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Determination of the Relative Sign of the Higgs Boson Couplings to W and Z Bosons Using WH Production via Vector-Boson Fusion with the ATLAS Detector

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Physical Review Letters 2024年第14期133卷 141801页

作者： G. Aad B. Abbott K. Abeling N. J. Abicht S. H. Abidi A. Aboulhorma H. Abramowicz H. Abreu Y. Abulaiti B. S. Acharya C. Adam Bourdarios L. Adamczyk S. V. Addepalli M. J. Addison J. Adelman A. Adiguzel T. Adye A. A. Affolder Y. Afik M. N. Agaras J. Agarwala A. Aggarwal C. Agheorghiesei A. Ahmad F. Ahmadov W. S. Ahmed S. Ahuja X. Ai G. Aielli A. Aikot M. Ait Tamlihat B. Aitbenchikh I. Aizenberg M. Akbiyik T. P. A. Åkesson A. V. Akimov D. Akiyama N. N. Akolkar S. Aktas K. Al Khoury G. L. Alberghi J. Albert P. Albicocco G. L. Albouy S. Alderweireldt Z. L. Alegria M. Aleksa I. N. Aleksandrov C. Alexa T. Alexopoulos F. Alfonsi M. Algren M. Alhroob B. Ali H. M. J. Ali S. Ali S. W. Alibocus M. Aliev G. Alimonti W. Alkakhi C. Allaire B. M. M. Allbrooke J. F. Allen C. A. Allendes Flores P. P. Allport A. Aloisio F. Alonso C. Alpigiani M. Alvarez Estevez A. Alvarez Fernandez M. Alves Cardoso M. G. Alviggi M. Aly Y. Amaral Coutinho A. Ambler C. Amelung M. Amerl C. G. Ames D. Amidei S. P. Amor Dos Santos K. R. Amos V. Ananiev C. Anastopoulos T. Andeen J. K. Anders S. Y. Andrean A. Andreazza S. Angelidakis A. Angerami A. V. Anisenkov A. Annovi C. Antel M. T. Anthony E. Antipov M. Antonelli F. Anulli M. Aoki T. Aoki J. A. Aparisi Pozo M. A. Aparo L. Aperio Bella C. Appelt A. Apyan N. Aranzabal S. J. Arbiol Val C. Arcangeletti A. T. H. Arce E. Arena J-F. Arguin S. Argyropoulos J.-H. Arling O. Arnaez H. Arnold G. Artoni H. Asada K. Asai S. Asai N. A. Asbah K. Assamagan R. Astalos S. Atashi R. J. Atkin M. Atkinson H. Atmani P. A. Atmasiddha K. Augsten S. Auricchio A. D. Auriol V. A. Austrup G. Avolio K. Axiotis G. Azuelos D. Babal H. Bachacou K. Bachas A. Bachiu F. Backman A. Badea T. M. Baer P. Bagnaia M. Bahmani D. Bahner A. J. Bailey V. R. Bailey J. T. Baines L. Baines O. K. Baker E. Bakos D. Bakshi Gupta V. Balakrishnan R. Balasubramanian E. M. Baldin P. Balek E. Ballabene F. Balli L. M. Baltes W. K. Balunas J. Balz E. Banas M. Bandieramonte A. Bandyopadhyay S. Bansal L. Barak M. Barakat E. L. Barberio D. Barberis M. Barbero M. CPPM Aix-Marseille Université CNRS/IN2P3 Marseille France Homer L. Dodge Department of Physics and Astronomy University of Oklahoma Norman Oklahoma USA II. Physikalisches Institut Georg-August-Universität Göttingen Göttingen Germany Fakultät Physik Technische Universität Dortmund Dortmund Germany Physics Department Brookhaven National Laboratory Upton New York USA Faculté des sciences Université Mohammed V Rabat Morocco 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 Department of Physics New York University New York New York USA INFN Gruppo Collegato di Udine Sezione di Trieste Udine Italy ICTP Trieste Italy LAPP Université Savoie Mont Blanc CNRS/IN2P3 Annecy France AGH University of Krakow Faculty of Physics and Applied Computer Science Krakow Poland Department of Physics Brandeis University Waltham Massachusetts USA School of Physics and Astronomy University of Manchester Manchester United Kingdom Department of Physics Northern Illinois University DeKalb Illinois USA Department of Physics Istanbul University Istanbul Türkiye Particle Physics Department Rutherford Appleton Laboratory Didcot United Kingdom Santa Cruz Institute for Particle Physics University of California Santa Cruz Santa Cruz California USA Enrico Fermi Institute University of Chicago Chicago Illinois USA Institut de Física d’Altes Energies (IFAE) Barcelona Institute of Science and Technology Barcelona Spain INFN Sezione di Pavia Italy Dipartimento di Fisica Università di Pavia Pavia Italy Institut für Physik Universität Mainz Mainz Germany Department of Physics Alexandru Ioan Cuza University of Iasi Iasi Romania Geneva Switzerland Affiliated with an international laboratory covered by a cooperation agreement with Department of Physics McGill University Montreal Quebec Canada Department of Physics Royal Holloway University of London E

