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Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO

Astrophysical Journal, Supplement Series 2023年第2期267卷 29-29页

作者： Abbott, R. Abe, H. Acernese, F. Ackley, K. Adhicary, S. Adhikari, N. Adhikari, R.X. Adkins, V.K. Adya, V.B. Affeldt, C. Agarwal, D. Agathos, M. Aguiar, O.D. Aiello, L. Ain, A. Ajith, P. Akutsu, T. Albanesi, S. Alfaidi, R.A. Al-Jodah, A. Alléné, C. Allocca, A. Almualla, M. Altin, P.A. Amato, A. Amez-Droz, L. Amorosi, A. Anand, S. Ananyeva, A. Andersen, R. Anderson, S.B. Anderson, W.G. Andia, M. Ando, M. Andrade, T. Andres, N. Andrés-Carcasona, M. Andrić, T. Ansoldi, S. Antelis, J.M. Antier, S. Aoumi, M. Apostolatos, T. Appavuravther, E.Z. Appert, S. Apple, S.K. Arai, K. Araya, A. Araya, M.C. Areeda, J.S. Arène, M. Aritomi, N. Arnaud, N. Arogeti, M. Aronson, S.M. Arun, K.G. Asada, H. Ashton, G. Aso, Y. Assiduo, M. Assis de Souza Melo, S. Aston, S.M. Astone, P. Aubin, F. AultONeal, K. Babak, S. Badalyan, A. Badaracco, F. Badger, C. Bae, S. Bagnasco, S. Bai, Y. Baier, J.G. Baiotti, L. Baird, J. Bajpai, R. Baka, T. Ball, M. Ballardin, G. Ballmer, S.W. Baltus, G. Banagiri, S. Banerjee, B. Bankar, D. Baral, P. Barayoga, J.C. Barber, J. Barish, B.C. Barker, D. Barneo, P. Barone, F. Barr, B. Barsotti, L. Barsuglia, M. Barta, D. Barthelmy, S.D. Barton, M.A. Bartos, I. Basak, S. Basalaev, A. Bassiri, R. Basti, A. Bawaj, M. Bayley, J.C. Baylor, A.C. Bazzan, M. Bécsy, B. Bedakihale, V.M. Beirnaert, F. Bejger, M. Bell, A.S. Benedetto, V. Beniwal, D. Benoit, W. Bentley, J.D. Ben Yaala, M. Bera, S. Berbel, M. Bergamin, F. Berger, B.K. Bernuzzi, S. Beroiz, M. Berry, C.P.L. Bersanetti, D. Bertolini, A. Betzwieser, J. Beveridge, D. Bevins, N. Bhandare, R. Bhandari, A.V. Bhardwaj, U. Bhatt, R. Bhattacharjee, D. Bhaumik, S. Bianchi, A. Bilenko, I.A. Bilicki, M. Billingsley, G. Bini, S. Birnholtz, O. Biscans, S. Bischi, M. Biscoveanu, S. Bisht, A. Biswas, B. Bitossi, M. Bizouard, M.-A. Blackburn, J.K. Blair, C.D. Blair, D.G. Blair, R.M. Bobba, F. Bode, N. Boër, M. Bogaert, G. Boileau, G. Boldrini, M. Bolingbroke, G.N. Bonavena, L.D. Bondarescu, R. Bondu, F. Bonilla, E. Bonilla, G.S. Bonnand, R. Booker, P. Bork, R. Boschi, V. Bose, N. LIGO Laboratory California Institute of Technology Pasadena 91125 CA United States Graduate School of Science Tokyo Institute of Technology 2-12-1 Ookayama Meguro-ku Tokyo 152-8551 Japan Dipartimento di Farmacia Università di Salerno Salerno Fisciano I-84084 Italy INFN Sezione di Napoli Napoli I-80126 Italy OzGrav School of Physics & Astronomy Monash University Clayton 3800 VIC Australia The Pennsylvania State University University Park 16802 PA United States University of Wisconsin-Milwaukee Milwaukee 53201 WI United States Louisiana State University Baton Rouge 70803 LA United States OzGrav Australian National University Canberra 0200 ACT Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) Hannover D-30167 Germany Leibniz Universität Hannover Hannover D-30167 Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Instituto Nacional de Pesquisas Espaciais São Paulo São José dos Campos 12227-010 Brazil Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa Pisa I-56127 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 Torino I-10125 Italy INFN Sezione di Torino Torino I-10125 Italy SUPA University of Glasgow Glasgow G12 8QQ United Kingdom OzGrav University of Western Australia Crawley 6009 WA Australia Univ. Savoie Mont Blanc CNRS Laboratoire d'Annecy de Physique des Particules - IN2P3 Annecy F-74000 France Università di Napoli “Federico II” Napoli I-80126 Italy University of Minnesota Minneapolis 55455 MN United States M

The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://***. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages. © 2023. The Author(s). Published by the American Astronomical Society.

