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arXiv 2019年

作者： Wu, W.L.K. Mocanu, L.M. Ade, P.A.R. Anderson, A.J. Austermann, J.E. Avva, J.S. Beall, J.A. Bender, A.N. Benson, B.A. Bianchini, F. Bleem, L.E. Carlstrom, J.E. Chang, C.L. Chiang, H.C. Citron, R. Moran, C. Corbett Crawford, T.M. Crites, A.T. De Haan, T. Dobbs, M.A. Everett, W. Gallicchio, J. George, E.M. Gilbert, A. Gupta, N. Halverson, N.W. Harrington, N. Henning, J.W. Hilton, G.C. Holder, G.P. Holzapfel, W.L. Hou, Z. Hrubes, J.D. Huang, N. Hubmayr, J. Irwin, K.D. Knox, L. Lee, A.T. Li, D. Lowitz, A. Manzotti, A. McMahon, J.J. Meyer, S.S. Millea, M. Montgomery, J. Nadolski, A. Natoli, T. Nibarger, J.P. Noble, G.I. Novosad, V. Omori, Y. Padin, S. Patil, S. Pryke, C. Reichardt, C.L. Ruhl, J.E. Saliwanchik, B.R. Sayre, J.T. Schaffer, K.K. Sievers, C. Simard, G. Smecher, G. Stark, A.A. Story, K.T. Tucker, C. Vanderlinde, K. Veach, T. Vieira, J.D. Wang, G. Whitehorn, N. Yefremenko, V. Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Institute of Theoretical Astrophysics University of Oslo P.O.Box 1029 Blindern OsloN-0315 Norway Cardiff University CardiffCF10 3XQ United Kingdom Fermi National Accelerator Laboratory MS209 P.O. Box 500 BataviaIL60510 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of California BerkeleyCA94720 United States High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue ArgonneIL60439 United States School of Physics University of Melbourne ParkvilleVIC3010 Australia Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics McGill University 3600 Rue University MontrealQCH3A 2T8 Canada School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban South Africa TAPIR Walter Burke Institute for Theoretical Physics California Institute of Technology 1200 E California Blvd PasadenaCA91125 United States California Institute of Technology MS 249-17 1216 E. California Blvd. PasadenaCA91125 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Canadian Institute for Advanced Research CIFAR Program in Cosmology and Gravity TorontoONM5G 1Z8 Canada Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO80309 United States Harvey Mudd College 301 Platt Blvd. ClaremontCA91711 United States European Southern Observatory Karl-Schwarzschild-Str. 2 Garching bei München85748 Germany Department of Physics University of Colorado BoulderCO80309 Unite

We present a measurement of the cosmic microwave background (CMB) lensing potential using 500 deg2of 150 GHz data from the SPTpol receiver on the South Pole Telescope. The lensing potential is reconstructed with signal-to-noise per mode greater than unity at lensing multipoles L 250, using a quadratic estimator on a combination of CMB temperature and polarization maps. We report measurements of the lensing potential power spectrum in the multipole range of 100 MV= 0.944±0.058 (Stat.)±0.025 (Sys.);restricting to only polarization data, we find APOL= 0.906 ± 0.090 (Stat.) ± 0.040 (Sys.). Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1 σ), and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination. Copyright © 2019, The Authors. All rights reserved.

关键词： Cosmology

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Constraints on cosmological parameters from the 500 deg2SPTpol lensing power spectrum

