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Crossover between liquidlike and gaslike behavior in CH4 at 400 K

Physical Review E 2017年第5期96卷 052113-052113页

作者： D. Smith M. A. Hakeem P. Parisiades H. E. Maynard-Casely D. Foster D. Eden D. J. Bull A. R. L. Marshall A. M. Adawi R. Howie A. Sapelkin V. V. Brazhkin J. E. Proctor Materials and Physics Research Group School of Computing Science and Engineering University of Salford Manchester M5 4WT United Kingdom School of Mathematics and Physical Sciences University of Hull Hull HU6 7RX United Kingdom European Synchrotron Radiation Facility Beamline ID27 Boîte Postale 220 Grenoble France IMPMC Université Pierre et Marie Curie 4 place Jussieu 75005 Paris France Australian Nuclear Science and Technology Organisation Locked Bag 2001 Kirrawee DC New South Wales 2232 Australia SUPA School of Physics and Centre for Science at Extreme Conditions University of Edinburgh Edinburgh EH9 3JZ United Kingdom Center for High Pressure Science & Technology Advanced Research (HPSTAR) Shanghai 201203 People's Republic of China School of Physics and Astronomy Queen Mary University of London London E1 4NS United Kingdom Institute for High Pressure Physics RAS 108440 Troitsk Moscow Russia Photon Science Institute and School of Electrical and Electronic Engineering The University of Manchester Oxford Road Manchester M13 9PL United Kingdom

We report experimental evidence for a crossover between a liquidlike state and a gaslike state in fluid methane (CH4). This crossover is observed in all of our experiments, up to a temperature of 397 K, 2.1 times the critical temperature of methane. The crossover has been characterized with both Raman spectroscopy and x-ray diffraction in a number of separate experiments, and confirmed to be reversible. We associate this crossover with the Frenkel line—a recently hypothesized crossover in dynamic properties of fluids extending to arbitrarily high pressure and temperature, dividing the phase diagram into separate regions where the fluid possesses liquidlike and gaslike properties. On the liquidlike side the Raman-active vibration increases in frequency linearly as pressure is increased, as expected due to the repulsive interaction between adjacent molecules. On the gaslike side this competes with the attractive van der Waals potential leading the vibration frequency to decrease as pressure is increased.

关键词： Critical phenomena Thermodynamics Fluid planets Liquids Raman spectroscopy X-ray diffraction

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Momentum mapping of continuum-electron wave-packet interference

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Physical Review A 2016年第4期94卷 043419-043419页

作者： Weifeng Yang Huatang Zhang Cheng Lin Jingwen Xu Zhihao Sheng Xiaohong Song Shilin Hu Jing Chen Department of Physics College of Science Shantou University Shantou Guangdong 515063 China CAPT HEDPS and IFSA Collaborative Innovation Center of MoE College of Engineering Peking University Beijing 100084 China Institute of Applied Physics and Computational Mathematics P.O. Box 8009 Beijing 100088 China

We analyze the two-dimensional photoelectron momentum distribution of an Ar atom ionized by midinfrared laser pulses and mainly concentrate on the energy range below 2Up. By using a generalized quantum trajectory Monte Carlo simulation and comparing with the numerical solution of the time-dependent Schrödinger equation, we demonstrate that a profound ringlike pattern coming from the interplay between the intra- and the intercycle interferences of electron trajectories can be observed in the deep tunneling ionization regime. Moreover, we found that the rescattered electrons play a negligible role on the formation of a ringlike interference pattern, and the appearance of the ringlike interference pattern masks the holographic interference structure. Our results provide an appropriate experimental condition for the observation of the photoelectron holography and help to gain physical insight into the corresponding ultrafast electron dynamic process with attosecond temporal resolution.