The associated production of Higgs and W bosons via vector-boson fusion is highly sensitive to the relative sign of the Higgs boson couplings to W and Z bosons. In this Letter, two searches for this process are presented, using 140 fb−1 of proton-proton collision data at s=13 TeV recorded by the ATLAS detector at the LHC. The first search targets scenarios with opposite-sign couplings of the W and Z bosons to the Higgs boson, while the second targets standard model-like scenarios with same-sign couplings. Both analyses consider Higgs boson decays into a pair of b quarks and W boson decays with an electron or muon. The data exclude the opposite-sign coupling hypothesis with a significance beyond 5σ, and the observed (expected) upper limit set on the cross section for vector-boson fusion WH production is 9.0 (8.7) times the standard model value at 95% confidence level.

关键词： Electroweak symmetry breaking Signatures with W or Z bosons Signatures with jets Higgs bosons

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The universal multiplicity function: counting haloes and voids

arXiv

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arXiv 2024年

作者： Verza, Giovanni Carbone, Carmelita Pisani, Alice Porciani, Cristiano Matarrese, Sabino Center for Cosmology and Particle Physics Department of Physics New York University 726 Broadway New YorkNY10003 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Dipartimento di Fisica e Astronomia "G. Galilei" Università degli Studi di Padova via Marzolo 8 PadovaI-35131 Italy INFN Sezione di Padova via Marzolo 8 PadovaI-35131 Italy Via Alfonso Corti 12 MilanoI-20133 Italy The Cooper Union for the Advancement of Science and Art 41 Cooper Square New YorkNY10003 United States Department of Astrophysical Sciences Princeton University Peyton Hall PrincetonNJ08544 United States Argelander-Institut für Astronomie Auf dem Hügel 71 BonnD-53121 Germany INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Gran Sasso Science Institute Viale F. Crispi 7 L’AquilaI-67100 Italy

We present a novel combination of the excursion-set approach with the peak theory formalism in Lagrangian space and provide accurate predictions for halo and void statistics over a wide range of scales. The set-up is based on an effective moving barrier. Besides deriving the corresponding numerical multiplicity function, we introduce a new analytical formula reaching the percent level agreement with the exact numerical solution obtained via Monte Carlo realisations down to small scales, ∼ 1012h−1M.. In the void case, we derive the dependence of the effective moving barrier on the void formation threshold, δv, by comparison against the Lagrangian void size function measured in the DEMNUni simulations. We discuss the mapping from Lagrangian to Eulerian space for both haloes and voids;adopting the spherical symmetry approximation, we obtain a strong agreement at intermediate and large scales. Finally, using the effective moving barrier, we derive Lagrangian void density profiles accurately matching measurements from cosmological simulations, a major achievement towards using void profiles for precision cosmology with the next generation of galaxy surveys. Copyright © 2024, The Authors. All rights reserved.

关键词： cosmology

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dm2gal: Mapping dark matter to galaxies with neural networks

arXiv

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arXiv 2020年

作者： Kasmanoff, Noah Tinker, Jeremy Villaescusa-Navarro, Francisco Ho, Shirley Center for Data Science New York University New YorkNY10011 United States Center for Cosmology and Particle Physics New York University New YorkNY10011 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States

Maps of cosmic structure produced by galaxy surveys are one of the key tools for answering fundamental questions about the Universe. Accurate theoretical predictions for these quantities are needed to maximize the scientific return of these programs. Simulating the Universe by including gravity and hydrodynamics is one of the most powerful techniques to accomplish this;unfortunately, these simulations are very expensive computationally. Alternatively, gravity-only simulations are cheaper, but do not predict the locations and properties of galaxies in the cosmic web. In this work, we use convolutional neural networks to paint galaxy stellar masses on top of the dark matter field generated by gravity-only simulations. Stellar mass of galaxies are important for galaxy selection in surveys and thus an important quantity that needs to be predicted. Our model outperforms the state-of-the-art benchmark model and allows the generation of fast and accurate models of the observed galaxy distribution. © 2020, CC BY.

