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arXiv 2021年

作者： Xue, Xiao Xia, Zi-Qing Zhu, Xingjiang Zhao, Yue Shu, Jing Yuan, Qiang Bhat, N.d. ramesh Cameron, Andrew d. dai, Shi Feng, Yi Goncharov, Boris Hobbs, George Howard, Eric Manchester, richard N. Parthasarathy, Aditya reardon, daniel J. russell, Christopher J. Shannon, ryan M. Spiewak, renée Thyagarajan, Nithyanandan Wang, Jingbo Zhang, Lei Zhang, Songbo II. Institute of Theoretical Physics Universität Hamburg Hamburg22761 Germany Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China Advanced Institute of Natural Sciences Beijing Normal University Zhuhai519087 China School of Physics and Astronomy Monash University ClaytonVIC3800 Australia OzGrav ARC Centre of Excellence for Gravitational Wave Discovery HawthornVIC3122 Australia Department of Physics and Astronomy University of Utah Salt Lake CityUT84112 United States CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing100190 China School of Physical Sciences University of Chinese Academy of Sciences Beijing100049 China CAS Center for Excellence in Particle Physics Beijing100049 China Center for High Energy Physics Peking University Beijing100871 China School of Fundamental Physics and Mathematical Sciences Hangzhou Institute for Advanced Study University of Chinese Academy of Sciences Hangzhou310024 China International Centre for Theoretical Physics Asia-Pacific Hangzhou Beijing China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China International Centre for Radio Astronomy Research Curtin University BentleyWA6102 Australia Australia Telescope National Facility CSIRO Astronomy and Space Science P.O. Box 76 EppingNSW1710 Australia Centre for Astrophysics and Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia School of Science Western Sydney University Locked Bag 1797 Penrith South DCNSW2751 Australia Zhejiang Lab Zhejiang Hangzhou311121 China Macquarie University Department of Physics and Astronomy SydneyNSW2109 Australia Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany CSIRO Scientific Computing Australian Technology Park Locked Bag 9013 AlexandriaNSW1435 Australia Jodrell

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 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 dark photon dark matter. 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. © 2021, CC BY.

关键词： Photons

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SPT clusters with dES and HST weak lensing. II. Cosmological constraints from the abundance of massive halos

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Physical review d 2024年第8期110卷 083510页