arXiv

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arXiv 2019年

作者： Bianchini, F. Wu, W.L.K. Ade, P.A.R. Anderson, A.J. Austermann, J.E. Avva, J.S. Beall, J.A. Bender, A.N. Benson, B.A. Bleem, L.E. Carlstrom, J.E. Chang, C.L. Chaubal, P. Chiang, H.C. Citron, R. Moran, C. Corbett Crawford, T.M. Crites, A.T. De Haan, T. Dobbs, M.A. Everett, W. Gallicchio, J. George, E.M. Gilbert, A. Gupta, N. Halverson, N.W. Harrington, N. Henning, J.W. Hilton, G.C. Holder, G.P. Holzapfel, W.L. Hrubes, J.D. Huang, N. Hubmayr, J. Irwin, K.D. Knox, L. Lee, A.T. Li, D. Lowitz, A. Manzotti, A. McMahon, J.J. Meyer, S.S. Millea, M. Mocanu, L.M. Montgomery, J. Nadolski, A. Natoli, T. Nibarger, J.P. Noble, G. Novosad, V. Omori, Y. Padin, S. Patil, S. Pryke, C. Reichardt, C.L. Ruhl, J.E. Saliwanchik, B.R. Sayre, J.T. Schaffer, K.K. Sievers, C. Simard, G. Smecher, G. Stark, A.A. Story, K.T. Tucker, C. Vanderlinde, K. Veach, T. Vieira, J.D. Wang, G. Whitehorn, N. Yefremenko, V. School of Physics University of Melbourne ParkvilleVIC3010 Australia Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Cardiff University CardiffCF10 3XQ United Kingdom Fermi National Accelerator Laboratory MS209 P.O. Box 500 BataviaIL60510 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Colorado BoulderCO80309 United States Department of Physics University of California BerkeleyCA94720 United States High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue ArgonneIL60439 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics McGill University 3600 Rue University MontrealQCH3A 2T8 Canada School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban South Africa University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States TAPIR Walter Burke Institute for Theoretical Physics California Institute of Technology 1200 E California Blvd PasadenaCA91125 United States California Institute of Technology MS 249-17 1216 E. California Blvd. PasadenaCA91125 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Canadian Institute for Advanced Research CIFAR Program in Gravity and the Extreme Universe TorontoONM5G 1Z8 Canada Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO80309 United States Harvey Mudd College 301 Platt Blvd. ClaremontCA91711 United States European Southern Observatory Karl-Schwarzschild-Str. 2 Garching bei München85748 Germany As

We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg2SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO) as well as primary CMB spectra from Planck and SPTpol. The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analysed alone and in combination with Planck full-sky primary CMB data. Within the ΛCDM model, CMB lensing data are primarily sensitive to the amount of large-scale structure as parametrized by σ8Ω0.25m. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on σ8Ω0.25m= 0.593 ± 0.025. Jointly fitting with BAO data, we find σ8= 0.779 ± 0.023, Ωm= 0.368+0.032-0.037, and H0= 72.0+2.1-2.5km s-1Mpc-1, up to 2 s away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. In combination with Planck primary CMB measurements and BAO, the SPTpol lensing spectrum constrains the spatial curvature to be ΩK= -0.0007 ± 0.0025 and the sum of the neutrino masses to be Σmν Copyright © 2019, The Authors. All rights reserved.

关键词： Cosmology

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Measurements of B-mode polarization of the cosmic microwave background from 500 square degrees of SPTpol data

