检索结果-内蒙古大学图书馆

The readout system based on the ultra-fast waveform sampler DRS4 for the Large-Sized Telescope of the Cherenkov Telescope Array

学校读者我要写书评

暂无评论

Journal of physics: Conference Series 2020年第1期1468卷

作者： S Nozaki O Blanch C Delgado P Gliwny D Hadasch Y Inome H Katagiri H Kubo Y Kobayashi D Mazin A Moralejo Y Nogami R Paoletti T Saito S Sakurai J Sitarek M Takahashi M Teshima T Yamamoto for the CTA Consortium Division of Physics and Astronomy Graduate School of Science Kyoto University Sakyo-ku Kyoto 606-8502 Japan Institut de Fisica d'Altes Energies (IFAE) The Barcelona Institute of Science and Technology Campus UAB 08193 Bellaterra (Barcelona) Spain CIEMAT Avda. Complutense 40 28040 Madrid Spain Faculty of Physics and Applied Computer Science University of Lódź ul. Pomorska 149-153 90-236 Lódź Poland Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Kashiwa Chiba 277-8582 Japan Faculty of Science Ibaraki University Mito Ibaraki 310-8512 Japan INFN Sezione di Pisa Largo Pontecorvo 3 56217 Pisa Italy Department of Physics Konan University Kobe Hyogo 658-8501 Japan

The Cherenkov Telescope Array (CTA) is the next-generation ground-based very-high-energy gamma-ray observatory. By using three types of telescopes CTA can cover a wide energy range (20 GeV–300 TeV) with an order of magnitude higher sensitivity than the current telescopes. The Large-Sized Telescope (LST) is designed to detect 20 GeV–1 TeV gamma rays thanks to the large light collection area, sensitive photosensors, a fast trigger system, and readout electronics. The camera readout system must have a high signal-to-noise ratio and a linear signal sampling with a large dynamic range in order to efficiently detect dim and low-energy atmospheric showers. To meet this requirement we use the Domino Ring Sampler version 4 (DRS4), which also enables ultra-fast sampling with low power consumption. Some of the intrinsic characteristics of DRS4 chips require software corrections. These procedures lower the effect of non-Gaussian noise contribution and improve the timing resolution of the system. In this contribution we discuss the calibration algorithms and the resulting performance.

关键词：

The dark energy survey supernova program: Cosmological biases from supernova photometric classification

学校读者我要写书评

暂无评论

arXiv 2021年

作者： Vincenzi, Maria Sullivan, M. Möller, A. Armstrong, P. Bassett, B.A. Brout, D. Carollo, D. Carr, A. Davis, T.M. Frohmaier, C. Galbany, L. Glazebrook, K. Graur, O. Kelsey, L. Kessler, R. Kovacs, E. Lewis, G.F. Lidman, C. Malik, U. Nichol, R.C. Popovic, B. Sako, M. Scolnic, D. Smith, M. Taylor, G. Tucker, B.E. Wiseman, P. Aguena, M. Allam, S. Annis, J. Asorey, J. Bacon, D. Bertin, E. Brooks, D. Burke, D.L. Rosell, A. Carnero Carretero, J. Castander, F.J. Costanzi, M. da Costa, L.N. Pereira, M.E.S. De Vicente, J. Desai, S. Diehl, H.T. Doel, P. Everett, S. Ferrero, I. Flaugher, B. Fosalba, P. Frieman, J. García-Bellido, J. Gerdes, D.W. Gruen, D. Gutierrez, G. Hinton, S.R. Hollowood, D.L. Honscheid, K. James, D.J. Kuehn, K. Kuropatkin, N. Lahav, O. Li, T.S. Lima, M. Maia, M.A.G. Marshall, J.L. Miquel, R. Morgan, R. Ogando, R.L.C. Palmese, A. Paz-Chinchón, F. Pieres, A. Malagón, A.A. Plazas Reil, K. Roodman, A. Sanchez, E. Schubnell, M. Serrano, S. Sevilla-Noarbe, I. Suchyta, E. Tarle, G. To, C. Varga, T.N. Weller, J. Wilkinson, R.D. School of Physics and Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Department of Physics Duke University DurhamNC27708 United States Centre for Astrophysics & Supercomputing Swinburne University of Technology VIC3122 Australia Université Clermont Auvergne CNRS IN2P3 LPC Clermont-FerrandF-63000 France The Research School of Astronomy and Astrophysics Australian National University ACT2601 Australia Madrid Spain African Institute for Mathematical Sciences 6 Melrose Road Muizenberg7945 South Africa Department of Maths and Applied Maths University of Cape Town Cape Town South Africa South African Astronomical Observatory Observatory Cape Town7925 South Africa Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States NASA Einstein INAF Astrophysical Observatory of Turin Pino TorineseI-10025 Italy School of Mathematics and Physics University of Queensland BrisbaneQLD4072 Australia Barcelona08034 Spain Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Department of Astrophysics American Museum of Natural History New YorkNY United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Sydney Institute for Astronomy School of Physics A28 The University of Sydney NSW2006 Australia Centre for Gravitational Astrophysics College of Science The Australian National University ACT2601 Australia Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Fermi National Accelerator Laboratory P. O. B