作者： S. Bocquet S. Grandis L. E. Bleem M. Klein J. J. Mohr T. Schrabback T. M. C. Abbott P. A. r. Ade M. Aguena A. Alarcon S. Allam S. W. Allen O. Alves A. Amon A. J. Anderson J. Annis B. Ansarinejad J. E. Austermann S. Avila d. Bacon M. Bayliss J. A. Beall K. Bechtol M. r. Becker A. N. Bender B. A. Benson G. M. Bernstein S. Bhargava F. Bianchini M. Brodwin d. Brooks L. Bryant A. Campos r. E. A. Canning J. E. Carlstrom A. Carnero rosell M. Carrasco Kind J. Carretero F. J. Castander r. Cawthon C. L. Chang C. Chang P. Chaubal r. Chen H. C. Chiang A. Choi T-L. Chou r. Citron C. Corbett Moran J. Cordero M. Costanzi T. M. Crawford A. T. Crites L. N. da Costa M. E. S. Pereira C. davis T. M. davis J. derose S. desai T. de Haan H. T. diehl M. A. dobbs S. dodelson C. doux A. drlica-Wagner K. Eckert J. Elvin-Poole S. Everett W. Everett I. Ferrero A. Ferté A. M. Flores J. Frieman J. Gallicchio J. García-Bellido M. Gatti E. M. George G. Giannini M. d. Gladders d. Gruen r. A. Gruendl N. Gupta G. Gutierrez N. W. Halverson I. Harrison W. G. Hartley K. Herner S. r. Hinton G. P. Holder d. L. Hollowood W. L. Holzapfel K. Honscheid J. d. Hrubes N. Huang J. Hubmayr E. M. Huff d. Huterer K. d. Irwin d. J. James M. Jarvis G. Khullar K. Kim L. Knox r. Kraft E. Krause K. Kuehn N. Kuropatkin F. Kéruzoré O. Lahav A. T. Lee P.-F. Leget d. Li H. Lin A. Lowitz N. MacCrann G. Mahler A. Mantz J. L. Marshall J. McCullough M. Mcdonald J. J. McMahon J. Mena-Fernández F. Menanteau S. S. Meyer r. Miquel J. Montgomery J. Myles T. Natoli A. Navarro-Alsina J. P. Nibarger G. I. Noble V. Novosad r. L. C. Ogando Y. Omori S. Padin S. Pandey P. Paschos S. Patil A. Pieres A. A. Plazas Malagón A. Porredon J. Prat C. Pryke M. raveri C. L. reichardt J. roberson r. P. rollins C. romero A. roodman J. E. ruhl E. S. rykoff B. r. Saliwanchik L. Salvati C. Sánchez E. Sanchez d. Sanchez Cid A. Saro K. K. Schaffer L. F. Secco I. Sevilla-Noarbe K. Sharon E. Sheldon T. Shin C. Sievers G. Smecher M. Smith T. Somboonpanyakul M. Sommer B. Stalder A. A. Stark J. Stephen V. Straz University Observatory Faculty of Physics Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstraße 25/8 6020 Innsbruck Austria High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Max Planck Institute for Extraterrestrial Physics Gießenbachstraße 1 85748 Garching Germany Argelander-Institut für Astronomie Auf dem Hügel 71 53121 Bonn Germany Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile School of Physics and Astronomy Cardiff University Cardiff CF24 3YB United Kingdom Laboratório Interinstitucional de e-Astronomia—LIneA Rua Gal. José Cristino 77 Rio de Janeiro Rio de Janeiro—20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall Stanford California 94305 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park California 94025 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom School of Physics University of Melbourne Parkville Victoria 3010 Australia NIST Quantum Devices Group 325 Broadway Mailcode 817.03 Boulder Colorado 80305 USA Department of Physics University of Colorado Boulder Colorado 80309 USA Institut de Física d’Altes Energies (IFAE) The Barcelona Institute of Science and Technology Campus UAB 08193 Bellaterra (Barcelona) Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth

We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel’dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the dark Energy Survey (dES) and the Hubble Space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range 0.25–1.78 over a total sky area of 5200 deg2. We use dES Year 3 weak-lensing data for 688 clusters with redshifts z<0.95 and HST weak-lensing data for 39 clusters with 0.6rements enable robust mass measurements of sample clusters and allow us to empirically constrain the SZ observable-mass relation without having to make strong assumptions about, e.g., the hydrodynamical state of the clusters. For a flat ΛCdM cosmology, and marginalizing over the sum of massive neutrinos, we measure Ωm=0.286±0.032, σ8=0.817±0.026, and the parameter combination σ8(Ωm/0.3)0.25=0.805±0.016. Our measurement of S8≡σ8Ωm/0.3=0.795±0.029 and the constraint from Planck CMB anisotropies (2018 TT, TE, EE+lowE) differ by 1.1σ. In combination with that Planck dataset, we place a 95% upper limit on the sum of neutrino masses ∑mν<0.18 eV. When additionally allowing the dark energy equation of state parameter w to vary, we obtain w=−1.45±0.31 from our cluster-based analysis. In combination with Planck data, we measure w=−1.34−0.15+0.22, or a 2.2σ difference with a cosmological constant. We use the cluster abundance to measure σ8 in five redshift bins between 0.25 and 1.8, and we find the results to be consistent with structure growth as predicted by the ΛCdM model fit to Planck primary CMB data.