关键词： Galaxies

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The AGEL Survey data Release 2: A Gravitational Lens Sample for Galaxy Evolution and cosmology

arXiv

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arXiv 2025年

作者： Barone, Tania M. Vasan, Keerthi G.C. Tran, Kim-Vy Kacprzak, Glenn G. Glazebrook, Karl Jones, Tucker Bowden, Duncan J. Dalessandro, Faith Sahu, Nandini Skobe, Hannah Allen, Rebecca J. Baker, A. Makai Ballard, Daniel J. Chen, Yuguang Collett, Thomas E. Ferrami, Giovanni González, Jimena Gottemoller, William Harshan, Anishya Huang, Xiaosheng Iwamoto, Leena Jacobs, Colin Jeltema, Tesla E. Gupta, Kaustubh Rajesh Lewis, Geraint F. Lopez, Sebastian Nanayakkara, Themiya Nielsen, Nikole M. O’Donnell, Jackson Qu, Huimin Rhoades, Sunny Shajib, Anowar Sweet, Sarah M. Tejos, Nicolas Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia Australia Department of Physics and Astronomy University of California Davis 1 Shields Avenue DavisCA95616 United States The Observatories of the Carnegie Institution for Science 813 Santa Barbara Street PasadenaCA91101 United States Center for Astrophysics Harvard & Smithsonian CambridgeMA02138 United States School of Physics & Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom University of New South Wales SydneyNSW2052 Australia Department of Physics McWilliams Center for Cosmology and Astrophysics Carnegie Mellon University 5000 Forbes Avenue PittsburghPA15213 United States School of Physics and Astronomy Monash University ClaytonVIC3800 Australia Sydney Institute for Astronomy School of Physics The University of Sydney A28 NSW2006 Australia Department of Physics The Chinese University of Hong Kong Shatin N.T. Hong Kong Institute of Cosmology and Gravitation University of Portsmouth Burnaby Rd PortsmouthPO1 3FX United Kingdom School of Physics University of Melbourne ParkvilleVIC3010 Australia Physics Department University of Wisconsin-Madison 2320 Chamberlin Hall. MadisonWI53706-1390 United States University of Ljubljana Department of Mathematics and Physics Jadranska ulica 19 LjubljanaSI-1000 Slovenia Department of Physics & Astronomy University of San Francisco 2130 Fulton Street San FranciscoCA94117-1080 United States 4 Physics Division Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States University of California Santa Cruz Santa CruzCA95064 United States Santa Cruz Institute for Particle Physics Santa CruzCA95064 United States Departamento de Astronomía Universidad de Chile Casilla 36-D Santiago Chile Homer L. Dodge Department of Physics and Astronomy The University of Oklahoma 440 W. Brooks St. NormanOK73019 United States Department o

The ASTRO 3D Galaxy Evolution with Lenses (AGEL) Survey is an ongoing effort to spectroscopically confirm a diverse sample of gravitational lenses with high spatial resolution imaging, to facilitate a broad range of science outcomes. The AGEL systems span single galaxy-scale deflectors to groups and clusters, and include rare targets such as galaxy-scale lenses with multiple sources, lensed quiescent galaxies, and Einstein rings. We build on the 77 systems presented in Tran et al. 2022 (AGEL data release 1) to present a total 138 lenses, and high resolution F140W and F200LP Hubble Space Telescope images for 71 lenses from a completed HST SNAP program. Lens candidates were originally identified by convolutional neural networks in the DES and DECaLS imaging fields, and of the targets with follow-up spectroscopy we find a high (96 %) success rate. Compared with other spectroscopic lens samples, AGEL lenses tend to have both higher redshift deflectors and sources. We briefly discuss the common causes of false-positive candidates, and strategies for mitigating false-positives in next generation lens searches. Lastly, we present 6 galaxy-scale double-source plane lenses useful for cosmological analyses. With next-generation telescopes and surveys such as Euclid, Vera Rubin’s Legacy Survey of Space and Time, Keck Observatory’s KAPA program, and 4MOST’s 4SLSLS surveys on the horizon, the AGEL survey represents a pathfinder for refining automated candidate search methods and identifying and triaging candidates for followup based on scientific potential. Copyright © 2025, The Authors. All rights reserved.

关键词： cosmology

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GRB 180128A: A Second Magnetar Giant Flare Candidate from the Sculptor Galaxy

arXiv

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arXiv 2023年

作者： Trigg, Aaron C. Burns, Eric Roberts, Oliver J. Negro, Michela Svinkin, Dmitry S. Baring, Matthew G. Wadiasingh, Zorawar Christensen, Nelson L. Andreoni, Igor Briggs, Michael S. Lalla, Niccolò Di Frederiks, Dmitry D. Lipunov, Vladimir M. Omodei, Nicola Ridnaia, Anna V. Veres, Peter Lysenko, Alexandra L. Department of Physics & Astronomy Louisiana State University Baton RougeLA70803 United States Science and Technology Institute Universities Space and Research Association 320 Sparkman Drive HuntsvilleAL35805 United States Ioffe Institute 26 Politekhnicheskaya St. Petersburg194021 Russia Department of Physics and Astronomy MS 108 Rice University 6100 Main Street HoustonTX77251-1892 United States Astrophysics Science Division NASA/GSFC GreenbeltMD20771 United States Department of Astronomy University of Maryland College ParkMD20742 United States Center for Research and Exploration in Space Science and Technology NASA/GSFC GreenbeltMD20771 United States Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Artemis Nice06304 France Joint Space-Science Institute University of Maryland College ParkMD20742 United States Astrophysics Science Division NASA Goddard Space Flight Center Mail Code 661 GreenbeltMD20771 United States Department of Space Science University of Alabama in Huntsville HuntsvilleAL35899 United States Department of Physics Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305 United States Department of Physics Lomonosov Moscow State University Sternberg Astronomical Institute Univeristetskij Prospekt Moscow119991 Russia