Cosmological analyses of samples of photometrically-identified Type Ia supernovae (SNe Ia) depend on understanding the effects of 'contamination' from core-collapse and peculiar SN Ia events. We employ a rigorous analysis on state-of-the-art simulations of photometrically identified SN Ia samples and determine cosmological biases due to such 'non-Ia' contamination in the Dark Energy Survey (DES) 5-year SN sample. As part of the analysis, we test on our DES simulations the performance of SuperNNova, a photometric SN classifier based on recurrent neural networks. Depending on the choice of non-Ia SN models in both the simulated data sample and training sample, contamination ranges from 0.8-3.5 per cent, with the efficiency of the classification from 97.7-99.5 per cent. Using the Bayesian Estimation applied to Multiple Species (BEAMS) framework and its extension BBC ('BEAMS with Bias Correction'), we produce a redshift-binned Hubble diagram marginalised over contamination and corrected for selection effects and we use it to constrain the dark energy equation-of-state, w. Assuming a flat universe with Gaussian ΩM prior of 0.311 ± 0.010, we show that biases on w are w,syst = 0.004. This compares to an expected statistical uncertainty of σw,stat = 0.039 for the DES-SN sample, thus showing that contamination is not a limiting uncertainty in our analysis. We also measure biases due to contamination on w0 and wa (assuming a flat universe), and find these to be 0 and a, hence 5 to 10 times smaller than the statistical uncertainties expected from the DES-SN sample. Copyright © 2021, The Authors. All rights reserved.

关键词： Surveys

The origin of antibunching in resonance fluorescence

学校读者我要写书评

暂无评论

arXiv 2020年

作者： Hanschke, Lukas Schweickert, Lucas Carreño, Juan Camilo López Schöll, Eva Zeuner, Katharina D. Lettner, Thomas Casalengua, Eduardo Zubizarreta Reindl, Marcus da Silva, Saimon Filipe Covre Trotta, Rinaldo Finley, Jonathan J. Rastelli, Armando del Valle, Elena Laussy, Fabrice P. Zwiller, Val Müller, Kai Jöns, Klaus D. Walter Schottky Institut Department of Electrical and Computer Engineering Technische Universität München Garching85748 Germany Munich80799 Germany Department of Applied Physics Royal Institute of Technology Albanova University Centre Roslagstullsbacken 21 Stockholm106 91 Sweden Faculty of Science and Engineering University of Wolverhampton Wulfruna St WolverhamptonWV1 1LY United Kingdom Institute of Semiconductor and Solid State Physics Johannes Kepler University Linz 4040 Austria Dipartimento di Fisica Sapienza Università di Roma Piazzale A. Moro 1 RomaI-00185 Italy Walter Schottky Institut and Physik Department Technische Universität München Garching85748 Germany Departamento de Física Téorica de la Materia Condensada Universidad Autónoma de Madrid Madrid28049 Spain Russian Quantum Center Novaya 100 Skolkovo Moscow Region143025 Russia

Epitaxial quantum dots have emerged as one of the best single-photon sources, not only for applications in photonic quantum technologies but also for testing fundamental properties of quantum optics. One intriguing observation in this area is the scattering of photons with subnatural linewidth from a two-level system under resonant continuous wave excitation. In particular, an open question is whether these subnatural linewidth photons exhibit simultaneously antibunching as an evidence of single-photon emission. Here, we demonstrate that this simultaneous observation of subnatural linewidth and antibunching is not possible with simple resonant excitation. First, we independently confirm single-photon character and subnatural linewidth by demonstrating antibunching in a Hanbury Brown and Twiss type setup and using high-resolution spectroscopy, respectively. However, when filtering the coherently scattered photons with filter bandwidths on the order of the homogeneous linewidth of the excited state of the two-level system, the antibunching dip vanishes in the correlation measurement. Our experimental work is consistent with recent theoretical findings, that explain antibunching from photon-interferences between the coherent scattering and a weak incoherent signal in a skewed squeezed state. Copyright © 2020, The Authors. All rights reserved.

