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Quantum-centric Supercomputing for Materials Science: A Perspective on Challenges and Future Directions

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arXiv 2023年

作者： Alexeev, Yuri Amsler, Maximilian Barroca, Marco Antonio Bassini, Sanzio Battelle, Torey Camps, Daan Casanova, David Choi, Young Jai Chong, Frederic T. Chung, Charles Codella, Christopher Córcoles, Antonio D. Cruise, James Di Meglio, Alberto Duran, Ivan Eckl, Thomas Economou, Sophia Eidenbenz, Stephan Elmegreen, Bruce Fare, Clyde Faro, Ismael Fernández, Cristina Sanz Ferreira, Rodrigo Neumann Barros Fuji, Keisuke Fuller, Bryce Gagliardi, Laura Galli, Giulia Glick, Jennifer R. Gobbi, Isacco Gokhale, Pranav de la Puente Gonzalez, Salvador Greiner, Johannes Gropp, Bill Grossi, Michele Gull, Emanuel Healy, Burns Hermes, Matthew R. Huang, Benchen Humble, Travis S. Ito, Nobuyasu Izmaylov, Artur F. Javadi-Abhari, Ali Jennewein, Douglas Jha, Shantenu Jiang, Liang Jones, Barbara de Jong, Wibe Albert Jurcevic, Petar Kirby, William Kister, Stefan Kitagawa, Masahiro Klassen, Joel Klymko, Katherine Koh, Kwangwon Kondo, Masaaki Kürkçüoglu, Doga Murat Kurowski, Krzysztof Laino, Teodoro Landfield, Ryan Leininger, Matt Leyton-Ortega, Vicente Li, Ang Lin, Meifeng Liu, Junyu Lorente, Nicolas Luckow, Andre Martiel, Simon Martin-Fernandez, Francisco Martonosi, Margaret Marvinney, Claire Medina, Arcesio Castaneda Merten, Dirk Mezzacapo, Antonio Michielsen, Kristel Mitra, Abhishek Mittal, Tushar Moon, Kyungsun Moore, Joel Mostame, Sarah Motta, Mario Na, Young-Hye Nam, Yunseong Narang, Prineha Ohnishi, Yu-Ya Ottaviani, Daniele Otten, Matthew Pakin, Scott Pascuzzi, Vincent R. Pednault, Edwin Piontek, Tomasz Pitera, Jed Rall, Patrick Ravi, Gokul Subramanian Robertson, Niall Rossi, Matteo A.C. Rydlichowski, Piotr Ryu, Hoon Samsonidze, Georgy Sato, Mitsuhisa Saurabh, Nishant Sharma, Vidushi Sharma, Kunal Shin, Soyoung Slessman, George Steiner, Mathias Sitdikov, Iskandar Suh, In-Saeng Switzer, Eric D. Tang, Wei Thompson, Joel Todo, Synge Tran, Minh C. Trenev, Dimitar Trott, Christian Tseng, Huan-Hsin Tubman, Norm M. Tureci, Esin Valiñas, David García Vallecorsa, Sofia Wever, Christopher Wojciechowski, Konrad Wu, Xiaodi Yoo, Shinjae Yoshioka, Argonne National Laboratory LemontIL60439 United States Corporate Sector Research and Advance Engineering Robert Bosch GmbH Robert-Bosch-Campus 1 RenningenD-71272 Germany IBM Research RJ Rio de Janeiro20031-170 Brazil Centro Brasileiro de Pesquisas Físicas RJ Rio de Janeiro22290-180 Brazil CINECA via Magnanelli 6/3 BO Casalecchio di Reno40033 Italy Arizona State University TempeAZ United States National Energy Research Scientific Computing Center Lawrence Berkeley National Laboratory BerkeleyCA United States Euskadi Donostia-San Sebastián20018 Spain Ikerbasque Basque Foundation for Science Bilbao48009 Spain Department of Physics Yonsei University Seoul03722 Korea Republic of University of Chicago ChicagoIL United States IBM Quantum IBM T.J. Watson Research Center Yorktown Heights NY10598 United States Cambridge Consultants part of Capgemini Invent Cambridge United Kingdom Geneva1211 Switzerland Virginia Tech BlacksburgVA24061 United States Los Alamos National Laboratory Los AlamosNM87545 United States Osaka University Osaka560-8531 Japan Department of Chemistry Chicago Center for Theoretical Chemistry University of Chicago ChicagoIL United States Fraunhofer ITWM Rheinland-Pfalz Kaiserslautern67663 Germany Infleqtion ChicagoIL60622 United States University of Illinois Urbana-Champaign United States University of Michigan Ann ArborMI48109 United States Research Office Oak Ridge National Laboratory One Bethel Valley Road Oak RidgeTN37831 United States Hyogo Kobe650-0047 Japan Chemical Physics Theory Group Department of Chemistry University of Toronto TorontoONM5S 3H6 Canada Department of Physical and Environmental Sciences University of Toronto Scarborough TorontoONM1C 1A4 Canada Brookhaven National Laboratory UptonNY United States Rutgers University New BrunswickNJ United States IBM Quantum Almaden Research Center San JoseCA95120 United States Applied Mathematics and Computational Research Division