关键词： Cosmological parameters dark energy Large scale structure of the Universe Galaxy clusters

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Erratum to: Search for exclusive Higgs and Z boson decays to ϕγ and ργ with the ATLAS detector

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Journal of high Energy Physics 2023年第12期2023卷 1-21页

作者： Aaboud, M. Aad, G. Abbott, B. Abdinov, O. Abeloos, B. Abidi, S. H. AbouZeid, O. S. Abraham, N. L. Abramowicz, H. Abreu, H. Abreu, r. Abulaiti, Y. Acharya, B. S. Adachi, S. Adamczyk, L. Adelman, J. Adersberger, M. Adye, T. Affolder, A. A. Afik, Y. Agatonovic-Jovin, T. Agheorghiesei, C. Aguilar-Saavedra, J. A. Ahlen, S. P. Ahmadov, F. Aielli, G. Akatsuka, S. Akerstedt, H. Åkesson, T. P. A. Akilli, E. Akimov, A. V. Alberghi, G. L. Albert, J. Albicocco, P. Alconada Verzini, M. J. Alderweireldt, S. C. 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. I. Alvarez Gonzalez, B. Álvarez Piqueras, d. Alviggi, M. G. Amadio, B. T. Amaral Coutinho, Y. Amelung, C. Amidei, d. Amor dos Santos, S. P. Amoroso, S. Amundsen, G. Anastopoulos, C. Ancu, L. S. Andari, N. Andeen, T. Anders, C. F. Anders, J. K. Anderson, K. J. Andreazza, A. Andrei, V. Angelidakis, S. Angelozzi, I. Angerami, A. Anisenkov, A. V. Anjos, N. Annovi, A. Antel, C. Antonelli, M. Antonov, A. Antrim, d. J. Anulli, F. Aoki, M. Aperio Bella, L. Arabidze, G. Arai, Y. Araque, J. P. Araujo Ferraz, V. Arce, A. T. H. Ardell, r. E. 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. Asquith, L. Assamagan, K. Astalos, r. Atkinson, M. Atlay, N. B. Augsten, K. Avolio, G. Axen, B. Ayoub, M. K. Azuelos, G. Baas, A. E. Baca, M. J. Bachacou, H. Bachas, K. Backes, M. Bagnaia, P. Bahmani, M. Bahrasemani, H. Baines, J. T. Bajic, M. Baker, O. K. Bakker, P. J. Baldin, E. M. Balek, P. Balli, F. Balunas, W. K. Banas, E. Bandyopadhyay, A. Banerjee, Sw. Bannoura, A. A. E. Barak, L. Barberio, E. L. Barberis, d. Barbero, M. Barillari, T. Barisits, M.-S. Barkeloo, J. T. Barklow, T. Barlow, N. Barnes, S. L. Barnett, B. M. Barnett, r. M. Barno Faculté des Sciences Université Mohamed Premier and LPTPM Oujda Morocco CPPM Aix-Marseille Université and CNRS/IN2P3 Marseille France Homer L. Dodge Department of Physics and Astronomy University of Oklahoma Norman United States of America Institute of Physics Azerbaijan Academy of Sciences Baku Azerbaijan LAL Univ. Paris-Sud CNRS/IN2P3 Université Paris-Saclay Orsay France Department of Physics University of Toronto Toronto Canada Santa Cruz Institute for Particle Physics University of California Santa Cruz Santa Cruz United States of America Department of Physics and Astronomy University of Sussex Brighton United Kingdom Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv Israel Department of Physics Technion: Israel Institute of Technology Haifa Israel Center for High Energy Physics University of Oregon Eugene United States of America Department of Physics Stockholm University Stockholm Sweden The Oskar Klein Centre Stockholm Sweden INFN Gruppo Collegato di Udine Sezione di Trieste Udine Italy ICTP Trieste Italy Department of Physics King’s College London London United Kingdom International Center for Elementary Particle Physics and Department of Physics The University of Tokyo Tokyo Japan AGH University of Science and Technology Faculty of Physics and Applied Computer Science Krakow Poland Department of Physics Northern Illinois University DeKalb United States of America Fakultät für Physik Ludwig-Maximilians-Universität München München Germany Particle Physics Department Rutherford Appleton Laboratory Didcot United Kingdom Institute of Physics University of Belgrade Belgrade Serbia Department of Physics Alexandru Ioan Cuza University of Iasi Iasi Romania Laboratório de Instrumentação e Física Experimental de Partículas – LIP Lisboa Portugal Departamento de Fisica Teorica y del Cosmos Universidad de Granada Granada Portugal Department of Physics Boston University Boston United States of America Joi

