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Search for a Structure in the Bs0π± Invariant Mass Spectrum with the ATLAS Experiment

Physical Review Letters 2018年第20期120卷 202007-202007页

作者： M. Aaboud G. Aad B. Abbott O. Abdinov B. Abeloos S. H. Abidi O. S. AbouZeid N. L. Abraham H. Abramowicz H. Abreu Y. Abulaiti B. S. Acharya S. Adachi L. Adamczyk J. Adelman M. Adersberger T. Adye A. A. Affolder Y. Afik C. Agheorghiesei J. A. Aguilar-Saavedra S. P. Ahlen F. Ahmadov G. Aielli S. Akatsuka H. Akerstedt T. P. A. Åkesson E. Akilli A. V. Akimov G. L. Alberghi J. Albert P. Albicocco M. J. Alconada Verzini S. Alderweireldt M. Aleksa I. N. Aleksandrov C. Alexa G. Alexander T. Alexopoulos M. Alhroob B. Ali M. Aliev G. Alimonti J. Alison S. P. Alkire B. M. M. Allbrooke B. W. Allen P. P. Allport A. Aloisio A. Alonso F. Alonso C. Alpigiani A. A. Alshehri M. I. Alstaty B. Alvarez Gonzalez D. Álvarez Piqueras M. G. Alviggi B. T. Amadio Y. Amaral Coutinho C. Amelung D. Amidei S. P. Amor Dos Santos S. Amoroso C. Anastopoulos L. S. Ancu N. Andari T. Andeen C. F. Anders J. K. Anders K. J. Anderson A. Andreazza V. Andrei S. Angelidakis I. Angelozzi A. Angerami A. V. Anisenkov N. Anjos A. Annovi C. Antel M. Antonelli A. Antonov D. J. Antrim F. Anulli M. Aoki L. Aperio Bella G. Arabidze Y. Arai J. P. Araque V. Araujo Ferraz A. T. H. Arce R. E. Ardell F. A. Arduh J-F. Arguin S. Argyropoulos M. Arik A. J. Armbruster L. J. Armitage O. Arnaez H. Arnold M. Arratia O. Arslan A. Artamonov G. Artoni S. Artz S. Asai N. Asbah A. Ashkenazi L. Asquith K. Assamagan R. Astalos M. Atkinson N. B. Atlay K. Augsten G. Avolio B. Axen M. K. Ayoub G. Azuelos A. E. Baas M. J. Baca H. Bachacou K. Bachas M. Backes P. Bagnaia M. Bahmani H. Bahrasemani J. T. Baines M. Bajic O. K. Baker P. J. Bakker D. Bakshi Gupta E. M. Baldin P. Balek F. Balli W. K. Balunas E. Banas A. Bandyopadhyay Sw. Banerjee A. A. E. Bannoura L. Barak E. L. Barberio D. Barberis M. Barbero T. Barillari M-S Barisits J. T. Barkeloo T. Barklow N. Barlow S. L. Barnes B. M. Barnett R. M. Barnett Z. Barnovska-Blenessy A. Baroncelli G. Barone A. J. Barr L. Barranco Navarro F. Barreiro J. Barreiro Guimarães da Costa R. Bartoldus A. E. Barton P. Bartos A. Basalaev A. Bassalat R. L. B 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 Oklahoma USA 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 Ontario Canada Santa Cruz Institute for Particle Physics University of California Santa Cruz Santa Cruz California USA 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 Department of Physics Stockholm University Sweden The Oskar Klein Centre Stockholm Sweden INFN Gruppo Collegato di Udine Sezione di Trieste Udine Italy ICTP Trieste Italy 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 Illinois USA Fakultät für Physik Ludwig-Maximilians-Universität München München Germany Particle Physics Department Rutherford Appleton Laboratory Didcot United Kingdom 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 Massachusetts USA Joint Institute for Nuclear Research JINR Dubna Dubna Russia INFN Sezione di Roma Tor Vergata Italy Dipartimento di Fisica Università di Roma Tor Vergata Roma Italy Faculty of Science Kyoto University Kyoto Japan Fysiska institutionen Lunds universit