Computational models are an essential tool for the design, characterization, and discovery of novel materials. Computationally hard tasks in materials science stretch the limits of existing high-performance supercomputing centers, consuming much of their resources for simulation, analysis, and data processing. Quantum computing, on the other hand, is an emerging technology with the potential to accelerate many of the computational tasks needed for materials science. In order to do that, the quantum technology must interact with conventional high-performance computing in several ways: approximate results validation, identification of hard problems, and synergies in quantum-centric supercomputing. In this paper, we provide a perspective on how quantum-centric supercomputing can help address critical computational problems in materials science, the challenges to face in order to solve representative use cases, and new suggested directions. Copyright © 2023, The Authors. All rights reserved.

关键词： Characterization (materials science)

Activating Bip-orbitals in Dispersed Clusters of Amorphous BiOxfor Electrocatalytic Nitrogen Reduction

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Angewandte Chemie 2023年第15期135卷

作者： Dr. Jianxin Kang Xiangyu Chen Rutong Si Prof. Xiang Gao Prof. Shuo Zhang Prof. Gilberto Teobaldi Prof. Annabella Selloni Li-Min Liu Prof. Lin Guo School of Chemistry Beijing Advanced Innovation Center for Biomedical Engineering Key Laboratory of Bio-Inspired Smart Interfacial Science and Technology Beihang University Beijing 100191 China Beijing Computational Science Research Center Beijing 100193 China School of Physics Beihang University Beijing 100191 China Center for High Pressure Science and Technology Advanced Research Beijing 100190 China Shanghai Synchrotron Radiation Facility Shanghai Institute of Applied Physics Chinese Academy of Sciences Shanghai 201204 China Scientific Computing Department STFC UKRI Rutherford Appleton Laboratory Didcot OX11 0QX UK School of Chemistry University of Southampton Highfield Southampton SO17 1BJ UK Department of Chemistry Princeton University Princeton NJ 08544 USA

Catalytic strategies based on main group metals are significantly less advanced than those of transition metal catalysis, leaving untapped areas of potentially fruitful research. We here demonstrate an effective approach for the modulation of Bi 6p energy levels during the construction of atomically dispersed clusters of amorphous BiO x . Bi oxidation state is proposed to strongly affects the nitrogen fixation activity, with the half-occupied p z orbitals of the Bi 2+ ions being highly efficient toward electron injection into the inert N 2 molecule. With sufficient catalytic sites to adsorb and activate N 2 , the bonding between N 2 and catalyst is able to be in situ identified. The catalyst shows an outstanding Faraday efficiency (≈30 %) and high yield (≈113 μg h −1 mg −1 cat ) in NH 3 production, outperforming most of the existing catalysts in aqueous solution. These results lay the basis for developing the potential of p- block elements for catalysis of multi-electron reactions.