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Multiwavelength variability and correlation studies of Mrk 421 during historically low X-ray and γ-ray activity in 2015–2016

arXiv

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arXiv 2020年

作者： Acciari, V.A. Ansoldi, S. Antonelli, L.A. Asano, K. Babić, A. Banerjee, Biswajit Baquero, A. Barres De Almeida, U. Barrio, J.A. Becerra González, J. Bednarek, W. Bellizzi, L. Bernardini, E. Bernardos, M. Berti, A. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Blanch, O. Bonnoli, G. Bošnjak, Ž. Busetto, G. Carosi, R. Ceribella, G. Cerruti, M. Chai, Y. Chilingarian, A. Cikota, S. Colak, S.M. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D’Amico, G. D’Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Delfino, M. Delgado, J. Delgado Mendez, C. Depaoli, D. Di Girolamo, T. Di Pierro, F. Di Venere, L. Do Souto Espiñeira, E. Dominis Prester, D. Donini, A. Doro, M. Fallah Ramazani, V. Fattorini, A. Ferrara, G. Foffano, L. Fonseca, M.V. Font, L. Fruck, C. Fukami, S. García López, R.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, J.G. Green, D. Hadasch, D. Hahn, A. Heckmann, L. Herrera, J. Hoang, J. Hrupec, D. Hütten, M. Inada, T. Inoue, S. Ishio, K. Iwamura, Y. Jormanainen, J. Jouvin, L. Kajiwara, Y. Karjalainen, M. Kerszberg, D. Kobayashi, Y. Kubo, H. Kushida, J. Lamastra, A. Lelas, D. Leone, F. Lindfors, E. Lombardi, S. Longo, F. López, M. López-Coto, R. López-Oramas, A. Loporchio, S. Machado De Oliveira Fraga, B. Maggio, C. Majumdar, P. Makariev, M. Mallamaci, M. Maneva, G. Manganaro, M. Maraschi, L. Mariotti, M. Martínez, M. Mazin, D. Mender, S. Mićanović, S. Miceli, D. Miener, T. Minev, M. Miranda, J.M. Mirzoyan, R. Molina, E. Moralejo, A. Morcuende, D. Moreno, V. Moretti, E. Munar-Adrover, P. Neustroev, V. Nigro, C. Nilsson, K. Ninci, D. Nishijima, K. Noda, K. Nozaki, S. Ohtani, Y. Oka, T. Otero-Santos, J. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J.M. Pavletić, L. Peñil, P. Perennes, C. Persic, M. Prada Moroni, P.G. Prandini, E. Priyadarshi, C. Puljak, I. Inst. de Astrofísica de Canarias La LagunaE-38200 Spain Universidad de La Laguna Dpto. Astrofísica Tenerife La LagunaE-38206 Spain Università di Udine INFN Trieste UdineI-33100 Italy RomeI-00136 Italy Japanese MAGIC Consortium ICRR The University of Tokyo Chiba277-8582 Japan Department of Physics Kyoto University Kyoto606-8502 Japan Tokai University Kanagawa259-1292 Japan Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan Konan University Hyogo658-8501 Japan RIKEN Saitama351-0198 Japan Technische Universität Dortmund DortmundD-44221 Germany Croatian Consortium: University of Rijeka Department of Physics Rijeka51000 Croatia University of Split - FESB Split21000 Croatia University of Zagreb - FER Zagreb10000 Croatia University of Osijek Osijek31000 Croatia Rudjer Boskovic Institute Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Università di Siena and INFN Pisa SienaI-53100 Italy ZeuthenD-15738 Germany Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Frascati Roma00044 Italy Max-Planck-Institut für Physik MünchenD-80805 Germany Bellaterra BarcelonaE-08193 Spain Università di Padova INFN PadovaI-35131 Italy Università di Pisa INFN Pisa PisaI-56126 Italy Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain The Armenian Consortium: ICRANet-Armenia at NAS RA A. Alikhanyan National Laboratory Universität Würzburg WürzburgD-97074 Germany University of Turku TurkuFI-20014 Finland Astronomy Research Unit University of Oulu OuluFI-90014 Finland Departament de Física CERES-IEEC Universitat Autònoma de Barcelona Bellaterra E-08193 Spain Saha Institute of Nuclear Physics HBNI 1/AF Bi