arXiv

引用

arXiv 2019年

作者： Sayre, J.T. Reichardt, Christian L. Henning, J.W. Ade, P.A.R. Anderson, A.J. Austermann, J.E. Avva, J.S. Beall, J.A. Bender, A.N. Benson, B.A. Bianchini, F. Bleem, L.E. Carlstrom, J.E. Chang, C.L. Chiang, H.C. Citron, R. Moran, C. Corbett Crawford, T.M. Crites, A.T. de Haan, T. Dobbs, M.A. Everett, W. Gallicchio, J. George, E.M. Gilbert, A. Gupta, N. Halverson, N.W. Harrington, N. Hilton, G.C. Holder, G.P. Holzapfel, W.L. Hrubes, J.D. Huang, N. Hubmayr, J. Irwin, K.D. Knox, L. Lee, A.T. Li, D. Lowitz, A. McMahon, J.J. Meyer, S.S. Mocanu, L.M. Montgomery, J. Nadolski, A. Natoli, T. Nibarger, J.P. Noble, G. Novosad, V. Padin, S. Patil, S. Pryke, C. Ruhl, J.E. Saliwanchik, B.R. Schaffer, K.K. Sievers, C. Smecher, G. Stark, A.A. Tucker, C. Vanderlinde, K. Veach, T. Vieira, J.D. Wang, G. Whitehorn, N. Wu, W.L.K. Yefremenko, V. Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO80309 United States Department of Physics University of Colorado BoulderCO80309 United States Physics Department Center for Education and Research in Cosmology and Astrophysics Case Western Reserve University ClevelandOH44106 United States School of Physics University of Melbourne ParkvilleVIC3010 Australia High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue ArgonneIL60439 United States Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Cardiff University CardiffCF10 3XQ United Kingdom Fermi National Accelerator Laboratory MS209 P.O. Box 500 BataviaIL60510 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of California BerkeleyCA94720 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics McGill University 3600 Rue University MontrealQCH3A 2T8 Canada School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban South Africa University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States TAPIR Walter Burke Institute for Theoretical Physics California Institute of Technology 1200 E California Blvd PasadenaCA91125 United States California Institute of Technology MS 249-17 1216 E. California Blvd. PasadenaCA91125 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Canadian Institute for Advanced Research CIFAR Program in Gravity and the Extreme Universe TorontoONM5G 1Z8 Canada Harvey Mudd Col

We report a B-mode power spectrum measurement from the cosmic microwave background (CMB) polarization anisotropy observations made using the SPTpol instrument on the South Pole Telescope. This work uses 500 deg2 of SPTpol data, a five-fold increase over the last SPTpol B-mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: 52 −71, corresponding to a 18.1 σ detection of power. An upper limit is set on the tensor-to-scalar ratio, r lens, the data prefer Alens = 1.17 ± 0.13. These data are currently the most precise measurements of B-mode power at > 320. Copyright © 2019, The Authors. All rights reserved.

关键词： Cosmology

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Fractional polarisation of extragalactic sources in the 500-square-degree SPTpol survey

arXiv

引用

arXiv 2019年

作者： Gupta, N. Reichardt, C.L. Ade, P.A.R. Anderson, A.J. Archipley, M. Austermann, J.E. Avva, J.S. Beall, J.A. Bender, A.N. Benson, B.A. Bianchini, F. Bleem, L.E. Carlstrom, J.E. Chang, C.L. Chiang, H.C. Citron, R. Corbett Moran, C. Crawford, T.M. Crites, A.T. de Haan, T. Dobbs, M.A. Everett, W. Feng, C. Gallicchio, J. George, E.M. Gilbert, A. Halverson, N.W. Harrington, N. Henning, J.W. Hilton, G.C. Holder, G.P. Holzapfel, W.L. Hou, Z. Hrubes, J.D. Huang, N. Hubmayr, J. Irwin, K.D. Knox, L. Lee, A.T. Li, D. Lowitz, A. Luong-Van, D. Marrone, D.P. McMahon, J.J. Meyer, S.S. Mocanu, L.M. Mohr, J.J. Montgomery, J. Nadolski, A. Natoli, T. Nibarger, J.P. Noble, G.I. Novosad, V. Padin, S. Patil, S. Pryke, C. Ruhl, J.E. Saliwanchik, B.R. Sayre, J.T. Schaffer, K.K. Shirokoff, E. Sievers, C. Smecher, G. Staniszewski, Z. Stark, A.A. Story, K.T. Switzer, E.R. Tucker, C. Vanderlinde, K. Veach, T. Vieira, J.D. Wang, G. Whitehorn, N. Williamson, R. Wu, W.L.K. Yefremenko, V. Zhang, L. School of Physics University of Melbourne ParkvilleVIC3010 Australia Cardiff University CardiffCF10 3XQ United Kingdom Fermi National Accelerator Laboratory MS209 P.O. Box 500 BataviaIL60510 United States Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Astronomy Department University of Illinois at Urbana-Champaign 1002 W. Green Street UrbanaIL61801 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of California BerkeleyCA94720 United States High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue ArgonneIL60439 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban South Africa University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States TAPIR Walter Burke Institute for Theoretical Physics California Institute of Technology 1200 E California Blvd PasadenaCA91125 United States California Institute of Technology MS 249-17 1216 E. California Blvd. PasadenaCA91125 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics McGill University 3600 Rue University MontrealQCH3A 2T8 Canada Canadian Institute for Advanced Research CIFAR Program in Cosmology and Gravity TorontoONM5G 1Z8 Canada Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO80309 United States Department of Physics University of Illinois Urbana-Champaign 1110 W. Green Street UrbanaIL61801 United States Harvey Mudd College 3