关键词： Amorphous Nanomaterial Electrocatalysis In Situ Identification Nitrogen Fixation p-Orbitals

Search for an isotropic gravitational-wave background with the Parkes Pulsar Timing Array

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arXiv 2023年

作者： Reardon, Daniel J. Zic, Andrew Shannon, Ryan M. Hobbs, George B. Bailes, Matthew Di Marco, Valentina Kapur, Agastya Rogers, Axl F. Thrane, Eric Askew, Jacob Ramesh Bhat, N.D. Cameron, Andrew Curylo, Malgorzata Coles, William A. Dai, Shi Goncharov, Boris Kerr, Matthew Kulkarni, Atharva Levin, Yuri Lower, Marcus E. Manchester, Richard N. Mandow, Rami Miles, Matthew T. Nathan, Rowina S. Oslowski, Stefan Russell, Christopher J. Spiewak, Renée Zhang, Songbo Zhu, Xing-Jiang Centre for Astrophysics and Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia OzGrav: The Australian Research Council Centre of Excellence for Gravitational Wave Discovery HawthornVIC3122 Australia Australia Telescope National Facility CSIRO Space and Astronomy P.O. Box 76 EppingNSW1710 Australia Department of Physics and Astronomy MQ Research Centre in Astronomy Astrophysics and Astrophotonics Macquarie University NSW2109 Australia School of Physics and Astronomy Monash University VIC3800 Australia OzGrav: The Australian Research Council Centre of Excellence for Gravitational Wave Discovery ClaytonVIC3800 Australia Institute for Radio Astronomy & Space Research Auckland University of Technology Private Bag 92006 Auckland1142 New Zealand International Centre for Radio Astronomy Research Curtin University BentleyWA6102 Australia Astronomical Observatory University of Warsaw Aleje Ujazdowskie 4 Warsaw00-478 Poland Electrical and Computer Engineering University of California La Jolla San DiegoCA United States School of Science Western Sydney University Locked Bag 1797 Penrith South DCNSW2751 Australia L'AquilaI-67100 Italy INFN Laboratori Nazionali del Gran Sasso AssergiI-67100 Italy Space Science Division US Naval Research Laboratory 4555 Overlook Ave SW WashingtonDC20375 United States Physics Department Columbia Astrophysics Laboratory Columbia University 538 West 120th Street New YorkNY10027 United States Center for Computational Astrophysics Flatiron Institute 162 5th Ave NY10011 United States Manly Astrophysics 15/41-42 East Esplanade ManlyNSW2095 Australia CSIRO Scientific Computing Australian Technology Park Locked Bag 9013 AlexandriaNSW1435 Australia Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy University of Manchester ManchesterM13 9PL United Kingdom Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China Advanced Instit

Pulsar timing arrays aim to detect nanohertz-frequency gravitational waves (GWs). A background of GWs modulates pulsar arrival times and manifests as a stochastic process, common to all pulsars, with a signature spatial correlation. Here we describe a search for an isotropic stochastic gravitational-wave background (GWB) using observations of 30 millisecond pulsars from the third data release of the Parkes Pulsar Timing Array (PPTA), which spans 18 years. Using current Bayesian inference techniques we recover and characterize a common-spectrum noise process. Represented as a strain spectrum hc = A(f/1yr−1)α, we measure (Equation presented) and α = −0.45 ± 0.20 respectively (median and 68% credible interval). For a spectral index of α = −2/3, corresponding to an isotropic background of GWs radiated by inspiraling supermassive black hole binaries, we recover an amplitude of (Equation presented). However, we demonstrate that the apparent signal strength is time-dependent, as the first half of our data set can be used to place an upper limit on A that is in tension with the inferred common-spectrum amplitude using the complete data set. We search for spatial correlations in the observations by hierarchically analyzing individual pulsar pairs, which also allows for significance validation through randomizing pulsar positions on the sky. For a process with α = −2/3, we measure spatial correlations consistent with a GWB, with an estimated false-alarm probability of p. 0.02 (approx. 2σ). The long timing baselines of the PPTA and the access to southern pulsars will continue to play an important role in the International Pulsar Timing Array. Copyright © 2023, The Authors. All rights reserved.