We report a characterization of the multi-band flux variability and correlations of the nearby (z=0.031) blazar Markarian 421 (Mrk 421) using data from Metsähovi, Swift, Fermi-LAT, MAGIC, FACT and other collaborations and instruments from November 2014 till June 2016. Mrk 421 did not show any prominent flaring activity, but exhibited periods of historically low activity above 1 TeV (F>1TeV -12 ph cm-2 s-1) and in the 2-10 keV (X-ray) band (F2-10 keV -11 erg cm-2 s-1), during which the Swift-BAT data suggests an additional spectral component beyond the regular synchrotron *** highest flux variability occurs in X-rays and very-high-energy (E>0.1 TeV) γ-rays, which, despite the low activity, show a significant positive correlation with no time lag. The HRkeV and HRTeV show the harder-when-brighter trend observed in many blazars, but the trend flattens at the highest fluxes, which suggests a change in the processes dominating the blazar variability. Enlarging our data set with data from years 2007 to 2014, we measured a positive correlation between the optical and the GeV emission over a range of about 60 days centered at time lag zero, and a positive correlation between the optical/GeV and the radio emission over a range of about 60 days centered at a time lag of 43+-96 *** observation is consistent with the radio-bright zone being located about 0.2 parsec downstream from the optical/GeV emission regions of the jet. The flux distributions are better described with a LogNormal function in most of the energy bands probed, indicating that the variability in Mrk 421 is likely produced by a multiplicative process. Copyright © 2020, The Authors. All rights reserved.

关键词： Optical correlation

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Observation of VVZ production at s=13 TeV with the ATLAS detector

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Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics 2025年 866卷

作者： Aad, G. Aakvaag, E. Abbott, B. Abdelhameed, S. Abeling, K. Abicht, N.J. Abidi, S.H. Aboelela, M. Aboulhorma, A. Abramowicz, H. Abulaiti, Y. Acharya, B.S. Ackermann, A. Adam Bourdarios, C. Adamczyk, L. Addepalli, S.V. Addison, M.J. Adelman, J. Adiguzel, A. Adye, T. Affolder, A.A. Afik, Y. Agaras, M.N. Aggarwal, A. Agheorghiesei, C. Ahmadov, F. Ahuja, S. Ai, X. Aielli, G. Aikot, A. Ait Tamlihat, M. Aitbenchikh, B. Akbiyik, M. Åkesson, T.P.A. Akimov, A.V. Akiyama, D. Akolkar, N.N. Aktas, S. Alberghi, G.L. Albert, J. Albicocco, P. Albouy, G.L. Alderweireldt, S. Alegria, Z.L. Aleksa, M. Aleksandrov, I.N. Alexa, C. Alexopoulos, T. Alfonsi, F. Algren, M. Alhroob, M. Ali, B. Ali, H.M.J. Ali, S. Alibocus, S.W. Aliev, M. Alimonti, G. Alkakhi, W. Allaire, C. Allbrooke, B.M.M. Allen, J.S. Allen, J.F. Allport, P.P. Aloisio, A. Alonso, F. Alpigiani, C. Alsolami, Z.M.K. Alvarez Fernandez, A. Alves Cardoso, M. Alviggi, M.G. Aly, M. Amaral Coutinho, Y. Ambler, A. Amelung, C. Amerl, M. Ames, C.G. Amidei, D. Amini, B. Amirie, K. Amirkhanov, A. Amor Dos Santos, S.P. Amos, K.R. Amperiadou, D. An, S. Ananiev, V. Anastopoulos, C. Andeen, T. Anders, J.K. Anderson, A.C. Andreazza, A. Angelidakis, S. Angerami, A. Anisenkov, A.V. Annovi, A. Antel, C. Antipov, E. Antonelli, M. Anulli, F. Aoki, M. Aoki, T. Aparo, M.A. Aperio Bella, L. Appelt, C. Apyan, A. Arbiol Val, S.J. Arcangeletti, C. Arce, A.T.H. Arguin, J.-F. Argyropoulos, S. Arling, J.-H. Arnaez, O. Arnold, H. Artoni, G. Asada, H. Asai, K. Asai, S. Asbah, N.A. Ashby Pickering, R.A. Aslam, A.M. Assamagan, K. Astalos, R. Astrand, K.S.V. Atashi, S. Atkin, R.J. Atmani, H. Atmasiddha, P.A. Augsten, K. Auriol, A.D. Austrup, V.A. Avolio, G. Axiotis, K. Azuelos, G. Babal, D. Bachacou, H. Bachas, K. Bachiu, A. Bachmann, E. Backes, M.J. Badea, A. Baer, T.M. Bagnaia, P. Bahmani, M. Bahner, D. Bai, K. Baines, J.T. Baines, L. Baker, O.K. Bakos, E. Bakshi Gupta, D. Balabram Filho, L.E. Balakrishnan, V. Balasubramanian, R. Baldin, E.M. Balek, P. Ballabene, E. Balli, F. Baltes, L.M. Balunas, W.K. Bal Department of Physics University of Adelaide Adelaide Australia Department of Physics University of Alberta Edmonton AB Canada Department of Physics Ankara University Ankara Turkey Division of Physics TOBB University of Economics and Technology Ankara Turkey LAPP Université Savoie Mont Blanc CNRS/IN2P3 Annecy France APC Université Paris Cité CNRS/IN2P3 Paris France High Energy Physics Division Argonne National Laboratory Argonne IL United States Department of Physics University of Arizona Tucson AZ United States Department of Physics University of Texas at Arlington Arlington TX United States Physics Department National and Kapodistrian University of Athens Athens Greece Physics Department National Technical University of Athens Zografou Greece Department of Physics University of Texas at Austin Austin TX United States Institute of Physics Azerbaijan Academy of Sciences Baku Azerbaijan Institut de Física d'Altes Energies (IFAE) Barcelona Institute of Science and Technology Barcelona Spain Institute of High Energy Physics Chinese Academy of Sciences Beijing China Physics Department Tsinghua University Beijing China Institute of Physics University of Belgrade Belgrade Serbia Department for Physics and Technology University of Bergen Bergen Norway Physics Division Lawrence Berkeley National Laboratory Berkeley CA United States University of California Berkeley CA United States Institut für Physik Humboldt Universität zu Berlin Berlin Germany Albert Einstein Center for Fundamental Physics Laboratory for High Energy Physics University of Bern Bern Switzerland School of Physics and Astronomy University of Birmingham Birmingham United Kingdom Department of Physics Bogazici University Istanbul Turkey Department of Physics Engineering Gaziantep University Gaziantep Turkey Department of Physics Istanbul University Istanbul Turkey Facultad de Ciencias y Centro de Investigaciónes Universidad Antonio Nariño Bogotá Colombia Departamento d