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reciprocal skin effect and its realization in a topolectrical circuit

arXiv

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arXiv 2019年

作者： Hofmann, Tobias Helbig, Tobias Schindler, Frank Salgo, Nora Brzezińska, Marta Greiter, Martin Kiessling, Tobias Wolf, david Vollhardt, Achim Kabaši, Anton Lee, Ching Hua Bilušić, Ante Thomale, ronny Neupert, Titus Institute for Theoretical Physics and Astrophysics University of Würzburg Am Hubland WürzburgD-97074 Germany Department of Physics University of Zurich Winterthurerstrasse 190 Zurich8057 Switzerland Kavli Institute for Theoretical Physics University of California Santa BarbaraCA93106 United States Department of Theoretical Physics Faculty of Fundamental Problems of Technology Wroclaw University of Science and Technology Wroclaw50-370 Poland Physikalisches Institut and Röntgen Research Center for Complex Material Systems Universität Würzburg WürzburgD-97074 Germany Centre of Excellence STIM University of Split Poljička cesta 35 SplitHR-21000 Croatia Department of Physics National University of Singapore Singapore117542 Singapore Institute of High Performance Computing A*STAR Singapore138632 Singapore University of Split Faculty of Science Rudera ¯ Boškovića 33 SplitHR-21000 Croatia

A system is non-Hermitian when it exchanges energy with its environment and non-reciprocal when it behaves differently upon the interchange of input and response. Within the field of metamaterial research on synthetic topological matter, the skin effect describes the conspiracy of non-Hermiticity and non-reciprocity to yield extensive anomalous localization of all eigenmodes in a (quasi) one-dimensional geometry. Here, we introduce the reciprocal skin effect, which occurs in non-Hermitian but reciprocal systems in two or more dimensions: Eigenmodes with opposite longitudinal momentum exhibit opposite transverse anomalous localization. We experimentally demonstrate the reciprocal skin effect in a passive rLC circuit, suggesting convenient alternative implementations in optical, acoustic, mechanical, and related platforms. Skin mode localization brings forth potential applications in directional and polarization detectors for electromagnetic waves. Copyright © 2019, The Authors. All rights reserved.

关键词： Timing circuits

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Ultralight vector dark matter search using data from the KAGrA O3GK run

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Physical review d 2024年第4期110卷 042001页

作者： A. G. Abac r. Abbott H. Abe I. Abouelfettouh F. Acernese K. Ackley C. Adamcewicz S. Adhicary N. Adhikari r. X. Adhikari V. K. Adkins V. B. Adya C. Affeldt d. Agarwal M. Agathos O. d. Aguiar I. Aguilar L. Aiello A. Ain P. Ajith 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 S. Anand 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 N. Aritomi F. Armato N. Arnaud M. Arogeti S. M. Aronson K. G. Arun G. Ashton Y. Aso M. Assiduo S. Assis de Souza Melo S. M. Aston P. Astone F. Aubin K. AultONeal G. Avallone S. Babak F. Badaracco C. Badger S. Bae S. Bagnasco E. Bagui Y. Bai J. G. Baier 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 S. d. Barthelmy M. A. Barton I. Bartos S. Basak A. Basalaev r. Bassiri A. Basti M. Bawaj P. Baxi J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale F. Beirnaert M. Bejger d. Belardinelli A. S. Bell V. Benedetto d. Beniwal 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 C. d. Blair d. G. Blair F. Bobba N. Bode G. Bogaert 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. Boumerdassi A. Bozzi C. Bradaschia P. r. Brady M. Braglia A. Branch M. Branchesi M. Breschi T. B Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-14476 Potsdam Germany LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Graduate School of Science Tokyo Institute of Technology 2-12-1 Ookayama Meguro-ku Tokyo 152-8551 Japan LIGO Hanford Observatory Richland Washington 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 United Kingdom OzGrav School of Physics & Astronomy Monash University Clayton 3800 Victoria Australia The Pennsylvania State University University Park Pennsylvania 16802 USA University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA Louisiana State University Baton Rouge Louisiana 70803 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Stanford University Stanford California 94305 USA Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa I-56127 Pisa Italy 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 Dipartimento di Fisica Università degli Studi di Torino I-10125 Torino Italy INFN Sezione di Torino I-10125 Torino Italy SUPA University of Glasgow Glasgow G12 8QQ United Kingdom OzGrav University of Western Austral