A search for the narrow structure, X(5568), reported by the D0 Collaboration in the decay sequence X→Bs0π±, Bs0→J/ψϕ, is presented. The analysis is based on a data sample recorded with the ATLAS detector at the LHC corresponding to 4.9 fb−1 of pp collisions at 7 TeV and 19.5 fb−1 at 8 TeV. No significant signal was found. Upper limits on the number of signal events, with properties corresponding to those reported by D0, and on the X production rate relative to Bs0 mesons, ρX, were determined at 95% confidence level. The results are N(X)<382 and ρX<0.015 for Bs0 mesons with transverse momenta above 10 GeV, and N(X)<356 and ρX<0.016 for transverse momenta above 15 GeV. Limits are also set for potential Bs0π± resonances in the mass range 5550 to 5700 MeV.

关键词： Exotic mesons Hadron colliders

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STUDIES ON STRUCTURAL AND MECHANICAL PROPERTIES UNDER ISOSTATIC COMPRESSION WITH LARGE-SCALE DISCRETE ELEMENT SIMULATIONS

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Acta Mechanica Solida Sinica 2014年第2期27卷 129-136页

作者： Jianguo Liu Qicheng Sun Feng Jin Qingkai Liu State Key Laboratory of Hydroscience and Engineering Tsinghua University High Performance Computing Center Institute of Applied Physics and Computational Mathematics

Granular systems undergo a jamming transition at point J simply by increasing the packing fraction. A large-scale parallel discrete element code （THDEM： TsingHua Discrete Element Method） was used to obtain a satisfying statistical description of the structural and me- chanical properties near point J. The isostatic compressions of 100,000 polydispersed frictionless particles were simulated on high performance computers to clearly observe the sophisticated con- figurations of force chains. The first peak of the pair correlation function, coordination number, spatial distribution of the packing fraction, and stress were calculated to analyze their variations with increasing packing fraction. The critical packing fraction at point J is determined to be 0.62. The incremental stress and coordination number from point J scale well with the power law, and coincide with previous theoretical predications. The distribution of the packing frac- tion is a normal distribution around the average value. The standard deviation decreases with increasing packing fraction, indicating the system is more uniform with a denser packing.

关键词： granular matter jamming transition force chains parallel computing

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Gravitational wave astronomy: the current status

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science China(Physics,Mechanics & Astronomy) 2015年第12期58卷 3-43页

作者： BLAIR David JU Li ZHAO ChunNong WEN LinQing CHU Qi FANG Qi CAI RongGen GAO JiangRui LIN XueChun LIU Dong WU Ling-An ZHU ZongHong REITZE David H. ARAI Koji ZHANG Fan FLAMINIO Raffaele ZHU XingJiang HOBBS George MANCHESTER Richard N. SHANNON Ryan M. BACCIGALUPI Carlo GAO Wei XU Peng BIAN Xing CAO ZhouJian CHANG ZiJing DONG Peng GONG XueFei HUANG ShuangLin JU Peng LUO ZiRen QIANG Li'E TANG WenLin WAN XiaoYun WANG Yue XU ShengNian ZANG YunLong ZHANG HaiPeng LAU Yun-Kau NI Wei-Tou School of Physics The University of Western Australia State Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences The School of Physics & Electronic Engineering Shanxi University Laboratory of All-Solid-State Light Sources Institute of Semiconductors Chinese Academy of Science State Key Laboratroy of Modern Optical Instrumentation Department of Optical Engineering Zhejiang University Laboratory of Optical Physics Institute of Physics Chinese Academy of Sciences Gravitational Wave and Cosmology Laboratory Department of Astronomy Beijing Normal University LIGO Laboratory California Institute of Technology Department of Physics University of Florida Department of Physics West Virginia University National Astronomical Observatory of Japan CSIRO Astronomy and Space Science International Centre for Radio Astronomy Research Curtin University SISSA Astrophysics Sector Institute of Applied Mathematics Academy of Mathematics and Systems Science Chinese Academy of Sciences University of Chinese Academy of Sciences Morningside Center of Mathematics Chinese Academy of Sciences State Key Laboratory of Scientific and Engineering Computing Academy of Mathematics and Systems ScienceChinese Academy of Sciences Department of Mathematics Henan University Department of Mathematics Capital Normal University Department of Geophysics College of the Geology Engineering and Geomatics Chang'an University QUEST Centre of Quantum Engineering and Space-Time Research Leibniz Universitt Hannover Max-Planck-Institut für Gravitationsphysik(Albert Einstein Institut) Aerospace Flight Dynamics Laboratory Beijing Aerospace Control Center Qian Xuesen Laboratory of Launch Vehicle Technology Center for Gravitation and Cosmology Department of Physics Tsing Hua University