关键词： Atomic & molecular processes in external fields Multiphoton or tunneling ionization & excitation Quantum Monte Carlo

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Validating semi-analytic models of high-redshift galaxy formation using radiation hydrodynamical simulations

arXiv

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arXiv 2017年

作者： Côté, Benoit Silvia, Devin W. O’Shea, Brian W. Smith, Britton Wise, John H. National Superconducting Cyclotron Laboratory Michigan State University MI48823 United States Konkoly Observatory Research Centre for Astronomy and Earth Sciences Hungarian Academy of Sciences Konkoly Thege Miklos ut 15-17 BudapestH-1121 Hungary Joint Institute for Nuclear Astrophysics Center for the Evolution of the Elements United States Department of Physics and Astronomy Michigan State University MI48823 United States Department of Computational Mathematics Science and Engineering Michigan State University MI48823 United States National Science Foundation Astronomy and Astrophysics United States San Diego Supercomputer Center University of California San DiegoCA92093 United States Center for Relativistic Astrophysics Georgia Institute of Technology 837 State Street AtlantaGA30332 United States

We use a cosmological hydrodynamic simulation calculated with Enzo and the semi-analytic galaxy formation model (SAM) GAMMA to address the chemical evolution of dwarf galaxies in the early universe. The long-term goal of the project is to better understand the origin of metal-poor stars and the formation of dwarf galaxies and the Milky Way halo by cross-validating these theoretical approaches. We combine GAMMA with the merger tree of the most massive galaxy found in the hydrodynamic simulation and compare the star formation rate, the metallicity distribution function (MDF), and the age-metallicity relationship predicted by the two approaches. We found that the SAM can reproduce the global trends of the hydrodynamic simulation. However, there are degeneracies between the model parameters and more constraints (e.g., star formation efficiency, gas flows) need to be extracted from the simulation to isolate the correct semi-analytic solution. Stochastic processes such as bursty star formation histories and star formation triggered by supernova explosions cannot be reproduced by the current version of GAMMA. Non-uniform mixing in the galaxy’s interstellar medium, coming primarily from self-enrichment by local supernovae, causes a broadening in the MDF that can be emulated in the SAM by convolving its predicted MDF with a Gaussian function having a standard deviation of ∼0.2 dex. We found that the most massive galaxy in the simulation retains nearby 100 % of its baryonic mass within its virial radius, which is in agreement with what is needed in GAMMA to reproduce the global trends of the simulation. Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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A multi-scale geometric flow method for molecular structure reconstruction

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computational science and Discovery 2015年第1期8卷

作者： Xu, Guoliang Li, Ming Chen, Chong State Key Laboratory of Scientific and Engineering Computing Institute of Computational Mathematics Academy of Mathematics and Systems Science Beijing100190 China

We have previously reported an L2-gradient flow (L2GF) method for cryo-electron tomography and single-particle reconstruction, which has a reasonably good performance. The aim of this paper is to further upgrade both the computational efficiency and accuracy of the L2GF method. In a finite-dimensional space spanned by the radial basis functions, a minimization problem combining a fourth-order geometric flow with an energy decreasing constraint is solved by a bi-gradient method. The bi-gradient method involves a free parameter As β increases from 0 to 1, the structures of the reconstructed function from coarse to fine are captured. The experimental results show that the proposed method yields more desirable results. © 2015 IOP Publishing Ltd.

关键词： Gradient methods

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The GALAH survey: Velocity fluctuations in the milky way using red clump giants