关键词： Pulsars

Dimerisierung eines reaktiven Azaacen Diradikals: Synthese eines kovalenten Azaacen-Käfigs

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Angewandte Chemie 2023年第32期135卷

作者： Kathleen Fuchs Dr. Samara Medina Rivero Anna Weidlich Dr. Frank Rominger Noel Israel Dr. Alexey A. Popov Prof. Dr. Andreas Dreuw Dr. Jan Freudenberg Prof. Juan Casado Prof. Dr. Uwe H. F. Bunz Organisch-Chemisches Institut Ruprecht-Karls-Universität Heidelberg Im Neuenheimer Feld 270 69120 Heidelberg Germany Department of Physical Chemistry University of Málaga Andalucia-Tech Campus de Teatinos s/n 29071 Málaga Spain Department of Physics & Astronomy University of Sheffield S37RH Sheffield UK Interdisciplinary Center for Scientific Computing Ruprecht-Karls-Universität Heidelberg Im Neuenheimer Feld 205 69120 Heidelberg Germany Center of Spectroelectrochemistry Leibniz Institute for Solid State and Materials Research (IFW) Dresden Helmholtzstraße 20 01069 Dresden Germany

Zwei Serien regioisomerer dicyanomethylen-substituierter Dithienodiazatetracenen mit formalen para - oder ortho -Chinodimethan-Untereinheiten wurden synthetisiert und charakterisiert. Während die para -Isomere ( p -n, Diradikalindex y 0 =0.01) stabil und isolierbar waren, dimerisierte das ortho -Isomer ( y 0 =0.98) zu einem kovalenten Azaacen-Käfig. Es wurden vier lange σ-CC-Bindungen gebildet und dabei die ehemaligen Tri iso propyl-silyl(TIPS)-Ethinyl-Gruppen in Kumulen-Einheiten umgewandelt. Der Azaacen-Käfig ( o -1) 2 wurde durch Einkristallröntgenstrukturanalyse charakterisiert. Weitere temperaturabhängige Experimente wie Infrarot- (IR), Elektronenspinresonanz- (ESR, Festkörper), Kernspinresonanz- (engl. nuclear magnetic resonance , NMR) und Absorptions- (engl. ultraviolet-visible , UV/Vis) Spektroskopie (Lösung) wurden durchgeführt, welche auf die Rückbildung des intermediären Diradikals o -1 hinweisen.