A search for the production of three massive vector bosons, VVZ(V=W,Z), in proton–proton collisions at s=13 TeV is performed using data with an integrated luminosity of 140 fb−1 recorded by the ATLAS detector at the ...

A search for the production of three massive vector bosons, VVZ(V=W,Z), in proton–proton collisions at s=13 TeV is performed using data with an integrated luminosity of 140 fb⁻¹ recorded by the ATLAS detector at the Large Hadron Collider. Events produced in the leptonic final states WWZ→ℓνℓνℓℓ (ℓ=e,μ), WZZ→ℓνℓℓℓℓ, ZZZ→ℓℓℓℓℓℓ, and the semileptonic final states WWZ→qqℓνℓℓ and WZZ→ℓνqqℓℓ, are analysed. The measured cross section for the pp→VVZ process is 660₋₉₀⁺⁹³(stat.)₋₈₁⁺⁸⁸(syst.) fb, and the observed (expected) significance is 6.4 (4.7) standard deviations, representing the observation of VVZ production. In addition, the measured cross section for the pp→WWZ process is 442±94(stat.)₋₅₂⁺⁶⁰(syst.) fb, and the observed (expected) significance is 4.4 (3.6) standard deviations, representing evidence of WWZ production. The measured cross sections are consistent with the Standard Model predictions. Constraints on physics beyond the Standard Model are also derived in the effective field theory framework by setting limits on Wilson coefficients for dimension-8 operators describing anomalous quartic gauge boson couplings. © 2025 CERN for the benefit of the ATLAS Collaboration

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Indirect Search for Dark Matter from the Galactic Center and Halo with the Super-Kamiokande Detector