We study the polarisation properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarised power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarised power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarisation fraction hp2i = [8.9 ± 1.1] × 10−4 at 95 GHz and [6.9 ± 1.1] × 10−4 at 150 GHz for the full sample. This is consistent with the values obtained for a sub-sample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 2> 95 −3 and 2> 150 −3. We find no evidence that the polarisation fraction depends on the source flux or observing frequency. The 1-σ upper limit on measured mean squared polarisation fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarisation power spectra out to at least ` . 5700 (` . 4700) and ` . 5300 (` . 3600), respectively at 95 (150) GHz. Copyright © 2019, The Authors. All rights reserved.

关键词： Polarization

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Equivalent-input-disturbance approach enables sliding-mode control systems to reject unmatched disturbances

Equivalent-input-disturbance approach enables sliding-mode c...

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IEEE International Conference on Industrial Technology (ICIT)

作者： Jinhua She Yaodong Pan Hiroshi Hashimoto Qi Lei Min Wu School of Computer Science Tokyo University of Technology Tokyo Japan School of Information Science and Engineering Central South University Changsha China Honeywell Canada Mississauga ON CA Master Program of Innovation for Design and Engineering Advanced Institute of Industrial Technology Tokyo Japan School of Automation China University of Geosciences Wuhan China

ISBN: (纸本)9781479978014

The incorporation of an equivalent-input-disturbance estimator into a conventional sliding-mode control (SMC) system results in a new structure with improved disturbance rejection performance. This configuration enables an SMC system to reject unmatched disturbances. Simulation results for the positioning control of a dual-stage feed drive show that the method not only rejects unmatched disturbances, but also improves the disturbance rejection performance for matched disturbances, thereby demonstrating the validity of the design.

关键词： Observers Actuators Solids State feedback

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Dark Energy Survey year 1 results: Joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions

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Physical Review D 2019年第2期100卷 023541-023541页