Magnetars are slowly rotating neutron stars that possess the strongest magnetic fields (1014−1015 G) known in the cosmos. They display a range of transient high-energy electromagnetic activity. The brightest and most energetic of these events are the gamma-ray bursts (GRBs) known as magnetar giant flares (MGFs), with isotropic energy E ≈ 1044 − 1046 erg. There are only seven detections identified as MGFs to date: three unambiguous events occurred in our Galaxy and the Magellanic Clouds, and the other four MGF candidates are associated with nearby star-forming galaxies. As all seven identified MGFs are bright at Earth, additional weaker events remain unidentified in archival data. We conducted a search of the Fermi Gamma-ray Burst Monitor (GBM) database for candidate extragalactic MGFs and, when possible, collected localization data from the Interplanetary Network (IPN) satellites. Our search yielded one convincing event, GRB 180128A. IPN localizes this burst with NGC 253, commonly known as the Sculptor Galaxy. This event is the second MGF in modern astronomy to be associated with this galaxy and the first time two bursts are associated with a single galaxy outside our own. Here, we detail the archival search criteria that uncovered this event and its spectral and temporal properties, which are consistent with expectations for a MGF. We also discuss the theoretical implications and finer burst structures resolved from various binning methods. Our analysis provides observational evidence for an eighth identified MGF. © 2023, CC BY-NC-ND.

关键词： Galaxies

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Application of 3D U-Net Neural Networks in Extracting the Epoch of Reionization Signal from SKA-Low Observations Based on Real Observations of NCP Field from LOFAR

arXiv

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arXiv 2024年

作者： Gao, Li-Yang Koopmans, Léon V.E. Mertens, Florent G. Munshi, Satyapan Li, Yichao Brackenhoff, Stefanie A. Ceccotti, Emilio Chege, J. Kariuki Acharya, Anshuman Ghara, Raghunath Giri, Sambit K. Iliev, Ilian T. Mellema, Garrelt Zhang, Xin Liaoning Key Laboratory of Cosmology and Astrophysics College of Sciences Northeastern University Shenyang110819 China Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands LERMA Observatoire de Paris Université PSL CNRS Sorbonne Université ParisF-75014 France INAF - Istituto di Radioastronomia Via P. Gobetti 101 Bologna40129 Italy Max-Planck-Institut für Astrophysik Garching85748 Germany Department of Physical Sciences Indian Institute of Science Education and Research Mohanpur WB Kolkata741246 India Van Swinderen Institute for Particle Physics and Gravity University of Groningen Nijenborgh 4 Groningen9747 AG Netherlands Department of Physics & Astronomy University of Sussex BrightonBN1 9QH United Kingdom Dept. of Astronomy & Oskar Klein Centre Stockholm University AlbaNova Stockholm University StockholmSE-106 91 Sweden MOE Key Laboratory of Data Analytics and Optimization for Smart Industry Northeastern University Shenyang110819 China National Frontiers Science Center for Industrial Intelligence and Systems Optimization Northeastern University Shenyang110819 China

Neutral hydrogen (HI) serves as a crucial probe for the Cosmic Dawn and the Epoch of Reionization (EoR). Actual observations of the 21-cm signal often encounter challenges such as thermal noise and various systematic effects. To overcome these challenges, we simulate SKA-Low-depth images and process them with a deep learning method. We utilized foreground residuals acquired by LOFAR during actual North Celestial Pole (NCP) field observations, thermal and excess variances calculated via Gaussian process regression (GPR), and 21-cm signals generated with 21cmFAST for signal extraction tests. Our approach to overcome these foreground, thermal noise, and excess variance components employs a 3D U-Net neural network architecture for image analysis. When considering thermal noise corresponding to 1400 hours of integration, U-Net provides reliable 2D power spectrum predictions, and robustness tests ensure that we get realistic EoR signals. Adding foreground residuals, however, causes inconsistencies below the horizon delay-line. Lastly, evaluating both thermal and excess variance with observations up to 3700 and 14000 hours ensures reliable power spectrum estimations within the EoR window and across nearly all scales, respectively. Copyright © 2024, The Authors. All rights reserved.