arXiv

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arXiv 2020年

作者： Abe, K. Bronner, C. Haga, Y. Hayato, Y. Ikeda, M. Imaizumi, S. Ito, H. Iyogi, K. Kameda, J. Kataoka, Y. Kato, Y. Kishimoto, Y. Marti, L. Miura, M. Moriyama, S. Mochizuki, T. Nagao, Y. Nakahata, M. Nakajima, Y. Nakajima, T. Nakayama, S. Okada, T. Okamoto, K. Orii, A. Pronost, G. Sekiya, H. Shiozawa, M. Sonoda, Y. Takeda, A. Takenaka, A. Tanaka, H. Tasaka, S. Tomura, T. Ueno, K. Yano, T. Yokozawa, T. Akutsu, R. Han, S. Irvine, T. Kajita, T. Kametani, I. Lee, K.P. McLachlan, T. Okumura, K. Richard, E. Tashiro, T. Wang, R. Xia, J. Bravo-Berguño, D. Labarga, L. Fernandez, P. Blaszczyk, F.D.M. Gustafson, J. Kachulis, C. Kearns, E. Raaf, J.L. Stone, J.L. Sulak, L.R. Sussman, S. Wan, L. Wester, T. Berkman, S. Tobayama, S. Bian, J. Carminati, G. Elnimr, M. Griskevich, N.J. Kropp, W.R. Locke, S. Mine, S. Renshaw, A. Smy, M.B. Sobel, H.W. Takhistov, V. Weatherly, P. Hartfiel, B.L. Hill, J. Keig, W.E. Hong, N. Kim, J.Y. Lim, I.T. Park, R.G. Akiri, T. Bodur, B. Himmel, A. Li, Z. O’Sullivan, E. Scholberg, K. Walter, C.W. Wongjirad, T. Coffani, A. Drapier, O. El Hedri, S. Giampaolo, A. Gonin, M. Imber, J. Mueller, Th.A. Paganini, P. Quilain, B. Ishizuka, T. Nakamura, T. Jang, J.S. Choi, K. Learned, J.G. Matsuno, S. Smith, S.N. Amey, J. Anthony, L.H.V. Litchfield, R.P. Ma, W.Y. Sztuc, A.A. Uchida, Y. Wascko, M.O. Berardi, V. Catanesi, M.G. Intonti, R.A. Radicioni, E. Calabria, N.F. Machado, L.N. de Rosa, G. Collazuol, G. Iacob, F. Lamoureux, M. Ospina, N. Ludovici, L. Boschi, T. Di Lodovico, F. Molina Sedgwick, S. Zsoldos, S. Nishimura, Y. Cao, S. Friend, M. Hasegawa, T. Ishida, T. Ishii, T. Kobayashi, T. Nakadaira, T. Nakamura, K. Oyama, Y. Sakashita, K. Sekiguchi, T. Tsukamoto, T. Abe, K.E. Hasegawa, M. Isobe, Y. Miyabe, H. Nakano, Y. Shiozawa, T. Sugimoto, T. Suzuki, A.T. Takeuchi, Y. Yamamoto, S. Ali, A. Ashida, Y. Hayashino, T. Hiraki, T. Hirota, S. Huang, K. Ieki, K. Jiang, M. Kikawa, T. Mori, M. Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu506-1205 Japan Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Kashiwa Chiba277-8582 Japan Department of Theoretical Physics University Autonoma Madrid Madrid28049 Spain Department of Physics Boston University BostonMA02215 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T1Z4 Canada Department of Physics and Astronomy University of California Irvine IrvineCA92697-4575 United States Department of Physics California State University Dominguez Hills CarsonCA90747 United States Institute for Universe and Elementary Particles Chonnam National University Gwangju61186 Korea Republic of Department of Physics Duke University DurhamNC27708 United States Ecole Polytechnique IN2P3-CNRS Laboratoire Leprince-Ringuet PalaiseauF-91120 France Junior College Fukuoka Institute of Technology Fukuoka Fukuoka811-0295 Japan Department of Physics Gifu University Gifu Gifu501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju61005 Korea Republic of Department of Physics and Astronomy University of Hawaii HonoluluHI96822 United States Department of Physics Imperial College London LondonSW7 2AZ United Kingdom Dipartimento Interuniversitario di Fisica INFN Sezione di Bari Università e Politecnico di Bari BariI-70125 Italy Dipartimento di Fisica INFN Sezione di Napoli Università di Napoli NapoliI-80126 Italy Dipartimento di Fisica INFN Sezione di Padova Università di Padova PadovaI-35131 Italy INFN Sezione di Roma Università di Roma "La Sapienza" RomaI-00185 Italy Department of Physics King’s College London LondonWC2R 2LS United Kingdom Department of Physics Keio University Yokohama Kanagawa223-8522 Japan Tsukuba Ibaraki305-0801 Japan Department of Physics Kobe University Kobe Hyogo657-8501 Japan Department of Physics Kyoto Unive

We present a search for an excess of neutrino interactions due to dark matter in the form of Weakly Interacting Massive Particles (WIMPs) annihilating in the galactic center or halo based on the data set of Super-Kamiokande-I, -II, -III and -IV taken from 1996 to 2016. We model the neutrino_flux, energy, and flavor distributions assuming WIMP self-annihilation is dominant to νν, µ+µ−, bb, or W+W−. The excess is in comparison to atmospheric neutrino interactions which are modeled in detail and fit to data. Limits on the self-annihilation cross section hσAV i are derived for WIMP masses in the range 1 GeV to 10 TeV, reaching as low as 9.6 × 10−23 cm3 s−1 for 5 GeV WIMPs in b¯b mode and 1.2×10−24 cm3 s−1 for 1 GeV WIMPs in νν¯ mode. The obtained sensitivity of the Super-Kamiokande detector to WIMP masses below several tens of GeV is the best among similar indirect searches to date. Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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26th Annual Computational Neuroscience Meeting (CNS*2017): Part 3 Antwerp, Belgium. 15-20 July 2017 Abstracts