arXiv

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arXiv 2018年

作者： Khanna, Shourya Sharma, Sanjib Bland-Hawthorn, Joss Hayden, Michael Nataf, David M. Ting, Yuan-Sen Kos, Janez Martell, Sarah Zwitter, Tomaž de Silva, Gayandhi Asplund, Martin Buder, Sven Duong, Ly Lin, Jane Simpson, Jeffrey D. Anguiano, Borja Horner, Jonathan Kafle, Prajwal R. Lewis, Geraint F. Nordlander, Thomas Wyse, Rosemary F.G. Wittenmyer, Robert A. Zucker, Daniel B. Sydney Institute for Astronomy School of Physics University of Sydney A28 NSW2006 Australia Australia Miller Institute UC Berkeley BerkeleyCA94720 United States Center for Astrophysical Sciences Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Institute for Advanced PrincetonNJ08540 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Observatories of the Carnegie Institution of Washington 813 Santa Barbara Street PasadenaCA91101 United States School of Physics University of New South Wales SydneyNSW2052 Australia Faculty of Mathematics and Physics University of Ljubljana Jadranska 19 Ljubljana1000 Slovenia Australian Astronomical Observatory 105 Delhi Rd North RydeNSW2113 Australia Research School of Astronomy & Astrophysics Australian National University ACT2611 Australia Koenigstuhl 17 Heidelberg69117 Germany Department of Astronomy University of Virginia P.O. Box 400325 CharlottesvilleVA22904-4325 United States University of Southern Queensland ToowoombaQld4350 Australia ICRAR University of Western Australia 35 Stirling Highway CrawleyWA6009 Australia University of Southern Queensland Computational Engineering and Science Research Centre ToowoombaQLD4350 Australia Australian Centre for Astrobiology University of New South Wales SydneyNSW2052 Australia

If the Galaxy is axisymmetric and in dynamical equilibrium, we expect negligible fluctuations in the residual line-of-sight velocity field. Recent results using the APOGEE survey find significant fluctuations in velocity for stars in the midplane (|z| −1 on a scale of 2.5 kpc. The existence of such large-scale streaming motions has important implications for determining the Sun’s motion about the Galactic Centre. Using Red Clump stars from GALAH and APOGEE, we map the line-of-sight velocities around the Sun (d−1) after taking into account a few systematics (e.g., volume completeness). Using a flexible axisymmetric model the power-amplitude is further reduced to 6.3 km s−1. Additionally, our simulations show that, in the plane, distances are underestimated for high-mass Red Clump stars which can lead to spurious power-amplitude of about 5.2 km s−1. Taking this into account, we estimate the amplitude of real fluctuations to be −1, about a factor of three less than the APOGEE result. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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25th Annual computational Neuroscience Meeting CNS-2016, Seogwipo City, South Korea, July 2-7, 2016 Abstracts

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BMC NEUROscience 2016年第1期17卷 1-112页

作者： [Anonymous] Computational Neurobiology Laboratory The Salk Institute for Biological Studies San Diego USA UNIC CNRS Gif sur Yvette France The European Institute for Theoretical Neuroscience (EITN) Paris France ATR Computational Neuroscience Laboratories Kyoto Japan Krembil Research Institute University Health Network Toronto Canada Department of Physiology University of Toronto Toronto Canada Department of Medicine (Neurology) University of Toronto Toronto Canada Department of Physics University of New Hampshire Durham USA Department of Neurophysiology Nencki Institute of Experimental Biology Warsaw Poland Department of Theory Wigner Research Centre for Physics of the Hungarian Academy of Sciences Budapest Hungary Department of Mathematical Sciences KAIST Daejoen Republic of Korea Department of Mathematics University of Houston Houston USA Department of Biochemistry & Cell Biology and Institute of Biosciences and Bioengineering Rice University Houston USA Department of Biology and Biochemistry University of Houston Houston USA Grupo de Neurocomputación Biológica Dpto. de Ingeniería Informática Escuela Politécnica Superior Universidad Autónoma de Madrid Madrid Spain Department of Biological Sciences University of Southern California Los Angeles USA Center for Neuroscience Korea Institute of Science and Technology Seoul South Korea Department of Neurology Albert Einstein College of Medicine Bronx USA Center for Neuroscience KIST Seoul South Korea Department of Neuroscience University of Science and Technology Daejon South Korea Systems Neuroscience Group QIMR Berghofer Medical Research Institute Herston Australia Department of Psychology Yonsei University Seoul South Korea Department of Psychiatry Kyung Hee University Hospital at Gangdong Seoul South Korea Department of Psychiatry Veterans Administration Boston Healthcare System and Harvard Medical School Brockton USA Department of Electrical and Electronic Engineering The University of Melbourne Parkvil