关键词： Azaacen-Käfig Cyclisierung σ-Dimerisierung Diradikal Kumulen

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

Waveform Modelling for the Laser Interferometer Space Antenna

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arXiv 2023年

作者： Afshordi, Niayesh Akçay, Sarp Seoane, Pau Amaro Antonelli, Andrea Aurrekoetxea, Josu C. Barack, Leor Barausse, Enrico Benkel, Robert Bernard, Laura Bernuzzi, Sebastiano Berti, Emanuele Bonetti, Matteo Bonga, Béatrice Bozzola, Gabriele Brito, Richard Buonanno, Alessandra Cárdenas-Avendaño, Alejandro Casals, Marc Chernoff, David F. Chua, Alvin J.K. Clough, Katy Colleoni, Marta Compère, Geoffrey Dhesi, Mekhi Druart, Adrien Durkan, Leanne Faye, Guillaume Ferguson, Deborah Field, Scott E. Gabella, William E. García-Bellido, Juan Gracia-Linares, Miguel Gerosa, Davide Green, Stephen R. Haney, Maria Hannam, Mark Heffernan, Anna Hinderer, Tanja Helfer, Thomas Hughes, Scott A. Husa, Sascha Isoyama, Soichiro Katz, Michael L. Kavanagh, Chris Khanna, Gaurav Kidder, Larry E. Korol, Valeriya Küchler, Lorenzo Laguna, Pablo Larrouturou, François Le Tiec, Alexandre Leather, Benjamin Lim, Eugene A. Lim, Hyun Littenberg, Tyson B. Long, Oliver Lousto, Carlos O. Lovelace, Geoffrey Lukes-Gerakopoulos, Georgios Lynch, Philip Macedo, Rodrigo P. Markakis, Charalampos Maggio, Elisa Mandel, Ilya Maselli, Andrea Mathews, Josh Mourier, Pierre Neilsen, David Nagar, Alessandro Nichols, David A. Novák, Jan Okounkova, Maria O’Shaughnessy, Richard Oshita, Naritaka O’Toole, Conor Pan, Zhen Pani, Paolo Pappas, George Paschalidis, Vasileios Pfeiffer, Harald P. Pompili, Lorenzo Pound, Adam Pratten, Geraint Rüter, Hannes R. Ruiz, Milton Sam, Zeyd Sberna, Laura Shapiro, Stuart L. Shoemaker, Deirdre M. Sopuerta, Carlos F. Spiers, Andrew Sundar, Hari Tamanini, Nicola Thompson, Jonathan E. Toubiana, Alexandre Tsokaros, Antonios Upton, Samuel D. van de Meent, Maarten Vernieri, Daniele Wachter, Jeremy M. Warburton, Niels Wardell, Barry Witek, Helvi Witzany, Vojtěch Yang, Huan Zilhão, Miguel Albertini, Angelica Arun, K.G. Bezares, Miguel Bonilla, Alexander Chapman-Bird, Christian Cownden, Bradley Cunningham, Kevin Devitt, Chris Dolan, Sam Duque, Francisco Dyson, Conor Fryer, Chris L. Gair, Jonathan R. Giacomazzo, Bruno Gupta, Priti Han, Wen-Biao Haas, Roland Perimeter Institute for Theoretical Physics WaterlooONN2L 2Y5 Canada School of Mathematics and Statistics University College Dublin Belfield Dublin 4 Ireland Universitat Politècnica de València València Spain Max Planck Institute for Extraterrestrial Physics Garching Germany Higgs Centre for Theoretical Physics Edinburgh United Kingdom Kavli Institute for Astronomy and Astrophysics Beijing100871 China William H. Miller III Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Astrophysics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom School of Mathematical Sciences and STAG Research Centre University of Southampton SouthamptonSO17 1BJ United Kingdom SISSA Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste IFPU Institute for Fundamental Physics of the Universe Via Beirut 2 Trieste34014 Italy Max Planck Institute for Gravitational Physics Albert Einstein Institute PotsdamD-14476 Germany Laboratoire Univers et Théories CNRS Observatoire de Paris Université PSL Université Paris Cité Meudon92190 France Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena Jena07743 Germany Dipartimento di Fisica "G. Occhialini" Universitá degli Studi di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy INFN Sezione di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy Institute for Mathematics Astrophysics and Particle Physics Radboud University Nijmegen6525 AJ Netherlands The University of Arizona Department of Astronomy TucsonAZ85721 United States CENTRA Departamento de Física Instituto Superior Técnico – IST Universidade de Lisboa – UL Avenida Rovisco Pais 1 Lisboa1049-001 Portugal Princeton Gravity Initiative Princeton University PrincetonNJ08544 United States Institut für Theoretische Physik Universität Leipzig Brüderstraße 16 Leipzig04103 Germany Rio de JaneiroCEP 22290-180 Brazil Department of Astronomy Cornell Univers