关键词： Thermal noise

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TAROGE-M: Radio Antenna Array on Antarctic High Mountain for Detecting Near-Horizontal Ultra-High Energy Air Showers

arXiv

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arXiv 2022年

作者： Wang, Shih-Hao Nam, Jiwoo Chen, Pisin Chen, Yaocheng Choi, Taejin Ham, Young-Bae Hsu, Shih-Ying Huang, Jian-Jung Huang, Ming-Huey A. Jee, Geonhwa Jung, Jongil Kim, Jieun Kuo, Chung-Yun Kwon, Hyuck-Jin Lee, Changsup Leung, Chung-Hei Liu, Tsung-Che Shiao, Yu-Shao J. Shin, Bok-Kyun Wang, Min-Zu Wang, Yu-Hsin Anker, Astrid Barwick, Steven W. Besson, Dave Z. Bouma, Sjoerd Cataldo, Maddalena Gaswint, Geoffrey Glaser, Christian Hallmann, Steffen Hanson, Jordan C. Henrichs, Jakob Kleinfelder, Stuart A. Lahmann, Robert Meyers, Zachary S. Nelles, Anna Novikov, Alexander Paul, Manuel P. Pyras, Lilly Persichilli, Christopher Plaisier, Ilse Rice-Smith, Ryan Seikh, Mohammad F.H. Tatar, Joulien Welling, Christoph Zhao, Leshan Department of Physics National Taiwan University Taipei10617 Taiwan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan Kavli Institute for Particle Astrophysics and Cosmology SLAC National Accelerator Laboratory Stanford University Stanford CA94305 United States Division of Atmospheric Sciences Korea Polar Research Institute Incheon Korea Republic of Department of Polar Science Korea University of Science and Technology Daejeon Korea Republic of Department of Energy Engineering National United University Miaoli Taiwan Department of Astronomy Space Science and Geology Chungnam National University Daejeon34134 Korea Republic of Department of Physics and Astronomy University of Delaware NewarkDE19716 United States Department of Electrophysics National Yang Ming Chiao Tung University Hsinchu300 Taiwan National Nano Device Laboratories Hsinchu300 Taiwan Ulsan National Institute of Science and Technology Ulsan44919 Korea Republic of Department of Physics and Astronomy University of California IrvineCA92697 United States Department of Physics and Astronomy University of Kansas LawrenceKS66045 United States DESY Zeuthen15738 Germany ECAP Friedrich-Alexander-Universität Erlangen-Nürnberg Erlangen91058 Germany Uppsala University Department of Physics and Astronomy UppsalaSE-752 37 Sweden Whittier College Department of Physics WhittierCA90602 United States Department of Electrical Engineering and Computer Science University of California IrvineCA92697 United States Research Cyberinfrastructure Center University of California IrvineCA92697 United States

The TAROGE-M radio observatory is a self-triggered antenna array on top of the ∼2700 m high Mt. Melbourne in Antarctica, designed to detect impulsive geomagnetic emission from extensive air showers induced by ultra-high energy (UHE) particles beyond 1017eV, including cosmic rays, Earth-skimming tau neutrinos, and particularly, the "ANITA anomalous events" (AAE) from near and below the horizon. The six AAE discovered by the ANITA experiment have signal features similar to tau neutrinos but that hypothesis is in tension either with the interaction length predicted by Standard Model or with the flux limits set by other experiments. Their origin remains uncertain, requiring more experimental inputs for clarification. The detection concept of TAROGE-M takes advantage of a high altitude with synoptic view toward the horizon as an efficient signal collector, and the radio quietness as well as strong and near vertical geomagnetic field in Antarctica, enhancing the relative radio signal strength. This approach has a low energy threshold, high duty cycle, and is easy to extend for quickly enlarging statistics. Here we report experimental results from the first TAROGE-M station deployed in January 2020, corresponding to approximately one month of livetime. The station consists of six receiving antennas operating at 180–450 MHz, and can reconstruct source directions of impulsive events with an angular resolution of ∼ 0.3°, calibrated in situ with a drone-borne pulser system. To demonstrate TAROGE-M’s ability to detect UHE air showers, a search for cosmic ray signals in 25.3-days of data together with the detection simulation were conducted, resulting in seven identified candidates. The detected events have a mean reconstructed energy of 0.95+0−0.3146 EeV and zenith angles ranging from 25° to 82°, with both distributions agreeing with the simulations, indicating an energy threshold at about 0.3 EeV. The estimated cosmic ray flux at that energy is (formula presented), also consis

关键词： Cosmic rays

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The Wavelength-shifting Optical Module for the IceCube Upgrade 37

