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arXiv 2019年

作者： Madhavacheril, Mathew S. Hill, J. Colin Nss, Sigurd Addison, Graeme E. Aiola, Simone Baildon, Taylor Battaglia, Nicholas Bean, Rachel Bond, J. Richard Calabrese, Erminia Calafut, Victoria Choi, Steve K. Darwish, Omar Devlin, Mark J. Dunkley, Joanna Dunner, Rolando Ferraro, Simone Gallardo, Patricio A. Halpern, Mark Han, Dongwon Hasseleld, Matthew Hilton, Matt Hincks, Adam D. Hlozek, Renee Ho, Shuay-Pwu Patty Huffenberger, Kevin M. Hughes, John P. Koopman, Brian J. Kosowsky, Arthur Lokken, Martine Louis, Thibaut Lungu, Marius MacInnis, Amanda Maurin, Loic McMahon, Jeffrey J. Moodley, Kavilan Nati, Federico Niemack, Michael D. Page, Lyman A. Partridge, Bruce Robertson, Naomi Sehgal, Neelima Schaan, Emmanuel Schillaci, Alessandro Sherwin, Blake D. Sifon, Cristobal Simon, Sara M. Spergel, David N. Staggs, Suzanne T. Storer, Emilie R. van Engelen, Alexander Vavagiakis, Eve M. Wollack, Edward J. Xu, Zhilei Centre for the Universe Perimeter Institute for Theoretical Physics WaterlooONN2L2Y5 Canada Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Physics Columbia University 550 West 120th Street New YorkNY10027 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States School of Natural Sciences Institute for Advanced Study PrincetonNJ08540 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Department of Physics University of Michigan Ann Arbor48103 United States Department of Astronomy Cornell University IthacaNY14853 United States Canadian Institute for Theoretical Astrophysics University of Toronto 60 St. George St. TorontoONM5S3H8 Canada School of Physics and Astronomy Cardiff University Parade CardiffCF243AA United Kingdom Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road CambridgeCB30WA United Kingdom Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Instituto de Astrofisica Centro de Astro-Ingenieria Facultad de Fisica Ponticia Universidad Catolica de Chile Av. Vicuna Mackenna 4860 Macul Santiago7820436 Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics Cornell University 109 Clark Hall IthacaNY14853 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T1Z1 Canada Physics and Astronomy Department Stony Brook University Stony BrookNY11794 United States Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Department of A

Optimal analyses of many signals in the cosmic microwave background (CMB) require maplevel extraction of individual components in the microwave sky, rather than measurements at the power spectrum level alone. To date, nearly all map-level component separation in CMB analyses has been performed exclusively using satellite data. In this paper, we implement a component separation method based on the internal linear combination (ILC) approach which we have designed to optimally account for the anisotropic noise (in the 2D Fourier domain) often found in groundbased CMB experiments. Using this method, we combine multi-frequency data from the Planck satellite and the Atacama Cosmology Telescope Polarimeter (ACTPol) to construct the first widearea, arcminute-resolution component-separated maps (covering ≈ 2100 sq. deg.) of the CMB temperature anisotropy and the thermal Sunyaev-Zel'dovich (tSZ) effect sourced by the inverse-Compton scattering of CMB photons off hot, ionized gas. Our ILC pipeline allows for explicit deprojection of various contaminating signals, including a modified blackbody approximation of the cosmic infrared background (CIB) spectral energy distribution. The cleaned CMB maps will be a useful resource for CMB lensing reconstruction, kinematic SZ cross-correlations, and primordial non-Gaussianity studies. The tSZ maps will be used to study the pressure profiles of galaxies, groups, and clusters through cross-correlations with halo catalogs, with dust contamination controlled via CIB deprojection. The data products described in this paper will be made available on LAMBDA. 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

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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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A measurement of the cosmic microwave background lensing potential and power spectrum from 500 deg2of sptpol temperature and polarization data

arXiv

引用

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

arXiv

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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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Planck intermediate results. LV. reliability and thermal properties of high-frequency sources in the second planck catalogue of compact sources