作者： T. M. C. Abbott F. B. Abdalla A. Alarcon S. Allam J. Annis S. Avila K. Aylor M. Banerji N. Banik E. J. Baxter K. Bechtol M. R. Becker B. A. Benson G. M. Bernstein E. Bertin F. Bianchini J. Blazek L. E. Bleem S. L. Bridle D. Brooks E. Buckley-Geer D. L. Burke J. E. Carlstrom A. Carnero Rosell M. Carrasco Kind J. Carretero F. J. Castander R. Cawthon C. Chang C. L. Chang H-M. Cho A. Choi R. Chown T. M. Crawford A. T. Crites M. Crocce C. E. Cunha C. B. D’Andrea L. N. da Costa C. Davis T. de Haan J. DeRose S. Desai J. De Vicente H. T. Diehl J. P. Dietrich M. A. Dobbs S. Dodelson P. Doel A. Drlica-Wagner T. F. Eifler J. Elvin-Poole W. B. Everett B. Flaugher P. Fosalba O. Friedrich J. Frieman J. García-Bellido M. Gatti E. Gaztanaga E. M. George D. W. Gerdes T. Giannantonio D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez N. W. Halverson N. L. Harrington W. G. Hartley G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid Z. Hou B. Hoyle J. D. Hrubes D. Huterer B. Jain D. J. James M. Jarvis T. Jeltema M. W. G. Johnson M. D. Johnson S. Kent D. Kirk L. Knox N. Kokron E. Krause K. Kuehn O. Lahav A. T. Lee E. M. Leitch T. S. Li M. Lima H. Lin D. Luong-Van N. MacCrann M. A. G. Maia A. Manzotti D. P. Marrone J. L. Marshall P. Martini J. J. McMahon F. Menanteau S. S. Meyer R. Miquel L. M. Mocanu J. J. Mohr J. Muir T. Natoli A. Nicola B. Nord Y. Omori S. Padin S. Pandey A. A. Plazas A. Porredon J. Prat C. Pryke M. M. Rau C. L. Reichardt R. P. Rollins A. K. Romer A. Roodman A. J. Ross E. Rozo J. E. Ruhl E. S. Rykoff S. Samuroff C. Sánchez E. Sanchez J. T. Sayre V. Scarpine K. K. Schaffer L. F. Secco S. Serrano I. Sevilla-Noarbe E. Sheldon E. Shirokoff G. Simard M. Smith M. Soares-Santos F. Sobreira Z. Staniszewski A. A. Stark K. T. Story E. Suchyta M. E. C. Swanson G. Tarle D. Thomas M. A. Troxel D. L. Tucker K. Vanderlinde J. D. Vieira P. Vielzeuf V. Vikram A. R. Walker R. H. Wechsler J. Weller R. Williamson W. L. K. Wu B. Yanny O. Zahn Y. Zhang J. Zuntz Cerro Tololo Inter-American Observatory National Optical Astronomy Observatory Casilla 603 La Serena Chile Department of Physics & Astronomy University College London Gower Street London WC1E 6BT United Kingdom Department of Physics and Electronics Rhodes University P.O. Box 94 Grahamstown 6140 South Africa Institut d’Estudis Espacials de Catalunya (IEEC) 08193 Barcelona Spain Institute of Space Sciences (ICE CSIC) Campus UAB Carrer de Can Magrans s/n 08193 Barcelona Spain Fermi National Accelerator Laboratory P.O. Box 500 Batavia Illinois 60510 USA Institute of Cosmology & Gravitation University of Portsmouth Portsmouth PO1 3FX United Kingdom Department of Physics University of California Davis California 95616 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA LSST 933 North Cherry Avenue Tucson Arizona 85721 USA Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA CNRS UMR 7095 Institut d’Astrophysique de Paris F-75014 Paris France Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris F-75014 Paris France School of Physics University of Melbourne Parkville VIC 3010 Australia Center for Cosmology and Astro-Particle Physics The Ohio State University Columbus Ohio 43210 USA Institute of Physics Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland High Energy Physics Division Argonne National Laboratory Argonne Illinois 60439 USA Jodrell Bank Center for Astrophysics School of Physic

We perform a joint analysis of the auto and cross-correlations between three cosmic fields: the galaxy density field, the galaxy weak lensing shear field, and the cosmic microwave background (CMB) weak lensing convergence field. These three fields are measured using roughly 1300 sq. deg. of overlapping optical imaging data from first year observations of the Dark Energy Survey (DES) and millimeter-wave observations of the CMB from both the South Pole Telescope Sunyaev-Zel’dovich survey and Planck. We present cosmological constraints from the joint analysis of the two-point correlation functions between galaxy density and galaxy shear with CMB lensing. We test for consistency between these measurements and the DES-only two-point function measurements, finding no evidence for inconsistency in the context of flat ΛCDM cosmological models. Performing a joint analysis of five of the possible correlation functions between these fields (excluding only the CMB lensing autospectrum) yields S8≡σ8Ωm/0.3=0.782−0.025+0.019 and Ωm=0.260−0.019+0.029. We test for consistency between these five correlation function measurements and the Planck-only measurement of the CMB lensing autospectrum, again finding no evidence for inconsistency in the context of flat ΛCDM models. Combining constraints from all six two-point functions yields S8=0.776−0.021+0.014 and Ωm=0.271−0.016+0.022. These results provide a powerful test and confirmation of the results from the first year DES joint-probes analysis.