A1 Functional advantages of cell-type heterogeneity in neural circuits Tatyana O. Sharpee A2 Mesoscopic modeling of propagating waves in visual cortex Alain Destexhe A3 Dynamics and biomarkers of mental disorders Mitsuo Kawato F1 Precise recruitment of spiking output at theta frequencies requires dendritic h-channels in multi-compartment models of oriens-lacunosum/moleculare hippocampal interneurons Vladislav Sekulić, Frances K. Skinner F2 Kernel methods in reconstruction of current sources from extracellular potentials for single cells and the whole brains Daniel K. Wójcik, Chaitanya Chintaluri, Dorottya Cserpán, Zoltán Somogyvári F3 The synchronized periods depend on intracellular transcriptional repression mechanisms in circadian clocks. Jae Kyoung Kim, Zachary P. Kilpatrick, Matthew R. Bennett, Kresimir Josić O1 Assessing irregularity and coordination of spiking-bursting rhythms in central pattern generators Irene Elices, David Arroyo, Rafael Levi, Francisco B. Rodriguez, Pablo Varona O2 Regulation of top-down processing by cortically-projecting parvalbumin positive neurons in basal forebrain Eunjin Hwang, Bowon Kim, Hio-Been Han, Tae Kim, James T. McKenna, Ritchie E. Brown, Robert W. McCarley, Jee Hyun Choi O3 Modeling auditory stream segregation, build-up and bistability James Rankin, Pamela Osborn Popp, John Rinzel O4 Strong competition between tonotopic neural ensembles explains pitch-related dynamics of auditory cortex evoked fields Alejandro Tabas, André Rupp, Emili Balaguer-Ballester O5 A simple model of retinal response to multi-electrode stimulation Matias I. Maturana, David B. Grayden, Shaun L. Cloherty, Tatiana Kameneva, Michael R. Ibbotson, Hamish Meffin O6 Noise correlations in V4 area correlate with behavioral performance in visual discrimination task Veronika Koren, Timm Lochmann, Valentin Dragoi, Klaus Obermayer O7 Input-location dependent gain modulation in cerebellar nucleus neurons Maria Psarrou, Maria Schilstra, Neil Davey, Benjamin Torben-Ni

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Web Interface for Continuum Modeling of Molecular Solvation and Ion Transport

Web Interface for Continuum Modeling of Molecular Solvation ...

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2015欧亚经济论坛-2015第五届国际纳米科技大会

作者： Benzhuo Lu Institute of Computational Mathematics and Scientific/Engineering Computing Academy of Mathematics and Systems Science Chinese Academy of Sciences

Continuum models(implicit solvent models) are widely applied to simulating molecular solvation and ionic transport in wide ion channels.A web-based graphical user interface(GUI) is presented for simulations of Poisson-Boltzmann electrostatics and Poisson-Nernst-Planck electrodiffusion of ion transport in channel proteins or *** webserver is designed to help users avoid most of the technical difficulties encountered in setting up and simulating complex ***-based 3D finite element/boundary element simulation platforms are built for these simulations,as well as design of *** the case of nanopore,the volume tetrahedral mesh is automatically generated on a web interface through typing a series of parameters describing the nanopore,such as the upper and lower pore radius,membrane thickness and box *** pore can carry surface charge density described as a given *** solvation energies,and the ionic concentration and electric potential profiles,and ionic current in the channel/pore cases can be *** are given for different types of simulations.