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BMC NEUROSCIENCE 2017年第SUPPL 1期18卷 95-176页

作者： [Anonymous] Department of Neuroscience Yale University New Haven CT 06520 USA Department Physiology & Pharmacology SUNY Downstate Brooklyn NY 11203 USA NYU School of Engineering 6 MetroTech Center Brooklyn NY 11201 USA Departament de Matemàtica Aplicada Universitat Politècnica de Catalunya Barcelona 08028 Spain Institut de Neurobiologie de la Méditerrannée (INMED) INSERM UMR901 Aix-Marseille Univ Marseille France Center of Neural Science New York University New York NY USA Aix-Marseille Univ INSERM INS Inst Neurosci Syst Marseille France Laboratoire de Physique Théorique et Modélisation CNRS UMR 8089 Université de Cergy-Pontoise 95300 Cergy-Pontoise Cedex France Department of Mathematics and Computer Science ENSAT Abdelmalek Essaadi’s University Tangier Morocco Laboratory of Natural Computation Department of Information and Electrical Engineering and Applied Mathematics University of Salerno 84084 Fisciano SA Italy Department of Medicine University of Salerno 84083 Lancusi SA Italy Dipartimento di Fisica Università degli Studi Aldo Moro Bari and INFN Sezione Di Bari Italy Data Analysis Department Ghent University Ghent Belgium Coma Science Group University of Liège Liège Belgium Cruces Hospital and Ikerbasque Research Center Bilbao Spain BIOtech Department of Industrial Engineering University of Trento and IRCS-PAT FBK 38010 Trento Italy Department of Data Analysis Ghent University Ghent 9000 Belgium The Wellcome Trust Centre for Neuroimaging University College London London WC1N 3BG UK Department of Electronic Engineering NED University of Engineering and Technology Karachi Pakistan Blue Brain Project École Polytechnique Fédérale de Lausanne Lausanne Switzerland Departement of Mathematics Swansea University Swansea Wales UK Laboratory for Topology and Neuroscience at the Brain Mind Institute École polytechnique fédérale de Lausanne Lausanne Switzerland Institute of Mathematics University of Aberdeen Aberdeen Scotland UK Department of Integrativ

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Growth mechanism of Co:TiO2 thin film deposited by metal organic chemical vapor deposition technique

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IOP Conference Series: Materials Science and engineering 2016年第1期128卷

作者： A Saripudin P Arifin Study Program of Electrical Engineering Dept. of Electrical Engineering Education Faculty of Technology and Vocational Universitas Pendidikan Indonesia Jl. Dr. Setiabudi 207 Bandung 40154 West Java Indonesia Physics of Electronics Material Lab. Study Program of Physics Faculty of Mathematics and Natural Science Institut Teknologi Bandung Jl. Ganeca 10 Bandung 40132 West Java Indonesia

In this research, we investigated the growth mechanism of cobalt-doped titanium dioxide (Co:TiO2) films. Thi Co:TiO2 thin films were grown on the n-type silicon substrate. The films were grown by metal organic chemical vapor deposition method. The growth temperature was varied of 325°C – 450°C. The films were characterized by SEM. Using Arheniu's equation, it is known that the activation energy value of film growth is positive in the range of temperature of 325°C – 400°C and negative in the range of temperature of 400°C – 450°C. These results show that the decomposition rate in the range of temperature of 325°C – 400°C is due to diffusion phase of precursor gas. On the other hand, the decomposition rate decreased in the range of temperature of 400°C – 450°C because the precursor gas decreased, and the surface chemical reaction was high.

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Bioremediation of Aged Petroleum Oil Contaminated Soil: From Laboratory Scale to Full Scale Application

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Procedia Chemistry 2015年 14卷 326-333页

作者： Qomarudin Helmy Rudy Laksmono Edwan Kardena Environmental Engineering Dept Faculty of Civil and Environmental Engineering Institut Teknologi Bandung Ganesha No. 10 BandungWest Java 40132 Indonesia Energy Security Study Program Indonesia Defence University Salemba Raya No. 14 Jakarta 10430 Indonesia

Large quantity of aged petroleum oil contamination such as dehydrated oil sludge, generated in the disposal process of oil-containing sewage in Indonesia. This study aims to investigate the OSCS removal by mean of bioremediation technique. Results found that petrofilic consortia and biosurfactants addition increased the removal efficiency up to 46% and 85%, respectively. At full scale application, this technique succeed in removing of 46 g TPH per kg soil from 4 883 m 3 of OSCS during 16 mo of treatment. These results suggest that petrofilic consortia and biosurfactants addition stimulate the biodegradation and overcome the limitation of OSCS degradation process.