关键词： Photons

Measurements of the W boson rapidity, helicity, double-differential cross sections, and charge asymmetry in pp collisions at s=13 TeV

学校读者我要写书评

暂无评论

Physical Review D 2020年第9期102卷 092012-092012页

作者： A. M. Sirunyan A. Tumasyan W. Adam F. Ambrogi T. Bergauer M. Dragicevic J. Erö A. Escalante Del Valle R. Frühwirth M. Jeitler N. Krammer L. Lechner D. Liko T. Madlener I. Mikulec N. Rad J. Schieck R. Schöfbeck M. Spanring S. Templ W. Waltenberger C.-E. Wulz M. Zarucki V. Chekhovsky A. Litomin V. Makarenko J. Suarez Gonzalez M. R. Darwish E. A. De Wolf D. Di Croce X. Janssen T. Kello A. Lelek M. Pieters H. Rejeb Sfar H. Van Haevermaet P. Van Mechelen S. Van Putte N. Van Remortel F. Blekman E. S. Bols S. S. Chhibra J. D’Hondt J. De Clercq D. Lontkovskyi S. Lowette I. Marchesini S. Moortgat Q. Python S. Tavernier W. Van Doninck P. Van Mulders D. Beghin B. Bilin B. Clerbaux G. De Lentdecker H. Delannoy B. Dorney L. Favart A. Grebenyuk A. K. Kalsi I. Makarenko L. Moureaux L. Pétré A. Popov N. Postiau E. Starling L. Thomas C. Vander Velde P. Vanlaer D. Vannerom L. Wezenbeek T. Cornelis D. Dobur I. Khvastunov M. Niedziela C. Roskas K. Skovpen M. Tytgat W. Verbeke B. Vermassen M. Vit G. Bruno C. Caputo P. David C. Delaere M. Delcourt I. S. Donertas A. Giammanco V. Lemaitre J. Prisciandaro A. Saggio A. Taliercio P. Vischia S. Wuyckens J. Zobec G. A. Alves G. Correia Silva C. Hensel A. Moraes W. L. Aldá Júnior E. Belchior Batista Das Chagas W. Carvalho J. Chinellato E. Coelho E. M. Da Costa G. G. Da Silveira D. De Jesus Damiao S. Fonseca De Souza H. Malbouisson J. Martins D. Matos Figueiredo M. Medina Jaime M. Melo De Almeida C. Mora Herrera L. Mundim H. Nogima P. Rebello Teles L. J. Sanchez Rosas A. Santoro S. M. Silva Do Amaral A. Sznajder M. Thiel E. J. Tonelli Manganote F. Torres Da Silva De Araujo A. Vilela Pereira C. A. Bernardes L. Calligaris T. R. Fernandez Perez Tomei E. M. Gregores D. S. Lemos P. G. Mercadante S. F. Novaes Sandra S. Padula A. Aleksandrov G. Antchev I. Atanasov R. Hadjiiska P. Iaydjiev M. Misheva M. Rodozov M. Shopova G. Sultanov M. Bonchev A. Dimitrov T. Ivanov L. Litov B. Pavlov P. Petkov A. Petrov W. Fang X. Gao L. Yuan M. Ahmad Z. Hu Y. Wang E. Chapon G. M. Chen H. S. Chen M. Chen C. H. Jiang Yerevan Physics Institute Yerevan Armenia Institut für Hochenergiephysik Wien Austria Institute for Nuclear Problems Minsk Belarus Universiteit Antwerpen Antwerpen Belgium Vrije Universiteit Brussel Brussel Belgium Université Libre de Bruxelles Bruxelles Belgium Ghent University Ghent Belgium Université Catholique de Louvain Louvain-la-Neuve Belgium Centro Brasileiro de Pesquisas Fisicas Rio de Janeiro Brazil Universidade do Estado do Rio de Janeiro Rio de Janeiro Brazil Universidade Estadual Paulista São Paulo Brazil Universidade Federal do ABC São Paulo Brazil Institute for Nuclear Research and Nuclear Energy Bulgarian Academy of Sciences Sofia Bulgaria University of Sofia Sofia Bulgaria Beihang University Beijing China National Centre for Physics Quaid-I-Azam University Islamabad Pakistan Department of Physics Tsinghua University Beijing China University of Virginia Charlottesville Virginia USA Institute of High Energy Physics Beijing China Massachusetts Institute of Technology Cambridge Massachusetts USA State Key Laboratory of Nuclear Physics and Technology Peking University Beijing China The University of Kansas Lawrence Kansas USA Sun Yat-Sen University Guangzhou China Zhejiang University Hangzhou China Universidad de Los Andes Bogota Colombia Universidad de Antioquia Medellin Colombia University of Split Faculty of Electrical Engineering Mechanical Engineering and Naval Architecture Split Croatia University of Split Faculty of Science Split Croatia Institute Rudjer Boskovic Zagreb Croatia University of Cyprus Nicosia Cyprus Charles University Prague Czech Republic Escuela Politecnica Nacional Quito Ecuador Universidad San Francisco de Quito Quito Ecuador Academy of Scientific Research and Technology of the Arab Republic of Egypt Egyptian Network of High Energy Physics Cairo Egypt National Institute of Chemical Physics and Biophysics Tallinn Estonia Department of Physics University of Helsinki Helsinki Finland Helsinki Inst