Among the various candidates for dark matter (dM), ultralight vector dM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGrA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector dM in the length change in the auxiliary channels. Here we present the result of a search for U(1)B−L gauge boson dM using the KAGrA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight dM, upper bounds on the coupling strength between the U(1)B−L gauge boson and ordinary matter are obtained for a range of dM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector dM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation timescale of dM.

关键词： dark matter Particle dark matter Gravitational wave detectors

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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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Galactic transient sources with the Cherenkov Telescope Array Observatory

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Monthly Notices of the royal Astronomical Society 2025年第1期540卷 205–238页

作者： Abe, K Abe, S Abhir, J Abhishek, A Acero, F Acharyya, A Adam, r Aguasca-Cabot, A Agudo, I Aguirre-Santaella, A Alfaro, J Alfaro, r Alvarez-Crespo, N Alves Batista, r Amans, J-P Amato, E Ambrosi, G Ambrosino, F Angüner, E O Antonelli, L A Aramo, C Arcaro, C Arnesen, T T H Asano, K Ascasibar, Y Aschersleben, J Ashkar, H Augusto Stuani, L Baack, d Backes, M Balazs, C Balbo, M Baquero Larriva, A Barbosa Martins, V Barres de Almeida, U Barrio, J A Barrios-Jiménez, L Batković, I Batzofin, r Baxter, J Becerra González, J Becker Tjus, J Belmont, r Benbow, W Bernete, J Bernlöhr, K Berti, A Bertucci, B Beshley, V Bhattacharjee, P Bhattacharyya, S Bigongiari, C Bissaldi, E Blanch, O Blazek, J Bocchino, F Boisson, C Bolmont, J Bonnoli, G Bonollo, A Bordas, P Bosnjak, Z Bottacini, E Böttcher, M Bradascio, F Bronzini, E Brown, A M Brunelli, G Bulgarelli, A Burelli, I Burger-Scheidlin, C Burmistrov, L Burton, M Buscemi, M Cailleux, J Campoy-Ordaz, A Cantlay, B K Capasso, G Caproni, A Capuzzo-dolcetta, r Caraveo, P Caroff, S Carosi, A Carosi, r Carquin, E Carrasco, M-S Cascone, E Cassol, F Castaldini, L Castrejon, N Castro-Tirado, A J Cerasole, d Ceribella, G Cerruti, M Chadwick, P M Chaty, S Chen, A W Chernyakova, M Chiavassa, A Chudoba, J Chytka, L Cicciari, G M Cifuentes, A Coimbra Araujo, C H Colapietro, M Conforti, V Contreras, J L Cortina, J Costa, A Costantini, H Cotter, G Cristofari, P Cuevas, O