关键词： Web Interface for Continuum Modeling of Molecular Solvation and Ion Transport

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GW28-e0638 Systematic Correlation of Environmental Exposure with Lower Extremity Peripheral Artery Disease: An Environment-Wide Association Study

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Journal of the American College of Cardiology 2017年第16期70卷 C180-C180页

作者： Xiaodong Zhuang Yanbo Shen Yue Guo Ao Ni Yunxi Jiang Xueqin Wang Xinxue Liao Cardiology department first affiliated hospital of Sun Yat-Sen University Key Laboratory on Assisted Circulation Ministry of Health Joint Institute of Engineering Sun Yat-Sen University Carnegie Mellon University Department of Statistical Science School of Mathematics and Computational Science Sun Yat-Sen University

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Astro2020 APC white paper project: The simons observatory

arXiv

引用

arXiv 2019年

作者： Abitbol, Maximilian H. Adachi, Shunsuke Ade, Peter Aguirre, James Ahmed, Zeeshan Aiola, Simone Ali, Aamir Alonso, David Alvarez, Marcelo A. Arnold, Kam Ashton, Peter Atkins, Zachary Austermann, Jason Awan, Humna Baccigalupi, Carlo Baildon, Taylor Lizancos, Anton Baleato Barron, Darcy Battaglia, Nick Battye, Richard Baxter, Eric Bazarko, Andrew Beall, James A. Bean, Rachel Beck, Dominic Beckman, Shawn Beringue, Benjamin Bhandarkar, Tanay Bhimani, Sanah Bianchini, Federico Boada, Steven Boettger, David Bolliet, Boris Richard Bond, J. Borrill, Julian Brown, Michael L. Bruno, Sarah Marie Bryan, Sean Calabrese, Erminia Calafut, Victoria Calisse, Paolo Carron, Julien Carl, Fred M. Cayuso, Juan Challinor, Anthony Chesmore, Grace Chinone, Yuji Chluba, Jens Cho, Hsiao-Mei Sherry Choi, Steve Clark, Susan Clarke, Philip Contaldi, Carlo Coppi, Gabriele Cothard, Nicholas F. Coughlin, Kevin Coulton, Will Crichton, Devin Crowley, Kevin D. Crowley, Kevin T. Cukierman, Ari D'Ewart, John M. Dünner, Rolando De Haan, Tijmen Devlin, Mark Dicker, Simon Dober, Bradley Duell, Cody J. Duff, Shannon Duivenvoorden, Adri Dunkley, Jo Bouhargani, Hamza El Errard, Josquin Fabbian, Giulio Feeney, Stephen Fergusson, James Ferraro, Simone Fluxà, Pedro Freese, Katherine Frisch, Josef C. Frolov, Andrei Fuller, George Galitzki, Nicholas Gallardo, Patricio A. Ghersi, Jose Tomas Galvez Gao, Jiansong Gawiser, Eric Gerbino, Martina Gluscevic, Vera Goeckner-Wald, Neil Golec, Joseph Gordon, Sam Gralla, Megan Green, Daniel Grigorian, Arpi Groh, John Groppi, Chris Guan, Yilun Gudmundsson, Jon E. Halpern, Mark Han, Dongwon Hargrave, Peter Harrington, Kathleen Hasegawa, Masaya Hasselfield, Matthew Hattori, Makoto Haynes, Victor Hazumi, Masashi Healy, Erin Henderson, Shawn W. Hensley, Brandon Hervias-Caimapo, Carlos Hill, Charles A. Colin Hill, J. Hilton, Gene Hilton, Matt Hincks, Adam D. Hinshaw, Gary Hložek, Renée Ho, Shirley Ho, Shuay-Pwu Patty Hoang, Thuong D. Hoh, Jonathan Hotinli, Selim C. Huang, Zhiqi Hubmayr, Johannes Huffenberger, Kevin Hughes, John P University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Department of Physics Faculty of Science Kyoto University Kyoto606 Japan School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Kavli Institute for Particle Astrophysics and Cosmology Menlo ParkCA94025 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Department of Physics University of California BerkeleyCA94720 United States Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics University of California San Diego CA92093 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States University of Tokyo Kashiwa277- 8583 Japan Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States NIST Quantum Sensors Group 325 Broadway Mailcode 687.08 BoulderCO80305 United States Department of Physics and Astronomy Rutgers State University of New Jersey PiscatawayNJ08854-8019 United States Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste Padriciano 99 Trieste34149 Italy Department of Physics University of Michigan Ann Arbor48103 United States Kavli Institute for Cosmology Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Institute of Astronomy Madingley Road CambridgeCB3 0HA United Kingdom Department of Physics and Astronomy University of New Mexico AlbuquerqueNM87131 United States Department of Astronomy Cornell University IthacaNY14853 United States Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester Manchester United Kingdom AstroParticule e