The differential cross section and charge asymmetry for inclusive W boson production at s=13 TeV is measured for the two transverse polarization states as a function of the W boson absolute rapidity. The measurement uses events in which a W boson decays to a neutrino and either a muon or an electron. The data sample of proton-proton collisions recorded with the CMS detector at the LHC in 2016 corresponds to an integrated luminosity of 35.9 fb−1. The differential cross section and its value normalized to the total inclusive W boson production cross section are measured over the rapidity range |yW|<2.5. In addition to the total fiducial cross section, the W boson double-differential cross section, d2σ/dpTℓd|ηℓ|, and the charge asymmetry are measured as functions of the charged lepton transverse momentum and pseudorapidity. The precision of these measurements is used to constrain the parton distribution functions of the proton using the next-to-leading order NNPDF3.0 set.

关键词： Higgs bosons Polarization Hadron colliders

Chvátal's conjecture holds for ground sets of seven elements

学校读者我要写书评

暂无评论

arXiv 2018年

作者： EIFLER, LEON GLEIXNER, AMBROS PULAJ, JONAD Takustr. 7 Berlin14195 Germany Department of Computer Science Mathematics and Physics Faculty of Science and Technology University of the West Indies Cave Hill St. Michael Barbados

We establish a general computational framework for Chvatal's conjecture based on exact rational integer programming. As a result we prove Chvatal's conjecture holds for all downsets whose union of sets contains seven elements or less. The computational proof relies on an exact branch-and-bound certificate that allows for elementary verification and is independent of the integer programming solver used.05-XX COMBINATORICS (For finite fields, see 11Txx), 90-XX OPERATIONS RESEARCH, MATHEMATICAL PROGRAMMING Copyright © 2018, The Authors. All rights reserved.

关键词： Integer programming

Measurement of the Jet Mass Distribution and Top Quark Mass in Hadronic Decays of Boosted Top Quarks in pp Collisions at s=13 TeV