LISA, the Laser Interferometer Space Antenna, will usher in a new era in gravitational-wave astronomy. As the first anticipated space-based gravitational-wave detector, it will expand our view to the millihertz gravitational-wave sky, where a spectacular variety of interesting new sources abound: from millions of ultra-compact binaries in our Galaxy, to mergers of massive black holes at cosmological distances;from the beginnings of inspirals that will venture into the ground-based detectors’ view to the death spiral of compact objects into massive black holes, and many sources in between. Central to realising LISA’s discovery potential are waveform models, the theoretical and phenomenological predictions of the pattern of gravitational waves that these sources emit. This white paper is presented on behalf of the Waveform Working Group for the LISA Consortium. It provides a review of the current state of waveform models for LISA sources, and describes the significant challenges that must yet be overcome. © 2023, CC BY.

关键词： Gravity waves

Testing the no-hair nature of binary black holes using the consistency of multipolar gravitational radiation

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Physical Review D 2020年第2期101卷 024032-024032页

作者： Tousif Islam Ajit Kumar Mehta Abhirup Ghosh Vijay Varma Parameswaran Ajith B. S. Sathyaprakash International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bangalore 560089 India Center for Scientific Computation and Visualization Research University of Massachusetts Dartmouth Dartmouth Massachusetts 02740 USA Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-14476 Potsdam-Golm Germany Theoretical Astrophysics 350-17 California Institute of Technology Pasadena California 91125 USA Canadian Institute for Advanced Research CIFAR Azrieli Global Scholar MaRS Centre West Tower 661 University Avenue Suite 505 Toronto Ontario M5G 1M1 Canada Department of Physics and Department of Astronomy and Astrophysics The Pennsylvania State University University Park Pennsylvania 16802 USA School of Physics and Astronomy Cardiff University Cardiff CF24 3AA United Kingdom

Gravitational-wave (GW) observations of binary black holes offer the best probes of the relativistic, strong-field regime of gravity. Gravitational radiation in the leading order is quadrupolar. However, nonquadrupole (higher order) modes make appreciable contribution to the radiation from binary black holes with large mass ratios and misaligned spins. The multipolar structure of the radiation is fully determined by the intrinsic parameters (masses and spin angular momenta of the companion black holes) of a binary in quasicircular orbit. Following our previous work [S. Dhanpal, A. Ghosh, A. K. Mehta, P. Ajith, and B. S. Sathyaprakash, Phys. Rev. D 99, 104056 (2019).], we develop multiple ways of testing the consistency of the observed GW signal with the expected multipolar structure of radiation from binary black holes in general relativity. We call this a no-hair test of binary black holes as this is similar to testing the no-hair theorem for isolated black holes through mutual consistency of the quasinormal mode spectrum. We use Bayesian inference on simulated GW signals that are consistent/inconsistent with binary black holes in general relativity to demonstrate the power of the proposed tests. We also make estimate systematic errors arising as a result of neglecting companion spins.