Curtis-Ginsberg, Z d’Aì, A d’Amico, G d’Ammando, F dai, S dazzi, F de Bony de Lavergne, M de Caprio, V de Cesare, G de Frondat Laadim, F de Gouveia dal Pino, E M de Lotto, B de Lucia, M de Martino, d de Menezes, r de Naurois, M de Ona Wilhelmi, E de Souza, V del Peral, L del Valle, M V delgado, C dell’aiera, M della Valle, M della Volpe, d depaoli, d devin, J di Girolamo, T di Piano, A di Pierro, F di Tria, r di Venere, L diebold, S dignam, C dima, r dinesh, A djuvsland, J dominik, r M dominis Prester, d donini, A dorner, d dörner, J doro, M dubos, C ducci, L dwarkadas, V V Ebr, J Eckner, C Egberts, K Einecke, S Elsässer, d Emery Department of Physics Tokai University 4-1-1 Kita-Kaname Hiratsuka Kanagawa 259-1292 Japan Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Kashiwa Chiba 277-8582 Japan ETH Zürich Institute for Particle Physics and Astrophysics Otto-Stern-Weg 5 CH-8093 Zürich Switzerland INFN and Università degli Studi di Siena Dipartimento di Scienze Fisiche della Terra e dell’Ambiente (DSFTA) Sezione di Fisica Via Roma 56 I-53100 Siena Italy Université Paris-Saclay Université Paris Cité CEA CNRS AIM F-91191 Gif-sur-Yvette Cedex France FSLAC IRL 2009 CNRS/IAC E-38205 La Laguna Tenerife Spain University of Alabama Tuscaloosa Department of Physics and Astronomy Gallalee Hall Box 870324 Tuscaloosa AL 35487-0324 USA Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Laboratoire Lagrange UF 06304 Nice France Laboratoire Leprince-Ringuet CNRS/IN2P3 École Polytechnique Institut Polytechnique de Paris F-91120 Palaiseau France Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Martí i Franquès 1 E-08028 Barcelona Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n E-18008 Granada Spain Institute for Computational Cosmology and Department of Physics Durham University South Road Durham DH1 3LE UK Pontificia Universidad Católica de Chile Av. Libertador Bernardo O’Higgins 340 8331150 Santiago Chile Universidad Nacional Autónoma de México Delegación Coyoacán 04510 Ciudad de México Mexico IPARCOS-UCM Instituto de Física de Partículas y del Cosmos and EMFTEL Department Universidad Complutense de Madrid E-28040 Madrid Spain Instituto de Física Teórica UAM/CSIC and Departamento de Física Teórica Universidad Autónoma de Madrid c/ Nicolás Cabrera 13-15 Campus de Cantoblanco UAM E-28049 Madrid Spain LUTH GEPI and LERMA Observatoire de Paris Université PSL Université Paris Cité CNRS 5 place Jules Janssen F-92190 Meudon France INAF – Osservatorio