arXiv

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arXiv 2020年

作者： Akrami, Y. Ashdown, M. Aumont, J. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basak, S. Benabed, K. Bernard, J.-P. Bersanelli, M. Bielewicz, P. Bond, J.R. Borrill, J. Bouchet, F.R. Burigana, C. Calabrese, E. Carvalho, P. Chiang, H.C. Crill, B.P. Cuttaia, F. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J.-M. Di Valentino, E. Diego, J.M. Dupac, X. Dusini, S. Efstathiou, G. Elsner, F. Enßlin, T.A. Eriksen, H.K. Fernandez-Cobos, R. Finelli, F. Fraisse, A.A. Franceschi, E. Frolov, A. Galeotta, S. Ganga, K. Gerbino, M. González-Nuevo, J. Górski, K.M. Gratton, S. Gruppuso, A. Gudmundsson, J.E. Handley, W. Hansen, F.K. Herranz, D. Hivon, E. Hobson, M. Huang, Z. Jones, W.C. Keihänen, E. Keskitalo, R. Kim, J. Kisner, T.S. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lamarre, J.-M. Lasenby, A. Lattanzi, M. Lawrence, C.R. Le Jeune, M. Lilje, P.B. Lindholm, V. López-Caniego, M. Ma, Y.-Z. Macías-Pérez, J.F. Maggio, G. Mandolesi, N. Marcos-Caballero, A. Maris, M. Martin, P.G. Martínez-González, E. Matarrese, S. Mauri, N. McEwen, J.D. Migliaccio, M. Molinari, D. Moneti, A. Montier, L. Morgante, G. Natoli, P. Paoletti, D. Partridge, B. Perrotta, F. Pettorino, V. Piacentini, F. Polenta, G. Puget, J.-L. Rachen, J.P. Reinecke, M. Remazeilles, M. Renzi, A. Rocha, G. Roudier, G. Ruiz-Granados, B. Savelainen, M. Scott, D. Sirri, G. Spencer, L.D. Suur-Uski, A.-S. Tauber, J.A. Tavagnacco, D. Tenti, M. Toffolatti, L. Tomasi, M. Trombetti, T. Valiviita, J. van Tent, B. Vielva, P. Villa, F. Wehus, I.K. Zacchei, A. Zonca, A. AIM CEA CNRS Université Paris-Saclay Université Paris-Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France APC AstroParticule et Cosmologie Université Paris Diderot CNRS/IN2P3 CEA/lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France African Institute for Mathematical Sciences 6-8 Melrose Road Muizenberg Cape Town South Africa Astrophysics Group Cavendish Laboratory University of Cambridge J J Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Private Bag X54001 Durban4000 South Africa CITA University of Toronto 60 St. George St. TorontoONM5S 3H8 Canada CMDLABS Cambridge Machines Deep Learning and Bayesian Systems Ltd 22 Wycombe End Beaconsfield BuckinghamshireHP9 1NB United Kingdom CNRS IRAP 9 Av. colonel Roche BP 44346 Toulouse cedex 4F-31028 France California Institute of Technology PasadenaCA United States Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States Département de Physique Théorique Université de Genève 24 Quai E. Ansermet Genève 41211 Switzerland Département de Physique École normale supérieure PSL Research University CNRS 24 rue Lhomond Paris75005 France La Laguna TenerifeE-38206 Spain Departamento de Física Universidad de Oviedo C/ Federico García Lorca 18 Oviedo Spain Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Physics & Astronomy University of British Columbia 6224 Agricultural Road VancouverBC Canada Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics Gustaf Hällströmin katu 2a University of Helsinki Helsinki Finland Department of Physics Princeton University PrincetonNJ United States Dipartimento di Fisica e Astronomia G. Galilei Univ

We describe an extension of the most recent version of the Planck Catalogue of Compact Sources (PCCS2), produced using a new multi-band Bayesian Extraction and Estimation Package (BeeP). BeeP assumes that the compact sources present in PCCS2 at 857 GHz have a dust-like spectral energy distribution (SED), which leads to emission at both lower and higher frequencies, and adjusts the parameters of the source and its SED to fit the emission observed in Planck’s three highest frequency channels at 353, 545, and 857 GHz, as well as the IRIS map at 3000 GHz. In order to reduce confusion regarding diffuse cirrus emission, BeeP’s data model includes a description of the background emission surrounding each source, and it adjusts the confidence in the source parameter extraction based on the statistical properties of the spatial distribution of the background emission. BeeP produces the following three new sets of parameters for each source: (a) fits to a modified blackbody (MBB) thermal emission model of the source;(b) SED-independent source flux densities at each frequency considered;and (c) fits to an MBB model of the background in which the source is embedded. BeeP also calculates, for each source, a reliability parameter, which takes into account confusion due to the surrounding cirrus. This parameter can be used to extract sub-samples of high-frequency sources with statistically well-understood properties. We define a high-reliability subset (BeeP/base), containing 26 083 sources (54.1 % of the total PCCS2 catalogue), the majority of which have no information on reliability in the PCCS2. We describe the characteristics of this specific high-quality subset of PCCS2 and its validation against other data sets, specifically for: the sub-sample of PCCS2 located in low-cirrus areas;the Planck Catalogue of Galactic Cold Clumps (GCC);the Herschel GAMA15-field catalogue;and the temperature- and spectral-index-reconstructed dust maps obtained with Planck’s Generalized Needlet Int

关键词： Extraction

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Bayesian modeling for decentralized UAV control and task allocation

Bayesian modeling for decentralized UAV control and task all...