The Wavelength-shifting Optical Module for the IceCube Upgra...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Rack-Helleis, John Pollmann, Anna Rongen, Martin Abbasi, R. Ackermann, M. Adams, J. Aguilar, J.A. Ahlers, M. Ahrens, M. Alispach, C. Alves, A.A. Amin, N.M. An, R. Andeen, K. Anderson, T. Anton, G. Argüelles, C. Ashida, Y. Axani, S. Bai, X. Balagopal, A.V. Barbano, A. Barwick, S.W. Bastian, B. Basu, V. Baur, S. Bay, R. Beatty, J.J. Becker, K.-H. Becker Tjus, J. Bellenghi, C. BenZvi, S. Berley, D. Bernardini, E. Besson, D.Z. Binder, G. Bindig, D. Blaufuss, E. Blot, S. Boddenberg, M. Bontempo, F. Borowka, J. Böser, S. Botner, O. Böttcher, J. Bourbeau, E. Bradascio, F. Braun, J. Bron, S. Brostean-Kaiser, J. Browne, S. Burgman, A. Burley, R.T. Busse, R.S. Campana, M.A. Carnie-Bronca, E.G. Chen, C. Chirkin, D. Choi, K. Clark, B.A. Clark, K. Classen, L. Coleman, A. Collin, G.H. Conrad, J.M. Coppin, P. Correa, P. Cowen, D.F. Cross, R. Dappen, C. Dave, P. De Clercq, C. DeLaunay, J.J. Dembinski, H. Deoskar, K. De Ridder, S. Desai, A. Desiati, P. de Vries, K.D. de Wasseige, G. de With, M. DeYoung, T. Dharani, S. Diaz, A. Díaz-Vélez, J.C. Dittmer, M. Dujmovic, H. Dunkman, M. DuVernois, M.A. Dvorak, E. Ehrhardt, T. Eller, P. Engel, R. Erpenbeck, H. Evans, J. Evenson, P.A. Fan, K.L. Fazely, A.R. Fiedlschuster, S. Fienberg, A.T. Filimonov, K. Finley, C. Fischer, L. Fox, D. Franckowiak, A. Friedman, E. Fritz, A. Fürst, P. Gaisser, T.K. Gallagher, J. Ganster, E. Garcia, A. Garrappa, S. Gerhardt, L. Ghadimi, A. Glaser, C. Glauch, T. Glüsenkamp, T. Goldschmidt, A. Gonzalez, J.G. Goswami, S. Grant, D. Grégoire, T. Griswold, S. Gündüz, M. Günther, C. Haack, C. Hallgren, A. Halliday, R. Halve, L. Halzen, F. Ha Minh, M. Hanson, K. Hardin, J. Harnisch, A.A. Haungs, A. Hauser, S. Hebecker, D. Helbing, K. Henningsen, F. Hettinger, E.C. Hickford, S. Hignight, J. Hill, C. Hill, G.C. Hoffman, K.D. Hoffmann, R. Hoinka, T. Hokanson-Fasig, B. Hoshina, K. Huang, F. Huber, M. Huber, T. Hultqvist, K. Hünnefeld, M. Institute for Physics JGU Mainz MainzD-55122 Germany Department of Physics Bergische Universität Wuppertal Gaußstraße 20 Wuppertal Germany III. Physikalisches Institut RWTH Aachen University AachenD-52056 Germany Department of Physics University of Adelaide Adelaide5005 Australia Dept. of Physics and Astronomy University of Alaska Anchorage 3211 Providence Dr. AnchorageAK99508 United States Dept. of Physics University of Texas at Arlington 502 Yates St. Science Hall Rm 108 Box 19059 ArlingtonTX76019 United States CTSPS Clark-Atlanta University AtlantaGA30314 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology AtlantaGA30332 United States Dept. of Physics Southern University Baton RougeLA70813 United States Dept. of Physics University of California BerkeleyCA94720 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Institut für Physik Humboldt-Universität zu Berlin BerlinD-12489 Germany Fakultät für Physik & Astronomie Ruhr-Universität Bochum BochumD-44780 Germany Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dienst ELEM BrusselsB-1050 Belgium Department of Physics Laboratory for Particle Physics and Cosmology Harvard University CambridgeMA02138 United States Dept. of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Dept. of Physics Institute for Global Prominent Research Chiba University Chiba263-8522 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Dept. of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Astronomy Ohio State University ColumbusOH43210 United States Dept. of Physics Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Niels Bohr Institute University

The Wavelength-shifting Optical Module (WOM) is a novel optical sensor that uses wavelength shifting and light guiding to substantially enhance the photosensitive area of UV optical modules. It has been designed for the IceCube Upgrade, a seven-string extension of the IceCube detector planned for the 2022/2023 South Pole deployment season. The WOM consists of a hollow quartz cylinder coated in wavelength shifting paint which serves as detection area and has two photomultipliers (PMTs) attached to the end faces. The light-collecting tube increases the effective photocathode area of the PMTs without producing additional dark current, making it suitable for low-signal, low-noise applications. We report on the design and performance of the WOM with a focus on the 12 modules in production for deployment in the IceCube Upgrade. While the WOM will be deployed in IceCube, its design is applicable to any large-volume particle detector based on the detection of Cherenkov light. © Copyright owned by the author(s).