A wide variety of Galactic sources show transient emission at soft and hard X-ray energies: low- and high-mass X-ray binaries containing compact objects, isolated neutron stars exhibiting extreme variability as magnetars as well as pulsar-wind nebulae. Although most of them can show emission up to MeV and/or GeV energies, many have not yet been detected in the TeV domain by Imaging Atmospheric Cherenkov Telescopes. In this paper, we explore the feasibility of detecting new Galactic transients with the Cherenkov Telescope Array Observatory (CTAO) and the prospects for studying them with Target of Opportunity observations. We show that CTAO will likely detect new sources in the TeV regime, such as the massive microquasars in the Cygnus region, low-mass X-ray binaries with low-viewing angle, flaring emission from the Crab pulsar-wind nebula or other novae explosions, among others. Since some of these sources could also exhibit emission at larger time-scales, we additionally test their detectability at longer exposures. We finally discuss the multiwavelength synergies with other instruments and large astronomical facilities.

关键词： binaries: general stars: magnetars novae cataclysmic variables pulsars: general gamma-rays: general

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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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First β-delayed γ-ray spectroscopy of Nb109: Single-quasiparticle states with prolate shape in Mo109

引用

Physical review C 2025年第5期111卷 054317-054317页

作者： S. Bae T. Sumikama P. M. Walker J. G. Li F. r. Xu S. Choi J. Ha F. Browne A. M. Bruce I. Nishizuka S. Nishimura P. doornenbal G. Lorusso P.-A. Söderström H. Watanabe r. daido Z. Patel S. rice L. Sinclair J. Wu Z. Xu A. Yagi H. Baba N. Chiga r. Carroll F. didierjean Y. Fang N. Fukuda G. Gey E. Ideguchi N. Inabe T. Isobe d. Kameda I. Kojouharov N. Kurz T. Kubo S. Lalkovski Z. Li r. Lozeva H. Nishibata A. Odahara Z. Podolyák P. H. regan O. J. roberts H. Sakurai H. Schaffner G. Simpson H. Suzuki H. Takeda M. Tanaka J. Taprogge V. Werner O. Wieland Department of Physics and Astronomy Seoul National University Seoul 08826 Republic of Korea RIKEN Nishina Center 2-1 Hirosawa Wako-shi Saitama 351-0198 Japan Center for Exotic Nuclear Studies Institute for Basic Science Daejeon 34126 Republic of Korea Center for Nuclear Study University of Tokyo Hirosawa 2-1 Wako Saitama 351-0198 Japan Department of Physics Tohoku University Aoba Sendai Miyagi 980-8578 Japan Department of Physics University of Surrey Guildford GU2 7XH United Kingdom CAS Key Laboratory of High Precision Nuclear Spectroscopy Institute of Modern Physics Lanzhou 730000 China School of Physics and State Key Laboratory of Nuclear Physics and Technology Peking University Beijing 100871 China School of Computing Engineering and Mathematics University of Brighton Brighton BN2 4GJ United Kingdom National Physical Laboratory Teddington Middlesex TW11 0LW United Kingdom Extreme Light Infrastructure-Nuclear Physics (ELI-NP)/Horia Hulubei National Institute for Physics and Nuclear Engineering (IFIN-HH) Str. Reactorulu Măgurele 077125 Romania IRCNPC School of Physics and Nuclear Energy Engineering Beihang University Beijing 100191 China Department of Physics Osaka University Toyonaka Osaka 560-0043 Japan Department of Physics University of York Heslington York YO10 5DD United Kingdom School of Physics Peking University Beijing 100871 China Department of Physics University of Tokyo Hongo Bunkyo-ku Tokyo 113-0033 Japan Department of Physics University of Hong Kong Pokfulam Road Hong Kong IPHC CNRS/IN2P3 Université de Strasbourg 67037 Strasbourg France LPSC Université Grenoble-Alpes CNRS/IN2P3 F-38026 Grenoble Cedex France ILL 38042 Grenoble Cedex France GSI Helmholtzzentrum für Schwerionenforschung GmbH 64291 Darmstadt Germany Department of Physics University of Sofia 1164 Sofia Bulgaria IJCLab CNRS/IN2P3 Université Paris-Saclay F-91405 Orsay France Research Center for Nuclear Physics (RCNP) Osaka University Toyonaka Osaka 560-00

The β-delayed γ-ray spectroscopy of Nb109 was performed to investigate the structure of Mo109 for the first time at the rIBF, Japan. Over one hundred transitions were assigned to Mo109, of these two were from the known isomeric state, and a new 33.1 keV excited state below the isomeric state was identified. The multipolarities of the transitions depopulating the isomeric state were restricted considering the internal conversion coefficients and empirically recommended upper limits of transition strengths. The intrinsic gyromagnetic ratio of the isomeric-state band was extracted, and the rotational band of the ground state was identified. The configurations of the ground and isomeric states in Mo109 were assigned to the ν1/2+[411] and ν5/2+[413] orbitals, respectively, with prolate shape. From the logft analysis, the ground state in Nb109 and a new excited state in Mo109 with a small logft value were assigned to the π5/2+[422] and ν5/2+[402] orbitals, respectively. The assignments were supported by potential energy surface calculations using the configuration-constrained method with a triaxially deformed Woods-Saxon potential. Although the ν1/2+[411] orbital was successfully predicted as the ground state, the order of quasiparticle configurations for excited states was not reproduced. The neutron emission probability in Nb109 β-decay was evaluated to be 27(11)% utilizing the β-delayed γ rays of Tc109 and Mo108.