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AIAA Infotech @ Aerospace 2015

作者： Hening, Sebastian Reguiro, Pedro Teodorescu, Mircea Rodriguez, Abel Nguyen, Nhan Ippolito, Corey Fladeland, Matthew Johnson, Matthew S. University of California Santa Cruz Santa CruzCA95064 United States NASA Ames Research Cente Moffett FieldCA94035 United States Department of Computer Engineering United States Department of Applied Mathematics and Statistics United States Advanced Control and Evolvable Systems Group United States Biospheric Science Branch Earth Science Division United States

ISBN: (数字)9781624103384

ISBN: (纸本)9781624103384

The current research represents a first step towards developing a decentralized network of small autonomous, intelligent and inexpensive unmanned aerial vehicles (UAV), which could be used for a variety of scientific missions where measurements from a distributed network of nodes could signiflcantly improve the assessment. The paper presents an adaptive airborne sensing platform (e.g., UAV) that could be used to fuse the information acquired through multiple sensing modalities (obtained from sensors located close to or inside the phenomena) to monitor environmental processes over space and time. The sensing platform is able to continuously reconflgure its trajectory according to the circumstances (e.g., continuously evolving scientific phenomena) to optimize the location of individual sensing waypoints. As proof of concept and validation, we will apply the proposed sensing approach to monitoring volcanic plumes. The paper focuses on (i) developing a Bayesian statistical method to create sensor fusion algorithms that is used to model the plume and guide the UAV in an optimal way (ii) implementing a distributed task allocation scheme which is able guide all the UAVs efficiently and optimize the UAV paths for various criteria. © 2015, American Institute of Aeronautics and Astronautics Inc. All rights received.

关键词： Unmanned aerial vehicles (UAV)

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Outcomes from the DOE workshop on turbulent flow simulation at the exascale 46

Outcomes from the DOE workshop on turbulent flow simulation ...

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46th AIAA Fluid Dynamics Conference, 2016

作者： Sprague, Michael A. Boldyrev, Stanislav Chang, Choong-Seock Fischer, Paul Grout, Ray Gustafson, William I. Hittinger, Jeffrey A. F. Merzari, Elia Moser, Robert National Renewable Energy Laboratory 15013 DenverWest Parkway GoldenCO80401 United States University of Wisconsin-Madison MadisonWI53706 United States Princeton University PrincetonNJ08543 United States University of Illinois at Urbana-Champaign UrbanaIL61801 United States National Renewable Energy Laboratory GoldenCO80401 United States Pacific Northwest National Laboratory RichlandWA99352 United States Lawrence Livermore National Laboratory LivermoreCA94551 United States Argonne National Laboratory ArgonneIL60439 United States University of Texas at Austin AustinTX78712 United States Computational Science Center 15013 DenverWest Parkway United States Physics Department 1150 University Avenue United States Princeton Plasma Physics Laboratory P.O. Box 451 United States Department of Computer Science 201 North Goodwin Avenue United States Computational Science Center 5013 Denver West Parkway United States Atmospheric Sciences and Global Change Division P.O. Box 999 K9-30 United States Scientific Computing Group Center for Applied Scientific Computing PO Box 808 L-561 United States Mathematics and Computer Science 9700 S. Cass Avenue United States Institute for Computational Engineering and Sciences and Department of Mechanical Engineering 201 East 24th United States

ISBN: (数字)9781624104367

ISBN: (纸本)9781624104367

This paper summarizes the outcomes from the Turbulent Flow Simulation at the Exascale: Opportunities and Challenges Workshop, which was held 4-5 August 2015, and was sponsored by the U.S. Department of Energy (DOE) Office of Advanced Scientific Computing Research (ASCR). The workshop objectives were to define and describe the challenges and opportunities that computing at the exascale will bring to turbulent-flow simulations in applied science and technology. The need for accurate simulation of turbulent flows is evident across the DOE applied-science and engineering portfolios, including combustion, plasma physics, nuclear-reactor physics, wind energy, and atmospheric science. The work-shop brought together experts in turbulent-flow simulation, computational mathematics, and high-performance computing. Building upon previous ASCR workshops on exascale computing, participants defined a research agenda and path forward that will enable scientists and engineers to continually leverage, engage, and direct advances in computational systems on the path to exascale computing. © 2016, American Institute of Aeronautics and Astronautics Inc, AIAA. All rights reserved.

关键词： Turbulent flow

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

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

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

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Absolute change pivot rule for the simplex algorithm

Absolute change pivot rule for the simplex algorithm

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International MultiConference of Engineers and computer Scientists, IMECS 2014

作者： Chankong, Kittiphong Intiyot, Boonyarit Sinapiromsaran, Krung Applied Mathematics and Computational Science Program Department of Mathematics and Computer Science Faculty of Science Chulalongkorn University Bangkok Thailand

ISBN: (纸本)9789881925336

The simplex algorithm is a widely used method for solving a linear programming problem (LP) which is first presented by George B. Dantzig. One of the important steps of the simplex algorithm is applying an appropriate pivot rule, the rule to select the entering variable. An effective pivot rule can lead to the optimal solution of LP with the small number of iterations. In a minimization problem, Dantzig's pivot rule selects an entering variable corresponding to the most negative reduced cost. The concept is to have the maximum improvement in the objective value per unit step of the entering variable. However, in some problems, Dantzig's rule may visit a large number of extreme points before reaching the optimal solution. In this paper, we propose a pivot rule that could reduce the number of such iterations over the Dantzig's pivot rule. The idea is to have the maximum improvement in the objective value function by trying to block a leaving variable that makes a little change in the objective function value as much as possible. Then we test and compare the efficacy of this rule with Dantzig' original rule.

关键词： Linear programming

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