The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile that promises to provide breakthrough discoveries in fundamental physics, cosmology, and astrophysics. Supported by the Simons Foundation, the Heising-Simons Foundation, and with contributions from collaborating institutions, SO will see first light in 2021 and start a five year survey in 2022. SO has 287 collaborators from 12 countries and 53 institutions, including 85 students and 90 postdocs. The SO experiment in its currently funded form ('SO-Nominal') consists of three 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT). Optimized for minimizing systematic errors in polarization measurements at large angular scales, the SATs will perform a deep, degree-scale survey of 10% of the sky to search for the signature of primordial gravitational waves. The LAT will survey 40% of the sky with arc-minute resolution. These observations will measure (or limit) the sum of neutrino masses, search for light relics, measure the early behavior of Dark Energy, and refine our understanding of the intergalactic medium, clusters and the role of feedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution of the Planck satellite, and roughly an order of magnitude increase in mapping speed over currently operating ("Stage 3") experiments, SO will measure the CMB temperature and polarization fluctuations to exquisite precision in six frequency bands from 27 to 280 GHz. SO will rapidly advance CMB science while informing the design of future observatories such as CMB-S4. Construction of SO-Nominal is fully funded, and operations and data analysis are funded for part of the planned five-year observations. We will seek federal funding to complete the observations and analysis of SO-Nominal, at the $25M level. The SO has a low risk and cost efficient upgrade path - the 6 m LAT

关键词： Observatories

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Construction of KAGRA: An underground gravitational wave observatory