In the centenary year of Einstein's General Theory of Relativity, this paper reviews the current status of gravitational wave astronomy across a spectrum which stretches from attohertz to kilohertz frequencies. Sect. 1 of this paper reviews the historical development of gravitational wave astronomy from Einstein's first prediction to our current understanding the spectrum. It is shown that detection of signals in the audio frequency spectrum can be expected very soon, and that a north-south pair of next generation detectors would provide large scientific benefits. Sect. 2 reviews the theory of gravitational waves and the principles of detection using laser interferometry. The state of the art Advanced LIGO detectors are then described. These detectors have a high chance of detecting the first events in the near future. Sect. 3 reviews the KAGRA detector currently under development in Japan,which will be the first laser interferometer detector to use cryogenic test masses. Sect. 4 of this paper reviews gravitational wave detection in the nanohertz frequency band using the technique of pulsar timing. Sect. 5 reviews the status of gravitational wave detection in the attohertz frequency band, detectable in the polarisation of the cosmic microwave background, and discusses the prospects for detection of primordial waves from the big bang. The techniques described in sects. 1–5 have already placed significant limits on the strength of gravitational wave sources. Sects. 6 and 7 review ambitious plans for future space based gravitational wave detectors in the millihertz frequency band. Sect. 6 presents a roadmap for development of space based gravitational wave detectors by China while sect. 7 discusses a key enabling technology for space interferometry known as time delay interferometry.

关键词： gravitational waves ground based detectors pulsar timing spaced based detectors CMB

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Studying the solar system with the International Pulsar Timing Array

arXiv

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arXiv 2018年

作者： Caballero, R.N. Guo, Y.J. Lee, K.J. Lazarus, P. Champion, D.J. Desvignes, G. Kramer, M. Plant, K. Arzoumanian, Z. Bailes, M. Bassa, C.G. Bhat, N.D.R. Brazier, A. Burgay, M. Burke-Spolaor, S. Chamberlin, S.J. Chatterjee, S. Cognard, I. Cordes, J.M. Dai, S. Demorest, P. Dolch, T. Ferdman, R.D. Fonseca, E. Gair, J.R. Garver-Daniels, N. Gentile, P. Gonzalez, M.E. Graikou, E. Guillemot, L. Hobbs, G. Janssen, G.H. Karuppusamy, R. Keith, M.J. Kerr, M. Lam, M.T. Lasky, P.D. Lazio, T.J.W. Levin, L. Liu, K. Lommen, A.N. Lorimer, D.R. Lynch, R.S. Madison, D.R. Manchester, R.N. McKee, J.W. McLaughlin, M.A. McWilliams, S.T. Mingarelli, C.M.F. Nice, D.J. Oslowski, S. Palliyaguru, N.T. PennucciT.T. Perera, B.B.P. Perrodin, D. Possenti, A. Ransom, S.M. Reardon, D.J. Sanidas, S.A. Sesana, A. Shaifullah, G. Shannon, R.M. Siemens, X. Simon, J. Spiewak, R. Stairs, I. Stappers, B. Stinebring, D.R. Stovall, K. Swiggum, J.K. Taylor, S.R. Theureau, G. Tiburzi, C. Toomey, L. Van Haasteren, R. Van Straten, W. Verbiest, J.P.W. Wang, J.B. Zhu, X.J. Zhu, W.W. Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester ManchesterM13 9PL United Kingdom Cahill Center for Astrophysics California Institute of Technology MC 249-17 1200 E. California Boulevard PasadenaCA91125 United States X-Ray Astrophysics Laboratory NASA Goddard Space Flight Center Code 662 GreenbeltMD20771 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia ASTRON Netherlands Institute for Radio Astronomy Postbus 2 Dwingeloo7990 AA Netherlands International Centre for Radio Astronomy Research Curtin University BentleyWA6102 Australia Cornell Center for Advanced Computing Cornell University IthacaNY14853 United States Cornell Center for Astrophysics and Planetary Science Cornell University IthacaNY14853 United States I-09047 Italy Department of Physics and Astronomy West Virginia University MorgantownWV26506 United States Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building MorgantownWV26505 United States Institute for Gravitation and the Cosmos Department of Physics Pennsylvania State University University ParkPA16802 United States Astronomy Department Cornell University IthacaNY14853 United States Laboratoire de Physique et Chimie de l'Environnement et de l'Espace LPC2E UMR7328 Université d'Orléans CNRS OrléansF-45071 France Station de Radioastronomie de Nançay Observatoire de Paris PSL University CNRS Université d'Orléans Nançay18330 France CSIRO Astronomy and Space Science Australia Telescope National Facility Box 76 EppingNSW1710 Australia National Radio Astronomy Observatory PO Box O SocorroNM87801 United States Department of Physics Hillsdale College 33 E. College Street HillsdaleMI