关键词： Gravitational waves

DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements

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arXiv 2024年

作者： Adame, A.G. Aguilar, J. Ahlen, S. Alam, S. Alexander, D.M. Prieto, C. Allende Alvarez, M. Alves, O. Anand, A. Andrade, U. Armengaud, E. Avila, S. Aviles, A. Awan, H. Bahr-Kalus, B. Bailey, S. Baltay, C. Bault, A. Behera, J. BenZvi, S. Beutler, F. Bianchi, D. Blake, C. Blum, R. Bonici, M. Brieden, S. Brodzeller, A. Brooks, D. Buckley-Geer, E. Burtin, E. Calderon, R. Canning, R. Rosell, A. Carnero Cereskaite, R. Cervantes-Cota, J.L. Chabanier, S. Chaussidon, E. Chaves-Montero, J. Chebat, D. Chen, S. Chen, X. Claybaugh, T. Cole, S. Cuceu, A. Davis, T.M. Dawson, K. de la Macorra, A. de Mattia, A. Deiosso, N. Dey, A. Dey, B. Ding, Z. Doel, P. Edelstein, J. Eftekharzadeh, S. Eisenstein, D.J. Elbers, W. Elliott, A. Fagrelius, P. Fanning, K. Ferraro, S. Ereza, J. Findlay, N. Flaugher, B. Font-Ribera, A. Forero-Sánchez, D. Forero-Romero, J.E. Frenk, C.S. Garcia-Quintero, C. Garrison, L.H. Gaztañaga, E. Gil-Marín, H. Gontcho, S.A. Gontcho Gonzalez-Morales, A.X. Gonzalez-Perez, V. Gordon, C. Green, D. Gruen, D. Gsponer, R. Gutierrez, G. Guy, J. Hadzhiyska, B. Hahn, C. Hanif, M.M.S. Herrera-Alcantar, H.K. Honscheid, K. Howlett, C. Huterer, D. Iršič, V. Ishak, M. Joyce, R. Juneau, S. Karaçaylı, N.G. Kehoe, R. Kent, S. Kirkby, D. Kong, H. Koposov, S.E. Kremin, A. Krolewski, A. Lahav, O. Lai, Y. Lan, T.-W. Landriau, M. Lang, D. Lasker, J. Le Goff, J.M. Le Guillou, L. Leauthaud, A. Levi, M.E. Li, T.S. Lodha, K. Magneville, C. Manera, M. Margala, D. Martini, P. Matthewson, W. Maus, M. McDonald, P. Medina-Varela, L. Meisner, A. Mena-Fernández, J. Miquel, R. Moon, J. Moore, S. Moustakas, J. Mudur, N. Mueller, E. Muñoz-Gutiérrez, A. Myers, A.D. Nadathur, S. Napolitano, L. Neveux, R. Newman, J.A. Nguyen, N.M. Nie, J. Niz, G. Noriega, H.E. Padmanabhan, N. Paillas, E. Palanque-Delabrouille, N. Pan, J. Penmetsa, S. Percival, W.J. Pieri, M.M. Pinon, M. Poppett, C. Porredon, A. Prada, F. Pérez-Fernández, A. UAM CSIC Universidad Autónoma de Madrid Cantoblanco MadridE-28049 Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Physics Dept. Boston University 590 Commonwealth Avenue BostonMA02215 United States Tata Institute of Fundamental Research Homi Bhabha Road Mumbai400005 India Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Tenerife La LagunaE-38206 Spain Instituto de Astrofísica de Canarias C/ Vía Láctea s/n Tenerife La LagunaE-38205 Spain Department of Physics University of Michigan Ann ArborMI48109 United States Leinweber Center for Theoretical Physics University of Michigan 450 Church Street Ann ArborMI48109-1040 United States IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Instituto de Ciencias Físicas Universidad Autónoma de México Morelos Cuernavaca62210 Mexico Instituto Avanzado de Cosmología A. C. San Marcos 11 - Atenas 202. Magdalena Contreras Ciudad de México10720 Mexico Université Claude Bernard Lyon 1 CNRS IN2P3 IP2I Lyon France Physics Department Yale University P.O. Box 208120 New HavenCT06511 United States Department of Physics and Astronomy University of California Irvine92697 United States Department of Physics Kansas State University 116 Cardwell Hall ManhattanKS66506 United States Department of Physics & Astronomy University of Rochester 206 Bausch and Lomb Hall P.O. Box 270171 RochesterNY14627-0171 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Dipartimento di Fisica "Aldo Pontremoli" Università degli Studi di Milano Via Celoria 16 MilanoI-20133 Italy Centre for Astrophysics &

