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4 results on '"miscellaneous [Cosmology]"'

1. Selection of highly-accreting quasars: Spectral properties of Fe II opt emitters not belonging to extreme Population A

Author

A. del Olmo, Deborah Dultzin, Mary Loli Martínez-Aldama, Mauro D'Onofrio, N. Bon, C. A. Negrete, Edi Bon, Paola Marziani, Ministry of Education, Science and Technological Development (Serbia), Istituto Nazionale di Astrofisica, Universidad Nacional Autónoma de México, Ministerio de Economía y Competitividad (España), European Commission, Agencia Estatal de Investigación (España), National Science Centre (Poland), and Consejo Nacional de Ciencia y Tecnología (México)

Subjects
Active galactic nucleus, absorption lines [Quasars], Astrophysics::High Energy Astrophysical Phenomena, Cosmology: miscellaneous, Population, FOS: Physical sciences, Quasars: supermassive black holes, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 01 natural sciences, Spectral line, Luminosity, emission lines [Quasars], 0103 physical sciences, miscellaneous [Cosmology], Emission spectrum, Galaxies: stellar content, Quasars: absorption lines, Quasars: emission lines, Quasars: general, 010306 general physics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Astronomy and Astrophysics, Quasar, general [Quasars], Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), stellar content [Galaxies], supermassive black holes [Quasars]
Abstract

Context. The quasar class of extreme Population A (xA) (also known as super-Eddington accreting massive black holes, SEAMBHs) has been hailed as potential distance indicators for cosmology. Aims. The aim of this paper is to define tight criteria for their proper identification, starting from the main selection criterion RFeII > 1, and to identify potential intruders that do not meet the selection criteria, which nonetheless have been selected as xA because of the coarseness of automatic searches. The inclusion of the spurious xA sources may dramatically increase the dispersion in the Hubble diagram of quasars, which were obtained from virial luminosity estimates. Methods. We studied a sample of 32 low-z quasars that were originally selected from the seventh data release of the Sloan Digital Sky Survey as xA or SEAMBHs, which have been proved to be almost certainly misclassified sources. All of them show moderate to strong Fe II emission and the large majority show strong absorption features in their spectra which are typical of fairly evolved stellar populations. We performed a simultaneous fit of a host galaxy spectrum, active galactic nucleus (AGN) continuum, FeII template, and emission lines to spectra, using the fitting technique based on ULySS, the full spectrum fitting package. We derived the main accretion parameters (i.e., luminosity, black hole mass, and Eddington ratio) and investigate the relation between host galaxy properties and AGN. Results. For sources in our sample with spectral types that correspond to a relatively low Eddington ratio, we find an overall consistency between HβNC, [O III]λλ4959,5007 line shifts, and the mean stellar velocity obtained from the host galaxy fit (within|60| km s-1). Only one source in our sample qualifies as a xA source. Conclusions. The correct classification of spectra that were contaminated by heavy absorption requires careful determination of the host galaxy spectrum. Contamination and misclassification are not usual in the identification of the xAs, nor at low z or at high z. We find a high fraction of host galaxy spectrum; in half of the sample this is even higher than 40%. When absorption lines are prominent, and the fraction of the host galaxy is high, host galaxy spectrum mimics FeII, which may result in a mistaken identification of FeII spectral features. We have identified several stellar absorption lines that, along with the continuum shape, may lead to an overestimate of RFeII, and therefore to the misclassification of sources as xA sources. © ESO 2020., This research is part of the projects 176001 "Astrophysical spectroscopy of extragalactic objects" and 176003 "Gravitation and the large scale structure of the Universe", funded by Ministry of Education, Science and Technological Development of the Republic of Serbia. PM and MDO acknowledge funding from the INAF PRIN-SKA 2017 program 1.05.01.88.04. PM also acknowledges the Programa de Estancias de Investigacion (PREI) No. DGAP/DFA/2192/2018 of UNAM. A.d.O. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness through grant AYA2016-76682-C3-1-P and from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). ML. M. A. acknowledges financial support of National Science Centre, Poland, grant No. 2017/26/A/ST9/00756 (Maestro 9). DD acknowledges support from grants PAPIIT, UNAM 113719, Mexico D.F. 04510, Mexico. AN acknowledges support from grant CONACyT research fellow -Instituto de Astronomia, UNAM, Mexico D.F. 04510, Mexico. We thank to Pu Du for his help and constructive comments. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/.The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.