Pulsar-timing analyses are sensitive to errors in the solar-system ephemerides (SSEs) that timing models utilise to estimate the location of the solar-system barycentre, the quasi-inertial reference frame to which all recorded pulse times-of-arrival are referred. Any error in the SSE will affect all pulsars, therefore pulsar timing arrays (PTAs) are a suitable tool to search for such errors and impose independent constraints on relevant physical parameters. We employ the first data release of the International Pulsar Timing Array to constrain the masses of the planet-moons systems and to search for possible unmodelled objects (UMOs) in the solar system. We employ ten SSEs from two independent research groups, derive and compare mass constraints of planetary systems, and derive the first PTA mass constraints on asteroid-belt objects. Constraints on planetary-system masses have been improved by factors of up to 20 from the previous relevant study using the same assumptions, with the mass of the Jovian system measured at 9.5479189(3)×10-4Mo. The mass of the dwarf planet Ceres is measured at 4.7(4)×10-10Mo. We also present the first sensitivity curves using real data that place generic limits on the masses of UMOs, which can also be used as upper limits on the mass of putative exotic objects. For example, upper limits on darkmatter clumps are comparable to published limits using independent methods. While the constraints on planetary masses derived with all employed SSEs are consistent, we note and discuss differences in the associated timing residuals and UMO sensitivity curves. Copyright © 2018, The Authors. All rights reserved.

关键词： Pulsars

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A preliminary study of level 1A data processing of a low-low satellite to satellite tracking mission

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Geodesy and Geodynamics 2015年第5期6卷 333-343页

作者： Xu Peng Qiang Li'e Bian Xing Dong Peng Ju Peng Gao Wei Gong Xuefei Luo Ziren Shao Mingxue Tang Werilin Wan Xiaoyun Lau Yun-Kau Institute of Applied Mathematics Academy of Mathematics and Systems ScienceChinese Academy of Sciences Morningside Center of Mathematics Chinese Academy of Sciences State Key Laboratory of Geodesy and Earth's Dynamics Institute of Geodesy and Geo-physicsChinese Academy of Sciences Department of Geophysics College o/the Geology Engineering and GeomaticsChang 'an University University of Chinese Academy of Sciences Max-Planck-Institute for Grauitational Physics(Albert Einstein Institute) Aerospace Flight Dynamics Laboratory Beijing Aerospace Control Center Qian Xuesen Laboratory of Launch Vehicle Technology State Key Laboratory of Scientific and Engineering Computing Academy of Mathematics and Systems ScienceChinese Academy of Sciences

With the Gravity Recovery and Climate Experiment {GRACE） mission as the prime example, an overview is given on the management and processing of Level IA data of a low-low satellite to satellite tracking mission. To illustrate the underlying principle and algorithm, a detailed study is made on the K-band ranging （KBR） assembly, which includes the measurement principles, modeling of noises, the generation of Level 1A data from that of Level 0 as well as Level IA to Level IB data processing.