学校读者我要写书评

暂无评论

Physical Review Letters 2020年第20期124卷 202001-202001页

作者： A. M. Sirunyan A. Tumasyan W. Adam F. Ambrogi T. Bergauer J. Brandstetter M. Dragicevic J. Erö A. Escalante Del Valle M. Flechl R. Frühwirth M. Jeitler N. Krammer I. Krätschmer D. Liko T. Madlener I. Mikulec N. Rad J. Schieck R. Schöfbeck M. Spanring D. Spitzbart W. Waltenberger C.-E. Wulz M. Zarucki V. Drugakov V. Mossolov J. Suarez Gonzalez M. R. Darwish E. A. De Wolf D. Di Croce X. Janssen A. Lelek M. Pieters H. Rejeb Sfar H. Van Haevermaet P. Van Mechelen S. Van Putte N. Van Remortel F. Blekman E. S. Bols S. S. Chhibra J. D’Hondt J. De Clercq D. Lontkovskyi S. Lowette I. Marchesini S. Moortgat Q. Python K. Skovpen S. Tavernier W. Van Doninck P. Van Mulders D. Beghin B. Bilin H. Brun B. Clerbaux G. De Lentdecker H. Delannoy B. Dorney L. Favart A. Grebenyuk A. K. Kalsi A. Popov N. Postiau E. Starling L. Thomas C. Vander Velde P. Vanlaer D. Vannerom T. Cornelis D. Dobur I. Khvastunov M. Niedziela C. Roskas D. Trocino M. Tytgat W. Verbeke B. Vermassen M. Vit O. Bondu G. Bruno C. Caputo P. David C. Delaere M. Delcourt A. Giammanco V. Lemaitre J. Prisciandaro A. Saggio M. Vidal Marono P. Vischia J. Zobec F. L. Alves G. A. Alves G. Correia Silva C. Hensel A. Moraes P. Rebello Teles E. Belchior Batista Das Chagas W. Carvalho J. Chinellato E. Coelho E. M. Da Costa G. G. Da Silveira D. De Jesus Damiao C. De Oliveira Martins S. Fonseca De Souza L. M. Huertas Guativa H. Malbouisson J. Martins D. Matos Figueiredo M. Medina Jaime M. Melo De Almeida C. Mora Herrera L. Mundim H. Nogima W. L. Prado Da Silva L. J. Sanchez Rosas A. Santoro A. Sznajder M. Thiel E. J. Tonelli Manganote F. Torres Da Silva De Araujo A. Vilela Pereira C. A. Bernardes L. Calligaris T. R. Fernandez Perez Tomei E. M. Gregores D. S. Lemos P. G. Mercadante S. F. Novaes Sandra S. Padula A. Aleksandrov G. Antchev R. Hadjiiska P. Iaydjiev M. Misheva M. Rodozov M. Shopova G. Sultanov M. Bonchev A. Dimitrov T. Ivanov L. Litov B. Pavlov P. Petkov W. Fang X. Gao L. Yuan M. Ahmad Z. Hu Y. Wang G. M. Chen H. S. Chen M. Chen C. H. Jiang D. Leggat H. Liao Z. Liu A. Yerevan Physics Institute Yerevan Armenia Institut für Hochenergiephysik Wien Austria Institute for Nuclear Problems Minsk Belarus Universiteit Antwerpen Antwerpen Belgium Vrije Universiteit Brussel Brussel Belgium Université Libre de Bruxelles Bruxelles Belgium Ghent University Ghent Belgium Université Catholique de Louvain Louvain-la-Neuve Belgium Centro Brasileiro de Pesquisas Fisicas Rio de Janeiro Brazil Universidade do Estado do Rio de Janeiro Rio de Janeiro Brazil Universidade Estadual Paulista São Paulo Brazil Universidade Federal do ABC São Paulo Brazil Institute for Nuclear Research and Nuclear Energy Bulgarian Academy of Sciences Sofia Bulgaria University of Sofia Sofia Bulgaria Beihang University Beijing China National Centre for Physics Quaid-I-Azam University Islamabad Pakistan Department of Physics Tsinghua University Beijing China University of Virginia Charlottesville Virginia USA Institute of High Energy Physics Beijing China State Key Laboratory of Nuclear Physics and Technology Peking University Beijing China The University of Kansas Lawrence Kansas USA Zhejiang University Hangzhou China Universidad de Los Andes Bogota Colombia Universidad de Antioquia Medellin Colombia University of Split Faculty of Electrical Engineering Mechanical Engineering and Naval Architecture Split Croatia University of Split Faculty of Science Split Croatia Institute Rudjer Boskovic Zagreb Croatia University of Cyprus Nicosia Cyprus Charles University Prague Czech Republic Escuela Politecnica Nacional Quito Ecuador Universidad San Francisco de Quito Quito Ecuador Academy of Scientific Research and Technology of the Arab Republic of Egypt Egyptian Network of High Energy Physics Cairo Egypt National Institute of Chemical Physics and Biophysics Tallinn Estonia Department of Physics University of Helsinki Helsinki Finland Helsinki Institute of Physics Helsinki Finland Lappeenranta University of Technology Lappeenranta Finland IRFU CEA Un

A measurement is reported of the jet mass distribution in hadronic decays of boosted top quarks produced in pp collisions at s=13 TeV. The data were collected with the CMS detector at the LHC and correspond to an integrated luminosity of 35.9 fb−1. The measurement is performed in the lepton+jets channel of tt¯ events, where the lepton is an electron or muon. The products of the hadronic top quark decay t→bW→bqq¯′ are reconstructed as a single jet with transverse momentum larger than 400 GeV. The tt¯ cross section as a function of the jet mass is unfolded at the particle level and used to extract a value of the top quark mass of 172.6±2.5 GeV. A novel jet reconstruction technique is used for the first time at the LHC, which improves the precision by a factor of 3 relative to an earlier measurement. This highlights the potential of measurements using boosted top quarks, where the new technique will enable future precision measurements.