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Search for continuous gravitational waves from 20 accreting millisecond x-ray pulsars in O3 LIGO data

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Physical review d 2022年第2期105卷 022002-022002页

作者： r. Abbott T. d. Abbott F. Acernese K. Ackley C. Adams N. Adhikari r. X. Adhikari V. B. Adya C. Affeldt d. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. d. Aguiar L. Aiello A. Ain T. Akutsu S. Albanesi A. Allocca P. A. Altin A. Amato C. Anand S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando T. Andrade N. Andres T. Andrić S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koji Arai Koya Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud S. M. Aronson K. G. Arun H. Asada Y. Asali G. Ashton Y. Aso M. Assiduo S. M. Aston P. Astone F. Aubin C. Austin S. Babak F. Badaracco M. K. M. Bader C. Badger S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird r. Bajpai M. Ball G. Ballardin S. W. Ballmer A. Balsamo G. Baltus S. Banagiri d. Bankar J. C. Barayoga C. Barbieri B. C. Barish d. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia d. Barta J. Bartlett M. A. Barton I. Bartos r. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto d. Beniwal T. F. Bennett J. d. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi d. Bersanetti A. Bertolini J. Betzwieser d. Beveridge r. Bhandare U. Bhardwaj d. Bhattacharjee S. Bhaumik I. A. Bilenko G. Billingsley S. Bini r. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn C. d. Blair d. G. Blair r. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini L. d. Bonavena F. Bondu E. Bonilla r. Bonnand P. Booker B. A. Boom r. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. r. Brady A. Bramley A. Branch M. Branchesi J. E. Brau M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks d. d. Brown S. Brunett G. Bruno r. Bruntz J. Bryant T. Bulik H. J. Bulten A. Buonanno r. Buscicchio d. Buskulic C. Buy r. L. Byer L. Cadonati G. Cagnoli C. Cahillane J. Calderón Bustillo J. d. Callaghan T. A. Callister E. Ca LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy OzGrav School of Physics & Astronomy Monash University Clayton 3800 Victoria Australia LIGO Livingston Observatory Livingston Louisiana 70754 USA University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa I-56127 Pisa Italy Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino I-10125 Torino Italy Università di Napoli “Federico II” Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy Université de Lyon Université Claude Bernard Lyon 1 CNRS Institut Lumière Matière F-69622 Villeurbanne France Department of Physics The University of Tokyo Bunkyo-ku Tokyo 113-0033 Japan Research Center for the Early Un

results are presented of searches for continuous gravitational waves from 20 accreting millisecond x-ray pulsars with accurately measured spin frequencies and orbital parameters, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. The search algorithm uses a hidden Markov model, where the transition probabilities allow the frequency to wander according to an unbiased random walk, while the J-statistic maximum-likelihood matched filter tracks the binary orbital phase. Three narrow subbands are searched for each target, centered on harmonics of the measured spin frequency. The search yields 16 candidates, consistent with a false alarm probability of 30% per subband and target searched. These candidates, along with one candidate from an additional target-of-opportunity search done for SAX J1808.4−3658, which was in outburst during one month of the observing run, cannot be confidently associated with a known noise source. Additional follow-up does not provide convincing evidence that any are a true astrophysical signal. When all candidates are assumed nonastrophysical, upper limits are set on the maximum wave strain detectable at 95% confidence, h095%. The strictest constraint is h095%=4.7×10−26 from IGr J17062−6143. Constraints on the detectable wave strain from each target lead to constraints on neutron star ellipticity and r-mode amplitude, the strictest of which are ε95%=3.1×10−7 and α95%=1.8×10−5 respectively. This analysis is the most comprehensive and sensitive search of continuous gravitational waves from accreting millisecond x-ray pulsars to date.

关键词： Gravitational waves Binary stars Neutron stars & pulsars

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