关键词： Data processingDual-one-way ranging （DOWR）Gravity recovery and climateexperiment （GRACE）K-band ranging （KBR）Satellite to satellite tracking （SST）Noise analysisSatellite gravityUltra stable oscillator （USO）

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Interweaving pfasst and parallel multigrid

Interweaving pfasst and parallel multigrid

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作者： Minion, M.L. Speck, R. Bolten, M. Emmett, M. Ruprecht, D. Center for Computational Sciences and Engineering Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Jülich Supercomputing Centre Forschungszentrum Jülich Germany Institute of Computational Science Università della Svizzera italiana Lugano Switzerland Department of Mathematics Bergische Universität Wuppertal Germany

The parallel full approximation scheme in space and time (PFASST) introduced by Emmett and Minion in 2012 is an iterative strategy for the temporal parallelization of ODEs and discretized PDEs. As the name suggests, PFASST is similar in spirit to a space-time full approximation scheme multigrid method performed over multiple time steps in parallel. However, since the original focus of PFASST was on the performance of the method in terms of time parallelism, the solution of any spatial system arising from the use of implicit or semi-implicit temporal methods within PFASST have simply been assumed to be solved to some desired accuracy completely at each substep and each iteration by some unspecified procedure. It hence is natural to investigate how iterative solvers in the spatial dimensions can be interwoven with the PFASST iterations and whether this strategy leads to a more efficient overall approach. This paper presents an initial investigation on the relative performance of different strategies for coupling PFASST iterations with multigrid methods for the implicit treatment of diffusion terms in PDEs. In particular, we compare full accuracy multigrid solves at each substep with a small fixed number of multigrid V-cycles. This reduces the cost of each PFASST iteration at the possible expense of a corresponding increase in the number of PFASST iterations needed for convergence. Parallel efficiency of the resulting methods is explored through numerical examples. © 2015 Society for Industrial and Applied mathematics.

关键词： Numerical methods

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Erratum to: Search for heavy resonances decaying into a W or Z boson and a Higgs boson in final states with leptons and b-jets in 36 fb−1 of TeV pp collisions with the ATLAS detector

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Journal of High Energy Physics 2018年第11期2018卷 1-18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. Barnovs 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

One correction is noted for the paper. The exclusion limits for the gluon-gluon fusion production of an A boson reported in the conclusions did not correspond to the exclusion plots shown in figure 6a.

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KROSS-SAMI: A direct IFS comparison of the tully-fisher relation across 8 Gyr since z ≈ 1

arXiv

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arXiv 2018年

作者： Tiley, A.L. Bureau, M. Cortese, L. Harrison, C.M. Johnson, H.L. Stott, J.P. Swinbank, A.M. Smail, I. Sobral, D. Bunker, A.J. Glazebrook, K. Bower, R.G. Obreschkow, D. Bryant, J.J. Jarvis, M.J. Bland-Hawthorn, J. Magdis, G. Medling, A.M. Sweet, S.M. Tonini, C. Turner, O.J. Sharples, R.M. Croom, S.M. Goodwin, M. Konstantopoulos, I.S. Lorente, N.P.F. Lawrence, J.S. Mould, J. Owers, M.S. Richards, S.N. Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Sub-dept. of Astrophysics Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom International Centre for Radio Astronomy Research University of Western Australia 35 Stirling Hw CrawleyWA6009 Australia European Southern Observatory Karl-Schwarzchild-Str. 2 Garching b. München85748 Germany Department of Physics Lancaster University LancasterLA1 4YB United Kingdom Affiliate Member Kavli Institute for the Physics and Mathematics of the Universe 5-1-5 Kashiwanoha Kashiwa277-8583 Japan Centre for Astrophysics and Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia Institute for Computational Cosmology Durham University South Road DurhamDH1 3LE United Kingdom School of Physics University of Sydney NSW2006 Australia Australian Astronomical Optics AAO-USydney School of Physics University of Sydney NSW2006 Australia Department of Physics University of the Western Cape Bellville7535 South Africa School of Physics University of Sydney NSW2006 Australia Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Mariesvej 30 CopenhagenDK-2100 Denmark Institute for Astronomy Astrophysics Space Applications and Remote Sensing National Observatory of Athens AthensGR-15236 Greece Research School for Astronomy & Astrophysics Australian National University CanberraACT2611 Australia Cahill Center for Astronomy and Astrophysics California Institute of Technology MS 249-17 PasadenaCA91125 United States Melbourne University School of Physics Parkville3010 Australia Scottish Universities Physics Alliance Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Centre for Advanced Instrumentation Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Aus