关键词： Top quark Hadron colliders

Belle II vertex detector performance 28

学校读者我要写书评

暂无评论

Belle II vertex detector performance

28th International Workshop on Vertex Detectors, Vertex 2019

作者： Bilka, T. Abudinén, F. Ackermann, K. Ahlburg, P. Aihara, H. Albalawi, M. Alonso, O. Andricek, L. Ayad, R. Aziz, T. Babu, V. Bacher, S. Bahinipati, S. Bai, Y. Barberio, E. Baroncelli, Ti. Baroncelli, To. Basith, A.K. Batignani, G. Bauer, A. Behera, P.K. Bertacchi, V. Bettarini, S. Bhuyan, B. Blanco, R. Bosi, F. Boronat, M. Bosisio, L. Bozek, A. Buchsteiner, F. Camien, C. Caldwell, A. Caria, G. Casarosa, G. Ceccanti, M. Červenkov, D. Chekelian, V. Czank, T. Dash, N. de Nuccio, M. Deschamps, B. Dieguez, A. Dingfelder, J. Doležal, Z. Esperante, D. Fischer, P. Forti, F. Fras, M. Frey, A. Friedl, M. Fuster, J. Gabriel, M. Gadow, K. Gebauer, U. Germic, L. Gessler, T. Getzkow, D. Gioi, L. Glazov, A. Gobbo, B. Gomis, P. Grimaldo, J.A.M. Hara, K. Heck, M. Hemperek, T. Hensel, M. Higuchi, T. Hoek, M. Irmler, C. Ishikawa, A. Jaegle, I. Jeon, H.B. Joo, C. Kaleta, M. Kandra, J. Kambara, N. Kang, K.H. Kapusta, P. Kiesling, C. Kisielewski, B. Kittlinger, D. Klose, D. Kodyš, P. Koffmane, C. Kohriki, T. Koike, S. Komarov, I. Konorov, I. Krivokuca, S. Krüger, H. Kuhr, T. Kühn, W. Kumar, M. Kumar, R. Kvasnička, P. la Licata, C. Lacasta, C. Lalwani, K. Lanceri, L. Lange, J.S. Lautenbach, K. Lee, J.Y. Lee, S.C. Leis, U. Leitl, P. Levit, D. Li, Y. Libby, J. Liemann, G. Liu, Z. Lueck, T. Lütticke, F. Macharski, L. Mammini, P. Mariñas, C. Martini, A. Mayekar, S.N. McCarney, S. Mohanty, G.B. Morii, T. Moser, H.G. Moya, D. Mueller, F.J. Müller, F. Münchow, D. Nakamura, K.R. Nakayama, H. Natkaniec, Z. Niebuhr, C. Ninkovic, J. Onuki, Y. Ostrowicz, W. Packheiser, U. Paladino, A. Paoloni, E. Park, H. Paschen, B. Paul, S. Peric, I. Poblotzki, F. Prasanth, K. Praz, C. Profeti, A. Rabusov, A. Rashevskaya, I. Rao, K.K. Reiter, S.P. Resmi, P.K. Richter, R. Ritter, M. Ritzert, M. Rizzo, G. Rozanska, M. Rummel, S. Sahoo, D. Sanchez, J.G. Santelj, L. Sasaki, J. Sato, N. Scavino, B. Schaller, G. School of Physics University of Melbourne MelbourneVIC3010 Australia Institute of High Energy Physics Austrian Academy of Sciences Vienna1050 Austria Institute of High Energy Physics CAS 19B Yuquan Road Shijingshan District Beijing China Faculty of Mathematics and Physics Charles University Prague121 16 Czech Republic University of Bonn Bonn53115 Germany Justus-Liebig-Universität Gießen Gießen35392 Germany II. Physikalisches Institut Georg-August-Universität Göttingen Göttingen37073 Germany Deutsches Elektronen-Synchrotron Hamburg22607 Germany Institute for Computer Engineering Heidelberg University Heidelberg69117 Germany Karlsruhe Institute of Technology Hermann-von-Helmholtz-Platz 1 Eggenstein-Leopoldshafen Karlsruhe76344 Germany Johannes Gutenberg University Mainz Mainz55099 Germany Ludwig Maximilians University Munich80539 Germany Technical University of Munich Arcisstrasse 21 MunichD-80333 Germany Max Planck Institute for Physics MunichD-80805 Germany Halbleiterlabor der Max-Planck-Gesellschaft Otto-Hahn-Ring 6 MunichD-81739 Germany Indian Institute of Technology Bhubaneswar Satya Nagar India Indian Institute of Technology Madras Chennai600036 India Indian Institute of Technology Guwahati Assam781039 India Malaviya National Institute of Technology Jaipur Jaipur302017 India Punjab Agricultural University Ludhiana141004 India Tata Institute of Fundamental Research Mumbai400005 India Dipartimento di Fisica Università di Pisa PisaI-56127 Italy INFN Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica Università di Trieste TriesteI-34127 Italy INFN Sezione di Trieste TriesteI-34127 Italy University of Tokyo Kashiwa277-8583 Japan Department of Physics Niigata University Niigata950-2181 Japan Department of Physics Tohoku University Sendai980-8578 Japan Department of Physics University of Tokyo Tokyo113-0033 Japan Tsukuba305-0801 Japan Department of Physics Kyungpook National University Daegu702-701