关键词： Cosmic microwave background Cosmological parameters Evolution of the Universe Large scale structure of the Universe

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Back Cover: H2S Sensors: Fumarate-Based fcu-MOF Thin Film Grown on a Capacitive Interdigitated Electrode (Angew. Chem. Int. Ed. 51/2016)

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Angewandte Chemie International Edition 2016年第51期55卷

作者： Dr. Omar Yassine Dr. Osama Shekhah Ayalew H. Assen Dr. Youssef Belmabkhout Prof. Khaled N. Salama Prof. Mohamed Eddaoudi Sensors Lab Electrical Engineering Program Division of Computer Electrical and Mathematical Sciences and Engineering King Abdullah University of Science and Technology Thuwal 23955-6900 Saudi Arabia Functional Materials Design Discovery and Development research group (FMD3) Advanced Membranes & Porous Materials Center Division of Physical Sciences and Engineering King Abdullah University of Science and Technology Thuwal 23955-6900 Saudi Arabia

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H2S Sensors: Fumarate‐Based fcu‐MOF Thin Film Grown on a Capacitive Interdigitated Electrode

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Angewandte Chemie 2016年第51期128卷

作者： Omar Yassine Osama Shekhah Ayalew H. Assen Youssef Belmabkhout Khaled N. Salama Mohamed Eddaoudi Sensors Lab Electrical Engineering Program Division of Computer Electrical and Mathematical Sciences and Engineering King Abdullah University of Science and Technology Thuwal 23955-6900 Saudi Arabia Functional Materials Design Discovery and Development research group (FMD3) Advanced Membranes & Porous Materials Center Division of Physical Sciences and Engineering King Abdullah University of Science and Technology Thuwal 23955-6900 Saudi Arabia

Herein we report the fabrication of an advanced sensor for the detection of hydrogen sulfide (H 2 S) at room temperature, using thin films of rare‐earth metal (RE)‐based metal–organic framework (MOF) with underlying fcu topology. This unique MOF‐based sensor is made via the in situ growth of fumarate‐based fcu ‐MOF (fum‐ fcu ‐MOF) thin film on a capacitive interdigitated electrode. The sensor showed a remarkable detection sensitivity for H 2 S at concentrations down to 100 ppb, with the lower detection limit around 5 ppb. The fum‐ fcu ‐MOF sensor exhibits a highly desirable detection selectivity towards H 2 S vs. CH 4 , NO 2 , H 2 , and C 7 H 8 as well as an outstanding H 2 S sensing stability as compared to other reported MOFs.

关键词： H2S Interdigital-Elektroden Metall-organische Gerüstverbindungen Seltenerdmetalle Sensoren

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Rücktitelbild: H2S Sensors: Fumarate‐Based fcu‐MOF Thin Film Grown on a Capacitive Interdigitated Electrode (Angew. Chem. 51/2016)

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Angewandte Chemie 2016年第51期128卷

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The curved surface visualization of the expert behavior for skill transfer using microsoft kinect 11

The curved surface visualization of the expert behavior for ...

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11th International Conference on Informatics in Control, Automation and Robotics, ICINCO 2014

作者： Mitsuhashi, Kaoru Hashimoto, Hiroshi Ohyama, Yasuhiro School of Computer Science Tokyo University of Technology Hachioji Tokyo Japan Master Program of Innovation for Design and Engineering Advanced Institute of Industrial Technology Tokyo Japan

ISBN: (纸本)9789897580406

Method of teaching and inheriting for skill is almost oral. It is not quantitative but qualitative. Quantitative inheriting of skill is difficult. In this paper, after tracking of a subject's skill motion using Microsoft Kinect, a subject's motion is visualized as the curved surface. A curved surface is fitted in the positions of a subject's joint, or the direction of trajectories. Expert and beginner perform swimming and karate motion. After the motions are tracked, the trajectories of joints are transformed to a curved surface. The difference of an action between an expert and a beginner is extracted by investigating curvatures and form on the visualized curved surface. Therefore, we expected that technical skill is transferred easily.

关键词： Visualization

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