We construct Tully-Fisher relations (TFRs), from large samples of galaxies with spatially-resolved Hα emission maps from the K-band Multi-Object Spectrograph (KMOS) Redshift One Spectroscopic Survey (KROSS) at z ≈ 1. We compare these to data from the Sydney-Australian-Astronomical-Observatory Multi-object Integral-Field Spectrograph (SAMI) Galaxy Survey at z ≈ 0. We stringently match the data quality of the latter to the former, and apply identical analysis methods and sub-sample selection criteria to both to conduct a direct comparison of the absolute K-band magnitude and stellar mass TFRs at z ≈ 1 and z ≈ 0. We find that matching the quality of the SAMI data to that of KROSS results in TFRs that differ significantly in slope, zero-point and (sometimes) scatter in comparison to the corresponding original SAMI relations. These differences are in every case as large or larger than the differences between the KROSS z ≈ 1 and matched SAMI z ≈ 0 relations. Accounting for these differences, we compare the TFRs at z ≈ 1 and z ≈ 0. For disk-like, star-forming galaxies we find no significant difference in the TFR zero-points between the two epochs. This suggests the growth of stellar mass and dark matter in these types of galaxies is intimately linked over this ≈ 8 Gyr period. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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M-Statistic for Kernel Change-Point Detection 15

M-Statistic for Kernel Change-Point Detection

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Annual Conference on Neural Information Processing Systems

作者： Shuang Li Yao Xie Hanjun Dai Le Song H. Milton Stewart School of Industrial and Systems Engineering Georgian Institute of Technology Computational Science and Engineering College of Computing Georgia Institute of Technology

ISBN: (纸本)9781510825024

Detecting the emergence of an abrupt change-point is a classic problem in statistics and machine learning. Kernel-based nonparametric statistics have been proposed for this task which make fewer assumptions on the distributions than traditional parametric approach. However, none of the existing kernel statistics has provided a computationally efficient way to characterize the extremal behavior of the statistic. Such characterization is crucial for setting the detection threshold, to control the significance level in the offline case as well as the average run length in the online case. In this paper we propose two related computationally efficient M-statistics for kernel-based change-point detection when the amount of background data is large. A novel theoretical result of the paper is the characterization of the tail probability of these statistics using a new technique based on change-of-measure. Such characterization provides us accurate detection thresholds for both offline and online cases in computationally efficient manner, without the need to resort to the more expensive simulations such as bootstrapping. We show that our methods perform well in both synthetic and real world data.

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Search for top squarks decaying to tau sleptons in pp collisions at s=13 TeV with the ATLAS detector

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Physical Review D 2018年第3期98卷 032008-032008页