The Belle II experiment at the SuperKEKB accelerator (KEK, Tsukuba, Japan) collected its first e+e− collision data in the spring 2019. The aim of accumulating a 50 times larger data sample than Belle at KEKB, a first generation B-Factory, presents substantial challenges to both the collider and the detector, requiring not only state-of-the-art hardware, but also modern software algorithms for tracking and alignment. The broad physics program requires excellent performance of the vertex detector, which is composed of two layers of DEPFET pixels and four layers of double sided-strip sensors. In this contribution, an overview of the vertex detector of Belle II and our methods to ensure its optimal performance, are described, and the first results and experiences from the first physics run are presented. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0).

关键词：

The mass and galaxy distribution around SZ-selected clusters

学校读者我要写书评

暂无评论

arXiv 2021年

作者： Shin, T. Jain, B. Adhikari, S. Baxter, E.J. Chang, C. Pandey, S. Salcedo, A. Weinberg, D.H. Amsellem, A. Battaglia, N. Belyakov, M. Dacunha, T. Goldstein, S. Kravtsov, A.V. Varga, T.N. Abbott, T.M.C. Aguena, M. Alarcon, A. Allam, S. Amon, A. Andrade-Oliveira, F. Annis, J. Bacon, D. Bechtol, K. Becker, M.R. Bernstein, G.M. Bertin, E. Bocquet, S. Bond, J.R. Brooks, D. Buckley-Geer, E. Burke, D.L. Campos, A. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Chen, R. Choi, A. Costanzi, M. da Costa, L.N. DeRose, J. Desai, S. de Vicente, J. Devlin, M.J. Diehl, H.T. Dietrich, J.P. Dodelson, S. Doel, P. Doux, C. Drlica-Wagner, A. Eckert, K. Elvin-Poole, J. Everett, S. Ferraro, S. Ferrero, I. Ferté, A. Flaugher, B. Frieman, J. Gallardo, P.A. Gatti, M. Gaztanaga, E. Gerdes, D.W. Gruen, D. Gruendl, R.A. Gutierrez, G. Harrison, I. Hartley, W.G. Hill, J.C. Hilton, M. Hinton, S.R. Hollowood, D.L. Hughes, J.P. James, D.J. Jarvis, M. Jeltema, T. Koopman, B.J. Krause, E. Kuehn, K. Kuropatkin, N. Lahav, O. Lima, M. Lokken, M. MacCrann, N. Madhavacheril, M.S. Maia, M.A.G. McCullough, J. McMahon, J. Melchior, P. Menanteau, F. Miquel, R. Mohr, J.J. Moodley, K. Morgan, R. Myles, J. Nati, F. Navarro-Alsina, A. Niemack, M.D. Ogando, R.L.C. Page, L.A. Palmese, A. Partridge, B. Paz-Chinchón, F. Pereira, M.E.S. Pieres, A. Malagón, A.A. Plazas Prat, J. Raveri, M. Rodriguez-Monroy, M. Rollins, R.P. Romer, A.K. Rykoff, E.S. Salatino, M. Sánchez, C. Sanchez, E. Santiago, B. Scarpine, V. Schillaci, A. Secco, L.F. Serrano, S. Sevilla-Noarbe, I. Sheldon, E. Sherwin, B.D. Sifón, C. Smith, M. Soares-Santos, M. Staggs, S.T. Suchyta, E. Swanson, M.E.C. Tarle, G. Thomas, D. To, C. Troxel, M.A. Tutusaus, I. Vavagiakis, E.M. Weller, J. Wollack, E.J. Yanny, B. Yin, B. Zhang, Y. Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Institute for Astronomy University of Hawaii HonoluluHI96822 United States Department of Astronomy Center for Cosmology and AstroParticle Physics Ohio State University ColumbusOH43210 United States Department of Astronomy Cornell University IthacaNY14853 United States Enrico Fermi Institute University of Chicago ChicagoIL60637 United States Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse Garching85748 Germany Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Departamento de Física Matemática Instituto de Física Universidade de São Paulo CP 66318 São Paulo SP05314-970 Brazil Laboratório Interinstitucional de e-Astronomia - LIneA RuaGal. José Cristino 77 Rio de Janeiro RJ20921-400 Brazil Argonne National Laboratory LemontIL60439 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Physics Department University of Wisconsin-Madison MadisonWI53706-1390 United States CNRS UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H4 Canada Dep

We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev-Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope (ACT) Data Release 5 (DR5) and the galaxies from the Dark Energy Survey (DES) Year 3 dataset. With signal-to-noise of 62 (43) for galaxy (weak lensing) profiles over scales of about 0.2 – 20h–1 Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: 1. The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. 2. The full mass profile is also consistent with the simulations;hence it can constrain alternative dark matter models that modify the mass distribution of clusters. 3. The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. This can be used to constrain processes such as quenching and tidal disruption that alter the galaxy distribution inside the halo, and scale-dependent features in the transition regime outside the halo. We measure the dependence of the profile shapes on the galaxy sample, redshift and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation and cosmology are discussed. © 2021, CC BY.

