogate model, NRSur7dq4, that includes all ≤ 4 spin-weighted spherical harmonic modes as well as the complete physical effects of precession. Properties of the remnant black holes’ (BH’s) mass, spin vector, and kick vector are found using an associated remnant surrogate model NRSur7dq4Remnant. Both NRSur7dq4 and NRSur7dq4Remnant models have errors comparable to numerical relativity simulations and allow for high-accuracy parameter estimates. We restrict our analysis to 47 BBH events that fall within the regime of validity of NRSur7dq4 (mass ratios greater than 1/6 and total masses greater than 60M☉). While for most of these events our results match the LVK analyses that were obtained using the semi-analytical models such as IMRPhenomXPHM and SEOBNRv4PHM, we find that for more than 20% of events the NRSur7dq4 model recovers noticeably different measurements of black hole properties like the masses and spins, as well as extrinsic properties like the binary inclination and distance. For instance, GW150914_095045 exhibits noticeable differences in spin precession and spin magnitude measurements. Other notable findings include one event (GW191109_010717) that constrains the effective spin χeff to be negative at a 99.3% credible level and two events (GW191109_010717 and GW200129_065458) with well-constrained kick velocities. Furthermore, compared to the models used in the LVK analyses, NRSur7dq4 recovers a larger signal-to-noise ratio and/or Bayes factors for several events. While these findings have important astrophysical implications, some of the more interesting events are affected by transient detector noise, which can be challenging to remove from short-duration signals. Copyright © 2023, The Au

关键词： Black holes

WALLABY Pilot Survey & ASymba: Comparing H i Detection Asymmetries to the SIMBA Simulation

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arXiv 2025年

作者： Perron-Cormier, Mathieu Deg, Nathan Spekkens, Kristine Richardson, Mark L.A. Glowacki, Marcin Oman, Kyle A. Verheijen, Marc A.W. Hank, Nadine A.N. Blyth, Sarah Dénes, Helga Rhee, Jonghwan Elagali, Ahmed Shen, Austin Xiaofan Raja, Wasim Lee-Waddell, Karen Cortese, Luca Catinella, Barbara Westmeier, Tobias Department of Physics Engineering Physics and Astronomy Queen’s University KingstonONK7L 3N6 Canada Arthur B. McDonald Canadian Astroparticle Physics Research Institute 64 Bader Lane KingstonONK7L 3N6 Canada Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom International Centre for Radio Astronomy Research Curtin University BentleyWA6102 Australia Inter-University Institute for Data Intensive Astronomy Department of Astronomy University of Cape Town Cape Town South Africa Institute for Computational Cosmology Physics Department Durham University South Road DurhamDH1 3LE United Kingdom Centre for Extragalactic Astronomy Physics Department Durham University South Road DurhamDH1 3LE United Kingdom Kapteyn Astronomical Institute University of Groningen Landleven 12 Groningen9747 AD Netherlands Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa School of Physical Sciences and Nanotechnology Yachay Tech University Hacienda San José S/N Urcuquí100119 Ecuador University of Western Australia 35 Stirling Hwy CrawleyWA6009 Australia School of Biological Sciences The University of Western Australia CrawleyWA Australia CSIRO Space and Astronomy PO Box 1130 BentleyWA6102 Australia The University of Western Australia 35 Stirling Highway CrawleyWA6009 Australia Australia

An avenue for understanding cosmological galaxy formation is to compare morphometric parameters in observations and simulations of galaxy assembly. In this second paper of the ASymba: Asymmetries of H i in Simba Galaxies series, we measure atomic gas (H i) asymmetries in spatially-resolved detections from the untargetted WALLABY survey, and compare them to realizations of WALLABY-like mock samples from the SIMBA cosmological simulations. We develop a Scanline Tracing method to create mock galaxy H i datacubes which minimizes shot noise along the spectral dimension compared to particle-based methods, and therefore spurious asymmetry contributions. We compute 1D and 3D asymmetries for spatially-resolved WALLABY Pilot Survey detections, and find that the highest 3D asymmetries (A3D 0.5) stem from interacting systems or detections with strong bridges or tails. We then construct a series of WALLABY-like mock realizations drawn from the SIMBA 50 Mpc simulation volume, and compare their asymmetry distributions. We find that the incidence of high A3D detections is higher in WALLABY than in the SIMBA mocks, but that difference is not statistically significant (p-value = 0.05). The statistical power of quantitative comparisons of asymmetries such as the one presented here will improve as the WALLABY survey progresses, and as simulation volumes and resolutions increase. © 2025, CC BY.

关键词： Shot noise