作者： M. Aaboud G. Aad B. Abbott O. Abdinov B. Abeloos S. H. Abidi O. S. Abouzeid N. L. Abraham H. Abramowicz H. Abreu Y. Abulaiti B. S. Acharya S. Adachi L. Adamczyk J. Adelman M. Adersberger T. Adye A. A. Affolder Y. Afik C. Agheorghiesei J. A. Aguilar-Saavedra F. Ahmadov G. Aielli S. Akatsuka T. P. A. Åkesson E. Akilli A. V. Akimov G. L. Alberghi J. Albert P. Albicocco M. J. Alconada Verzini S. Alderweireldt M. Aleksa I. N. Aleksandrov C. Alexa G. Alexander T. Alexopoulos M. Alhroob B. Ali M. Aliev G. Alimonti J. Alison S. P. Alkire C. Allaire B. M. M. Allbrooke B. W. Allen P. P. Allport A. Aloisio A. Alonso F. Alonso C. Alpigiani A. A. Alshehri M. I. Alstaty B. Alvarez Gonzalez D. Álvarez Piqueras M. G. Alviggi B. T. Amadio Y. Amaral Coutinho L. Ambroz C. Amelung D. Amidei S. P. Amor Dos Santos S. Amoroso C. Anastopoulos L. S. Ancu N. Andari T. Andeen C. F. Anders J. K. Anders K. J. Anderson A. Andreazza V. Andrei S. Angelidakis I. Angelozzi A. Angerami A. V. Anisenkov A. Annovi C. Antel M. T. Anthony M. Antonelli A. Antonov D. J. A. Antrim F. Anulli M. Aoki L. Aperio Bella G. Arabidze Y. Arai J. P. Araque V. Araujo Ferraz R. Araujo Pereira A. T. H. Arce R. E. Ardell F. A. Arduh J-F. Arguin S. Argyropoulos A. J. Armbruster L. J. Armitage O. Arnaez H. Arnold M. Arratia O. Arslan A. Artamonov G. Artoni S. Artz S. Asai N. Asbah A. Ashkenazi L. Asquith K. Assamagan R. Astalos R. J. Atkin M. Atkinson N. B. Atlay K. Augsten G. Avolio R. Avramidou B. Axen M. K. Ayoub G. Azuelos A. E. Baas M. J. Baca H. Bachacou K. Bachas M. Backes P. Bagnaia M. Bahmani H. Bahrasemani J. T. Baines M. Bajic O. K. Baker P. J. Bakker D. Bakshi Gupta E. M. Baldin P. Balek F. Balli W. K. Balunas E. Banas A. Bandyopadhyay Sw. Banerjee A. A. E. Bannoura L. Barak W. M. Barbe E. L. Barberio D. Barberis M. Barbero T. Barillari M-S Barisits J. Barkeloo T. Barklow N. Barlow R. Barnea S. L. Barnes B. M. Barnett R. M. Barnett Z. Barnovska-Blenessy A. Baroncelli G. Barone A. J. Barr L. Barranco Navarro F. Barreiro J. Barreiro Guimarães da Costa R. Bartol Faculté des Sciences Université Mohamed Premier and LPTPM Oujda CPPM Aix-Marseille Université and CNRS/IN2P3 Marseille France Homer L. Dodge Department of Physics and Astronomy University of Oklahoma Norman Oklahoma USA Institute of Physics Azerbaijan Academy of Sciences Baku Azerbaijan LAL Université Paris-Sud CNRS/IN2P3 Université Paris-Saclay Orsay France Department of Physics University of Toronto Toronto Ontario Canada Santa Cruz Institute for Particle Physics University of California Santa Cruz Santa Cruz California USA 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 High Energy Physics Division Argonne National Laboratory Argonne Illinois USA INFN Gruppo Collegato di Udine Sezione di Trieste Udine ICTP Trieste 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 Department of Physics Northern Illinois University DeKalb Illinois USA Fakultät für Physik Ludwig-Maximilians-Universität München München Germany Particle Physics Department Rutherford Appleton Laboratory Didcot United Kingdom Department of Physics Alexandru Ioan Cuza University of Iasi Iasi Departamento de Fisica Teorica y del Cosmos Universidad de Granada Granada (Spain) Laboratório de Instrumentação e Física Experimental de Partículas - LIP Lisboa Joint Institute for Nuclear Research JINR Dubna Dubna Russia INFN Sezione di Roma Tor Vergata Roma Italy Dipartimento di Fisica Università di Roma Tor Vergata Roma Italy Faculty of Science Kyoto University Kyoto Japan Fysiska institutionen Lunds universitet Lund Sweden Departement de Physique Nucléaire et Corpusculaire Université de Genève Geneva Switzerland P.N. Lebede

A search for direct pair production of top squarks in final states with two tau leptons, b-jets, and missing transverse momentum is presented. The analysis is based on proton-proton collision data at s=13 TeV corresponding to an integrated luminosity of 36.1 fb−1 recorded with the ATLAS detector at the Large Hadron Collider in 2015 and 2016. Two exclusive channels with either two hadronically decaying tau leptons or one hadronically and one leptonically decaying tau lepton are considered. No significant deviation from the Standard Model predictions is observed in the data. The analysis results are interpreted in terms of model-independent limits and used to derive exclusion limits on the masses of the top squark t˜1 and the tau slepton τ˜1 in a simplified model of supersymmetry with a nearly massless gravitino. In this model, masses up to m(t˜1)=1.16 TeV and m(τ˜1)=1.00 TeV are excluded at 95% confidence level.

关键词： Supersymmetric models Superpartners Tau leptons Top quark Particle data analysis

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