We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-α forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been thoroughly validated in a series of supporting papers as summarised in [1]. We combine the full-shape information with DESI’s DR1 constraints from the baryon acoustic oscillations (BAO) of these tracers. In the flat ΛCDM cosmological model, DESI (FS+BAO), combined with a baryon density prior from Big Bang Nucleosynthesis and a weak prior on the scalar spectral index, determines matter density to Ωm = 0.2962 ±0.0095, and the amplitude of mass fluctuations to σ8 = 0.842±0.034. The addition of the cosmic microwave background (CMB) data tightens these constraints to Ωm = 0.3056 ± 0.0049 and σ8 = 0.8121 ± 0.0053, while further addition of the the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data further improves these measurements, and leads to a 0.4% determination of the Hubble constant, H0 = (68.40 ± 0.27) km s−1 Mpc−1. In models with a time-varying dark energy equation of state parametrised by w0 and wa, combinations of DESI (FS+BAO) with CMB and type Ia supernovae continue to show the preference, previously found in the DESI DR1 BAO analysis, for w0 > −1 and wa ν 0 = 0.04 ± 0.22 and Σ0 = 0.044 ± 0.047, again in agreement with general relativity. © 2024, CC BY.

关键词： Dark energy

Observation of a Floquet symmetry-protected topological phase with superconducting qubits

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Research Square

research Square 2021年

作者： Zhang, Xu Jiang, Wenjie Deng, Jinfeng Wang, Ke Chen, Jiachen Zhang, Pengfei Ren, Wenhui Dong, Hang Xu, Shibo Gao, Yu Jin, Feitong Zhu, Xuhao Guo, Qiujiang Li, Hekang Song, Chao Gorshkov, Alexey V. Iadecola, Thomas Liu, Fangli Gong, Zhe-Xuan Wang, Zhen Deng, Dong-Ling Wang, H. Interdisciplinary Center for Quantum Information State Key Laboratory of Modern Optical Instrumentation Zhejiang Province Key Laboratory of Quantum Technology and Device Department of Physics Zhejiang University Hangzhou310027 China Center for Quantum Information IIIS Tsinghua University Beijing100084 China Alibaba-Zhejiang University Joint Research Institute of Frontier Technologies Hangzhou310027 China Hangzhou Global Scientific and Technological Innovation Center Zhejiang University Hangzhou311215 China Joint Quantum Institute Joint Center for Quantum Information and Computer Science University of Maryland and NIST College ParkMD United States Department of Physics and Astronomy Iowa State University AmesIA50011 United States Ames Laboratory AmesIA50011 United States QuEra Computing Inc. BostonMA02135 United States Department of Physics Colorado School of Mines GoldenCO80401 United States National Institute of Standards and Technology BoulderCO80305 United States Shanghai Qi Zhi Institute 41th Floor AI Tower No. 701 Yunjin Road Xuhui District Shanghai200232 China

Quantum many-body systems away from equilibrium host a rich variety of exotic phenomena that are forbidden by equilibrium thermodynamics. A prominent example is that of discrete time crystals [1–8], where time translational symmetry is spontaneously broken in periodically driven systems. Pioneering experiments have observed signatures of time crystalline phases with trapped ions [9, 10], spins in nitrogen-vacancy centers [11–13], ultracold atoms [14, 15], solid spin ensembles [16, 17], and superconducting qubits [18–20]. Here, we report the observation of a distinct type of intrinsically non-equilibrium state of matter, a Floquet symmetry-protected topological phase, which is implemented through digital quantum simulation with an array of programmable superconducting qubits. Unlike the discrete time crystals reported in previous experiments, where spontaneous breaking of the discrete time translational symmetry occurs for local observables throughout the whole system, the Floquet symmetry-protected topological phase observed in our experiment breaks the time translational symmetry only at the boundaries and has trivial dynamics in the bulk. More concretely, we observe robust long-lived temporal correlations and sub-harmonic temporal response for the edge spins over up to 40 driving cycles using a circuit whose depth exceeds 240. We demonstrate that the sub-harmonic response is independent of whether the initial states are random product states or symmetry-protected topological states, and experimentally map out the phase boundary between the time crystalline and thermal phases. Our work paves the way to exploring novel non-equilibrium phases of matter emerging from the interplay between topology and localization as well as periodic driving, with current noisy intermediate-scale quantum processors [21]. © 2021, CC BY.

关键词： Trapped ions