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When to Point Your Telescopes: Gravitational Wave Trigger Classification for Real-Time Multi-Messenger Followup Observations

arXiv

引用

arXiv 2023年

作者： Ray, Anarya Niu, Wanting Sakon, Shio Ewing, Becca Creighton, Jolien D.E. Hanna, Chad Adhicary, Shomik Baral, Pratyusava Baylor, Amanda Cannon, Kipp Caudill, Sarah Cousins, Bryce Fong, Heather George, Richard N. Godwin, Patrick Harada, Reiko Huang, Yun-Jing Huxford, Rachael Joshi, Prathamesh Kapadia, Shasvath Kennington, James Kuwahara, Soichiro Li, Alvin K.Y. Magee, Ryan Meacher, Duncan Messick, Cody Morisaki, Soichiro Mukherjee, Debnandini Pace, Alex Posnansky, Cort Sachdev, Surabhi Singh, Divya Tapia, Ron Tsukada, Leo Tsutsui, Takuya Ueno, Koh Viets, Aaron Wade, Leslie Wade, Madeline Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee MilwaukeeWI53201 United States Department of Physics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States RESCEU The University of Tokyo Tokyo113-0033 Japan Department of Physics University of Massachusetts DartmouthMA02747 United States Center for Scientific Computing and Data Science Research University of Massachusetts DartmouthMA02747 United States Department of Physics University of Illinois UrbanaIL61801 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada Graduate School of Science The University of Tokyo Tokyo113-0033 Japan Center for Gravitational Physics University of Texas at Austin AustinTX78712 United States LIGO Laboratory California Institute of Technology MS 100-36 PasadenaCA91125 United States The Inter-University Centre for Astronomy and Astrophysics Post Bag 4 Ganeshkhind Pune411007 India MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba277-8582 Japan NASA Marshall Space Flight Center HuntsvilleAL35811 United States Center for Space Plasma and Aeronomic Research University of Alabama in Huntsville HuntsvilleAL35899 United States School of Physics Georgia Institute of Technology AtlantaGA30332 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Concordia University Wisconsin MequonWI53097 United States Department of Physics Hayes Hall Kenyon College GambierOH43022 United States

We develop a robust and self-consistent framework to extract and classify gravitational wave candidates from noisy data, for the purpose of assisting in real-time multi-messenger follow-ups during LIGO-Virgo-KAGRA’s fourth observing run (O4). Our formalism implements several improvements to the low latency calculation of the probability of astrophysical origin (Pastro), so as to correctly account for various factors such as the sensitivity change between observing runs, and the deviation of the recovered template waveform from the true gravitational wave signal that can strongly bias said calculation. We demonstrate the high accuracy with which our new formalism recovers and classifies gravitational wave triggers, by analyzing replay data from previous observing runs injected with simulated sources of different categories. We show that these improvements enable the correct identification of the majority of simulated sources, many of which would have otherwise been misclassified. We carry out the aforementioned analysis by implementing our formalism through the GstLAL search pipeline even though it can be used in conjunction with potentially any matched filtering pipeline. Armed with robust and self-consistent Pastro values, the GstLAL pipeline can be expected to provide accurate source classification information for assisting in multi-messenger follow-up observations to gravitational wave alerts sent out during O4. © 2023, CC BY.

关键词： Gravity waves

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Search for Light Long-Lived particles in pp Collisions at s=13 TeV Using Displaced Vertices in the ATLAS Inner Detector