关键词： Biodegradation bioremediation biosurfactant oil sludge petrofilic petroleum.

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Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Anti-neutrinos from Pre-supernova Emission

arXiv

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arXiv 2019年

作者： Simpson, C. Abe, K. Bronner, C. Hayato, Y. Ikeda, M. Ito, H. Iyogi, K. Kameda, J. Kataoka, Y. Kato, Y. Kishimoto, Y. Marti, L.L. Miura, M. Moriyama, S. Mochizuki, T. Nakahata, M. Nakajima, Y. Nakayama, S. Okada, T. Okamoto, K. Orii, A. Pronost, G. Sekiya, H. Shiozawa, M. Sonoda, Y. Takeda, A. Takenaka, A. Tanaka, H. Yano, T. Akutsu, R. Kajita, T. Okumura, K. Wang, R. Xia, J. Bravo-Berguño, D. Labarga, L. Fernandez, P. Blaszczyk, F.D.M. Kachulis, C. Kearns, E. Raaf, J.L. Stone, J.L. Wan, L. Wester, T. Sussman, S. Berkman, S. Bian, J. Griskevich, N.J. Kropp, W.R. Locke, S. Mine, S. Smy, M.B. Sobel, H.W. Takhistov, V. Weatherly, P. Ganezer, K.S. Hill, J. Kim, J.Y. Lim, I.T. Park, R.G. Bodur, B. Scholberg, K. Walter, C.W. Coffani, A. Drapier, O. Gonin, M. Imber, J. Mueller, T.H.A. Paganini, P. Ishizuka, T. Nakamura, T. Jang, J.S. Choi, K. Learned, J.G. Matsuno, S. Litchfield, R.P. Sztuc, A.A. Uchida, Y. Wascko, M.O. Berardi, V. Calabria, N.F. Catanesi, M.G. Intonti, R.A. Radicioni, E. de Rosa, G. Collazuol, G. Iacob, F. Ludovici, L. Nishimura, Y. Cao, S. Friend, M. Hasegawa, T. Ishida, T. Kobayashi, T. Nakadaira, T. Nakamura, K. Oyama, Y. Sakashita, K. Sekiguchi, T. Tsukamoto, T. Abe, K.E. Hasegawa, M. Isobe, Y. Miyabe, H. Nakano, Y. Shiozawa, T. Sugimoto, T. Suzuki, A.T. Takeuchi, Y. Ali, A. Ashida, Y. Hayashino, T. Hirota, S. Jiang, M. Kikawa, T. Mori, M. Nakamura, K.E. Nakaya, T. Wendell, R.A. Anthony, L.H.V. McCauley, N. Pritchard, A. Tsui, K.M. Fukuda, Y. Itow, Y. Murrase, M. Niwa, T. Taani, M. Tsukada, M. Mijakowski, P. Frankiewicz, K. Jung, C.K. Li, X. Palomino, J.L. Santucci, G. Vilela, C. Wilking, M.J. Yanagisawa, C. Fukuda, D. Harada, M. Hagiwara, K. Horai, T. Ishino, H. Ito, S. Koshio, Y. Sakuda, M. Takahira, Y. Xu, C. Kuno, Y. Cook, L. Wark, D. Di Lodovico, F. Sedgwick, S.M. Molina Richards, B. Zsoldos, S. Kim, S.B. Tacik, R. Thiesse, M. Thompson, L. Okazawa, H. Department of Physics Oxford University OxfordOX1 3PU United Kingdom University of Tokyo Institutes for Advanced Study University of Tokyo KashiwaChiba277-8583 Japan Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu506-1205 Japan Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo KashiwaChiba277-8582 Japan Department of Theoretical Physics University Autonoma Madrid Madrid28049 Spain Department of Physics Boston University BostonMA02215 United States Department of Physics and Astronomy University of California Irvine IrvineCA92697-4575 United States Department of Physics California State University Dominguez Hills CarsonCA90747 United States Department of Physics Chonnam National University Kwangju500-757 Korea Republic of Department of Physics Duke University DurhamNC27708 United States Ecole Polytechnique IN2P3-CNRS Laboratoire Leprince-Ringuet PalaiseauF-91120 France Junior College Fukuoka Institute of Technology FukuokaFukuoka811-0295 Japan Department of Physics Gifu University GifuGifu501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju500-712 Korea Republic of Department of Physics and Astronomy University of Hawaii HonoluluHI96822 United States Department of Physics Imperial College London LondonSW7 2AZ United Kingdom Dipartimento Interuniversitario di Fisica INFN Sezione di Bari Università e Politecnico di Bari BariI-70125 Italy Dipartimento di Fisica INFN Sezione di Napoli Università di Napoli NapoliI-80126 Italy Dipartimento di Fisica INFN Sezione di Padova Università di Padova PadovaI-35131 Italy INFN Sezione di Roma Università di Roma "La Sapienza" RomaI-00185 Italy Department of Physics King’s College London LondonWC2R 2LS United Kingdom Department of Physics Keio University YokohamaKanagawa223-8522 Japan TsukubaIbaraki305-0801 Japan Department of Physics Kobe University KobeHyogo