关键词： Galaxies

Synthetic galaxy clusters and observations based on dark energy survey year 3 data

学校读者我要写书评

暂无评论

arXiv 2021年

作者： Varga, T.N. Gruen, D. Seitz, S. MacCrann, N. Sheldon, E. Hartley, W.G. Amon, A. Choi, A. Palmese, A. Zhang, Y. Becker, M.R. McCullough, J. Rozo, E. Rykoff, E.S. To, C. Grandis, S. Bernstein, G.M. Dodelson, S. Eckert, K. Everett, S. Gruendl, R.A. Harrison, I. Herner, K. Rollins, R.P. Sevilla-Noarbe, I. Troxel, M.A. Yanny, B. Zuntz, J. Diehl, H.T. Jarvis, M. Aguena, M. Allam, S. Annis, J. Bertin, E. Bhargava, S. Brooks, D. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Costanzi, M. da Costa, L.N. Pereira, M.E.S. de Vicente, J. Desai, S. Dietrich, J.P. Ferrero, I. Flaugher, B. García-Bellido, J. Gaztanaga, E. Gerdes, D.W. Gschwend, J. Gutierrez, G. Hinton, S.R. Honscheid, K. Jeltema, T. Kuehn, K. Kuropatkin, N. Maia, M.A.G. March, M. Melchior, P. Menanteau, F. Miquel, R. Morgan, R. Myles, J. Paz-Chinchón, F. Plazas, A.A. Romer, A.K. Sanchez, E. Scarpine, V. Schubnell, M. Serrano, S. Smith, M. Soares-Santos, M. Suchyta, E. Swanson, M.E.C. Tarle, G. Thomas, D. Weller, J. Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse Garching85748 Germany Universitäts-Sternwarte Fakultät für Physik Ludwig-Maximilians Universität München Scheinerstr. 1 München81679 Germany Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Department of Applied Mathematics and Theoretical Physics University of Cambridge CambridgeCB3 0WA United Kingdom Brookhaven National Laboratory Bldg 510 UptonNY11973 United States Département de Physique Théorique Center for Astroparticle Physics Université de Genéve 24 quai Ernest Ansermet CH-1211Geneva Switzerland Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Department of Physics University of Arizona TucsonAZ85721 United States Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Physics Carnegie Mellon University PittsburghPA15312 United States Santa Cruz Institute for Particle Physics Santa CruzCA95064 United States Center for Astrophysical Surveys National Center for Supercomputing Applications 1205 West Clark St. UrbanaIL61801 United States Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street UrbanaIL61801 United States Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Jodrell Bank Center for

We develop a novel data-driven method for generating synthetic optical observations of galaxy clusters. In cluster weak lensing, the interplay between analysis choices and systematic effects related to source galaxy selection, shape measurement and photometric redshift estimation can be best characterized in end-to-end tests going from mock observations to recovered cluster masses. To create such test scenarios, we measure and model the photometric properties of galaxy clusters and their sky environments from the Dark Energy Survey Year 3 (DES Y3) data in two bins of cluster richness λ ∈ [30;45), λ ∈ [45;60) and three bins in cluster redshift (z ∈ [0.3;0.35), z ∈ [0.45;0.5) and z ∈ [0.6;0.65). Using deep-field imaging data we extrapolate galaxy populations beyond the limiting magnitude of DES Y3 and calculate the properties of cluster member galaxies via statistical background subtraction. We construct mock galaxy clusters as random draws from a distribution function, and render mock clusters and line-of-sight catalogs into synthetic images in the same format as actual survey observations. Synthetic galaxy clusters are generated from real observational data, and thus are independent from the assumptions inherent to cosmological simulations. The recipe can be straightforwardly modified to incorporate extra information, and correct for survey incompleteness. New realizations of synthetic clusters can be created at minimal cost, which will allow future analyses to generate the large number of images needed to characterize systematic uncertainties in cluster mass measurements. Copyright © 2021, The Authors. All rights reserved.

关键词： Galaxies