引用

Physical Review Letters 2024年第16期133卷 161803页

作者： G. Aad E. Aakvaag B. Abbott S. Abdelhameed K. Abeling N. J. Abicht S. H. Abidi M. Aboelela A. Aboulhorma H. Abramowicz H. Abreu Y. Abulaiti B. S. Acharya A. Ackermann C. Adam Bourdarios L. Adamczyk S. V. Addepalli M. J. Addison J. Adelman A. Adiguzel T. Adye A. A. Affolder Y. Afik M. N. Agaras J. Agarwala A. Aggarwal C. Agheorghiesei A. Ahmad F. Ahmadov W. S. Ahmed S. Ahuja X. Ai G. Aielli A. Aikot M. Ait Tamlihat B. Aitbenchikh M. Akbiyik T. P. A. Åkesson A. V. Akimov D. Akiyama N. N. Akolkar S. Aktas K. Al Khoury G. L. Alberghi J. Albert P. Albicocco G. L. Albouy S. Alderweireldt Z. L. Alegria M. Aleksa I. N. Aleksandrov C. Alexa T. Alexopoulos F. Alfonsi M. Algren M. Alhroob B. Ali H. M. J. Ali S. Ali S. W. Alibocus M. Aliev G. Alimonti W. Alkakhi C. Allaire B. M. M. Allbrooke J. F. Allen C. A. Allendes Flores P. P. Allport A. Aloisio F. Alonso C. Alpigiani Z. M. K. Alsolami M. Alvarez Estevez A. Alvarez Fernandez M. Alves Cardoso M. G. Alviggi M. Aly Y. Amaral Coutinho A. Ambler C. Amelung M. Amerl C. G. Ames D. Amidei K. J. Amirie S. P. Amor Dos Santos K. R. Amos S. An V. Ananiev C. Anastopoulos T. Andeen J. K. Anders A. C. Anderson S. Y. Andrean A. Andreazza S. Angelidakis A. Angerami A. V. Anisenkov A. Annovi C. Antel E. Antipov M. Antonelli F. Anulli M. Aoki T. Aoki M. A. Aparo L. Aperio Bella C. Appelt A. Apyan S. J. Arbiol Val C. Arcangeletti A. T. H. Arce E. Arena J-F. Arguin S. Argyropoulos J.-H. Arling O. Arnaez H. Arnold G. Artoni H. Asada K. Asai S. Asai N. A. Asbah R. A. Ashby Pickering K. Assamagan R. Astalos K. S. V. Astrand S. Atashi R. J. Atkin M. Atkinson H. Atmani P. A. Atmasiddha K. Augsten S. Auricchio A. D. Auriol V. A. Austrup G. Avolio K. Axiotis G. Azuelos D. Babal H. Bachacou K. Bachas A. Bachiu F. Backman A. Badea T. M. Baer P. Bagnaia M. Bahmani D. Bahner K. Bai J. T. Baines L. Baines O. K. Baker E. Bakos D. Bakshi Gupta L. E. Balabram Filho V. Balakrishnan R. Balasubramanian E. M. Baldin P. Balek E. Ballabene F. Balli L. M. Baltes W. K. Balunas J. Balz I. Bamwidhi E. Banas M. Bandi CPPM Aix-Marseille Université CNRS/IN2P3 Marseille France Department for Physics and Technology University of Bergen Bergen Norway Homer L. Dodge Department of Physics and Astronomy University of Oklahoma Norman Oklahoma USA New York University Abu Dhabi Abu Dhabi United Arab Emirates II. Physikalisches Institut Georg-August-Universität Göttingen Göttingen Germany Fakultät Physik Technische Universität Dortmund Dortmund Germany Physics Department Brookhaven National Laboratory Upton New York USA Physics Department Southern Methodist University Dallas Texas USA Faculté des sciences Université Mohammed V Rabat Morocco 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 Department of Physics New York University New York New York USA INFN Gruppo Collegato di Udine Sezione di Trieste Udine Italy ICTP Trieste Italy Kirchhoff-Institut für Physik Ruprecht-Karls-Universität Heidelberg Heidelberg Germany LAPP Université Savoie Mont Blanc CNRS/IN2P3 Annecy France AGH University of Krakow Faculty of Physics and Applied Computer Science Krakow Poland Department of Physics Brandeis University Waltham Massachusetts USA School of Physics and Astronomy University of Manchester Manchester United Kingdom Department of Physics Northern Illinois University DeKalb Illinois USA Department of Physics Istanbul University Istanbul Türkiye Particle Physics Department Rutherford Appleton Laboratory Didcot United Kingdom Santa Cruz Institute for Particle Physics University of California Santa Cruz Santa Cruz California USA Enrico Fermi Institute University of Chicago Chicago Illinois USA Institut de Física d’Altes Energies (IFAE) Barcelona Institute of Science and Technology Barcelona Spain INFN Sezione di Pavia Italy Dipartimento di Fisica Università di Pavia Pavia Italy Institut für Physik Universität Mainz Mainz Germany Department o

A search for long-lived particles (LLPs) using 140 fb−1 of pp collision data with s=13 TeV recorded by the ATLAS experiment at the LHC is presented. The search targets LLPs with masses between 5 and 55 GeV that decay hadronically in the ATLAS inner detector. Benchmark models with LLP pair production from exotic decays of the Higgs boson and models featuring long-lived axionlike particles (ALPs) are considered. No significant excess above the expected background is observed. Upper limits are placed on the branching ratio of the Higgs boson to pairs of LLPs, the cross section for ALPs produced in association with a vector boson, and, for the first time, on the branching ratio of the top quark to an ALP and a u/c quark.

关键词： Axion-like particles Higgs bosons Top quark Hadron colliders

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