Supernova detection is a major objective of the Super-Kamiokande (SK) experiment. In the next stage of SK (SK-Gd), gadolinium (Gd) sulfate will be added to the detector, which will improve the ability of the detector to identify neutrons. A core-collapse supernova will be preceded by an increasing flux of neutrinos and anti-neutrinos, from thermal and weak nuclear processes in the star, over a timescale of hours;some of which may be detected at SK-Gd. This could provide an early warning of an imminent core-collapse supernova, hours earlier than the detection of the neutrinos from core collapse. Electron anti-neutrino detection will rely on inverse beta decay events below the usual analysis energy threshold of SK, so Gd loading is vital to reduce backgrounds while maximising detection efficiency. Assuming normal neutrino mass ordering, more than 200 events could be detected in the final 12 hours before core collapse for a 15-25 solar mass star at around 200 pc, which is representative of the nearest red supergiant to Earth, α-Ori (Betelgeuse). At a statistical false alarm rate of 1 per century, detection could be up to 10 hours before core collapse, and a pre-supernova star could be detected by SK-Gd up to 600 pc away. A pre-supernova alert could be provided to the astrophysics community following gadolinium loading. Copyright © 2019, The Authors. All rights reserved.

关键词： Supernovae

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Heart sound feature extraction and classification using autoregressive power spectral density (AR-PSD) and statistics features

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AIP Conference Proceedings 2016年第1期1755卷

作者： Domy Kristomo Risanuri Hidayat Indah Soesanti Adi Kusjani 1Department of Electrical Engineering and Information Technology Faculty of Engineering Gadjah Mada University Jalan Grafika No. 2 Yogyakarta 55281 Indonesia 2Study Program of Computer Engineering STMIK AKAKOM of Yogyakarta Jalan Raya Janti 143 Karang Jambe Yogyakarta 55198 Indonesia

Heart auscultation is a screening method done by listening using a stethoscope for early diagnosis of heart disease, it is low cost and non-invasive, but it has a limitation of human hearing. This paper presents a noise-robust feature extraction method by combining and selecting a heart sound (HS) feature in time and frequency domain. Wavelet decomposition (WD) is used for noise removal. Features are extracted by AR-PSD and used as inputs for classification. The nine types of abnormal HS that were taken from Michigan Heart Sound Database were classified into nine categories. In this research, statistics features in time and frequency domain are used as additional features. Correlation-based Feature Selection (CFS) is used to select the best feature among 13 features extracted. The performance of a new feature set is called Feature Set 3 compared to CFS. The result shows that the proposed feature set achieves the highest level of accuracy.

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Data rate of connections in performing packet delivery of Wireless Mesh Network using Hybrid Wireless Mesh Protocol and Optimized Link State Routing protocol 1

Data rate of connections in performing packet delivery of Wi...

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2014 1st International Conference on Information Technology, Computer, and Electrical engineering, ICITACEE 2014

作者： Putra, Alexander William Setiawan Suhartomo, Antonius Faculty of Engineering Study Program of Electrical Engineering President University Bekasi Indonesia

ISBN: (纸本)9781479964314

Wireless Mesh Network (WMN) relies in routing protocols for route discovery from sender to receiving nodes. There are two routing protocols that are evaluated: Hybrid Wireless Mesh Protocol (HWMP) and Optimized Link State Routing (OLSR). Packet delivery is very crucial in telecommunication. Data rate of connections relate closely with the performance of packet delivery in telecommunication especially WMN. HWMP and OLSR have different mechanisms of route discovery which are affected by the changes of data rate of connections and can affect the packet delivery of data. This experiment focuses in evaluating the performance of both protocols under different conditions of data rate of connections. The objective of this experiment is to evaluate the performance of both protocols and find the relevancy between the results of simulations and theories of the mechanism of both protocols. All of the simulations are done with using Network Simulator Version 3. The simulations are done for more than 100 times in order to get the consistency of the results of simulations and to evaluate the natural behaviors of both protocols. © 2014 IEEE.

关键词： Routing protocols

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