arXiv

引用

arXiv 2017年

作者： Akutsu, T. Ando, M. Araki, S. Araya, A. Arima, T. Aritomi, N. Asada, H. Aso, Y. Atsuta, S. Awai, K. Baiotti, L. Barton, M.A. Chen, D. Cho, K. Craig, K. DeSalvo, R. Doi, K. Eda, K. Enomoto, Y. Flaminio, R. Fujibayashi, S. Fujii, Y. Fujimoto, M.-K. Fukushima, M. Furuhata, T. Hagiwara, A. Haino, S. Harita, S. Hasegawa, K. Hasegawa, M. Hashino, K. Hayama, K. Hirata, N. Hirose, E. Ikenoue, B. Inoue, Y. Ioka, K. Ishizaki, H. Itoh, Y. Jia, D. Kagawa, T. Kaji, T. Kajita, T. Kakizaki, M. Kakuhata, H. Kamiizumi, M. Kanbara, S. Kanda, N. Kanemura, S. Kaneyama, M. Kasuya, J. Kataoka, Y. Kawaguchi, K. Kawai, N. Kawamura, S. Kawazoe, F. Kim, C. Kim, J. Kim, J.C. Kim, W. Kimura, N. Kitaoka, Y. Kobayashi, K. Kojima, Y. Kokeyama, K. Komori, K. Kotake, K. Kubo, K. Kumar, R. Kume, T. Kuroda, K. Kuwahara, Y. Lee, H.-K. Lee, H.-W. Lin, C.-Y. Liu, Y. Majorana, E. Mano, S. Marchio, M. Matsui, T. Matsumoto, N. Matsushima, F. Michimura, Y. Mio, N. Miyakawa, O. Miyake, K. Miyamoto, A. Miyamoto, T. Miyo, K. Miyoki, S. Morii, W. Morisaki, S. Moriwaki, Y. Muraki, Y. Murakoshi, M. Musha, M. Nagano, K. Nagano, S. Nakamura, K. Nakamura, T. Nakano, H. Nakano, M. Nakano, M. Nakao, H. Nakao, K. Narikawa, T. Ni, W.-T. Nonomura, T. Obuchi, Y. Oh, J.J. Oh, S.-H. Ohashi, M. Ohishi, N. Ohkawa, M. Ohmae, N. Okino, K. Okutomi, K. Ono, K. Ono, Y. Oohara, K. Ota, S. Park, J. Peña Arellano, F.E. Pinto, I.M. Principe, M. Sago, N. Saijo, M. Saito, T. Saito, Y. Saitou, S. Sakai, K. Sakakibara, Y. Sasaki, Y. Sato, S. Sato, T. Sato, Y. Sekiguchi, T. Sekiguchi, Y. Shibata, M. Shiga, K. Shikano, Y. Shimoda, T. Shinkai, H. Shoda, A. Someya, N. Somiya, K. Son, E.J. Starecki, T. Suemasa, A. Sugimoto, Y. Susa, Y. Suwabe, H. Suzuki, T. Tachibana, Y. Tagoshi, H. Takada, S. Takahashi, H. Takahashi, R. Takamori, A. Takeda, H. Tanaka, H. Tanaka, K. Tanaka, T. Tatsumi, D. National Astronomical Observatory of Japan Tokyo181-8588 Japan Graduate School of Science University of Tokyo Tokyo113-0033 Japan Department of Physics Graduate School of Science University of Tokyo Tokyo113-0033 Japan Ibaraki305-0801 Japan Earthquake Research Institute University of Tokyo Tokyo113-0032 Japan Department of Physics Graduate School of Science Osaka City University Osaka558-8585 Japan Graduate School of Science and Technology Hirosaki University Aomori036-8561 Japan Department of Physics Graduate School of Science and Engineering Tokyo Institute of Technology Tokyo152-8551 Japan Institute for Cosmic Ray Research University of Tokyo Chiba277-8582 Japan Institute for Cosmic Ray Research University of Tokyo Gifu506-1205 Japan Graduate School of Science Osaka University Osaka560-0043 Japan Department of Physics Sogang University Seoul121-742 Korea Republic of University of Sannio at Benevento BeneventoI-82100 Italy Sezione di Napoli NapoliI-80126 Italy University of Toyama Toyama930-8555 Japan Department of Physics Graduate School of Science Kyoto University Kyoto606-8502 Japan Institute of Physics Academia Sinica Taipei11529 Taiwan University of Toyama Toyama930-8555 Japan Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan Albert-Einstein-Institut Max-Planck-Institut für Gravitationsphysik HannoverD-30167 Germany Department of Physics and Astronomy Seoul National University Seoul151-742 Korea Republic of Daejeon34055 Korea Republic of Department of Physics Myongji University Yongin449-728 Korea Republic of Department of Computer Simulation Inje University Gimhae-shi50834 Korea Republic of Daejeon34047 Korea Republic of Department of Physical Science Graduate School of Science Hiroshima University Hiroshima903-0213 Japan Department of Applied Physics Graduate School of Science Fukuoka University Fukuoka814-0180 Japan Graduate School of Science and Engineer

Major construction and initial-phase operation of a second-generation gravitational-wave detector KAGRA has been completed. The entire 3-km detector is installed underground in a mine in order to be isolated from background seismic vibrations on the surface. This allows us to achieve a good sensitivity at low frequencies and high stability of the detector. Bare-bones equipment for the interferometer operation has been installed and the first test run was accomplished in March and April of 2016 with a rather simple configuration. The initial configuration of KAGRA is named iKAGRA. In this paper, we summarize the construction of KAGRA, including the study of the advantages and challenges of building an underground detector and the operation of the iKAGRA interferometer together with the geophysics interferometer that has been constructed in the same tunnel. Copyright © 2017, The Authors. All rights reserved.

关键词： Interferometers

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