Published
2020

2. KiDS-1000 methodology: Modelling and inference for joint weak gravitational lensing and spectroscopic galaxy clustering analysis

Author

J. Zuntz, Fabian Köhlinger, Roman Scoccimarro, Hendrik Hildebrandt, Chieh-An Lin, Angus H. Wright, Martin Crocce, Benjamin Joachimi, Henk Hoekstra, E. Sellentin, Maciej Bilicki, Arun Kannawadi, Konrad Kuijken, Nicola R. Napolitano, J. L. van den Busch, Ariel G. Sánchez, Peter Schneider, Fedor Getman, Catherine Heymans, Marika Asgari, Andrej Dvornik, M. von Wietersheim-Kramsta, Huanyuan Shan, Chris Blake, Benjamin Giblin, Thomas Erben, and Tilman Tröster

Subjects
Data Analysis, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-Scale Structure of Universe, Large-scale structure of Universe, Cosmology: miscellaneous, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Standard deviation, Gravitational lensing: weak, Methods: data analysis, analytical [Methods], 0103 physical sciences, Methods, miscellaneous [Cosmology], Weak, Point estimation, Methods: analytical, data analysis [Methods], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Weak gravitational lensing, Photometric redshift, Gravitational Lensing, Physics, 010308 nuclear & particles physics, Estimator, Astronomy and Astrophysics, Analytical, Statistical, Covariance, Methods. statistical, Galaxy, Cosmology, Miscellaneous, Sampling distribution, Space and Planetary Science, astro-ph.CO, Instrumentation and Methods for Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, weak [Gravitational lensing], Cosmology and Nongalactic Astrophysics, astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Joachimi, B., et al., We present the methodology for a joint cosmological analysis of weak gravitational lensing from the fourth data release of the ESO Kilo-Degree Survey (KiDS-1000) and galaxy clustering from the partially overlapping Baryon Oscillation Spectroscopic Survey (BOSS) and the 2-degree Field Lensing Survey (2dFLenS). Cross-correlations between BOSS and 2dFLenS galaxy positions and source galaxy ellipticities have been incorporated into the analysis, necessitating the development of a hybrid model of non-linear scales that blends perturbative and non-perturbative approaches, and an assessment of signal contributions by astrophysical effects. All weak lensing signals were measured consistently via Fourier-space statistics that are insensitive to the survey mask and display low levels of mode mixing. The calibration of photometric redshift distributions and multiplicative gravitational shear bias has been updated, and a more complete tally of residual calibration uncertainties was propagated into the likelihood. A dedicated suite of more than 20 000 mocks was used to assess the performance of covariance models and to quantify the impact of survey geometry and spatial variations of survey depth on signals and their errors. The sampling distributions for the likelihood and the χ2 goodness-of-fit statistic have been validated, with proposed changes for calculating the effective number of degrees of freedom. The prior volume was explicitly mapped, and a more conservative, wide top-hat prior on the key structure growth parameter S8 = σ8 (ωm/0.3)1/2 was introduced. The prevalent custom of reporting S8 weak lensing constraints via point estimates derived from its marginal posterior is highlighted to be easily misinterpreted as yielding systematically low values of S8, and an alternative estimator and associated credible interval are proposed. Known systematic effects pertaining to weak lensing modelling and inference are shown to bias S8 by no more than 0.1 standard deviations, with the caveat that no conclusive validation data exist for models of intrinsic galaxy alignments. Compared to the previous KiDS analyses, S8 constraints are expected to improve by 20% for weak lensing alone and by 29% for the joint analysis.

Published
2021
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3. Planck 2013 results. XXIII. Isotropy and statistics of the CMB

Author

Olivier Doré, A. Renzi, Luigi Danese, E. P. S. Shellard, C. Hernández-Monteagudo, T. J. Pearson, O. Perdereau, J. Tuovinen, A. Coulais, L. Mendes, Jose Alberto Rubino-Martin, Sabino Matarrese, L. Toffolatti, G. de Zotti, C. Gauthier, Andrea Zonca, A. Curto, R. Fernandez-Cobos, Federico Nati, S. Colombi, Luca Terenzi, C. Combet, Charles R. Lawrence, Anthony Lasenby, M. Ashdown, Sophie Henrot-Versille, R. A. Sunyaev, Jean-François Cardoso, E. Martínez-González, M. Piat, A. Gregorio, F. Boulanger, H. C. Chiang, Paolo Natoli, A. Benoit-Lévy, M. Giard, E. Keihänen, Aurelien A. Fraisse, K. Ganga, L. Montier, Theodore Kisner, Allan Hornstrup, B. P. Crill, H. K. Eriksen, Laura Bonavera, R. V. Sudiwala, F. Pasian, C. A. Oxborrow, V. Stolyarov, Etienne Pointecouteau, M. Cruz, K. Mikkelsen, A. Frejsel, C. Renault, Jose M. Diego, Andrea Zacchei, Peter G. Martin, Rafael Rebolo, Martin Kunz, Alain Benoit, J.-L. Puget, Alessandro Melchiorri, François R. Bouchet, M. Rossetti, S. R. Hildebrandt, Mathieu Remazeilles, L. P. L. Colombo, D. Molinari, Dmitry Novikov, T. R. Jaffe, Reijo Keskitalo, E. Battaner, Andrei V. Frolov, M. Tristram, G. Polenta, M. Linden-Vørnle, Sarah E. Church, Pavel Naselsky, Jon E. Gudmundsson, L. Pagano, Carlo Burigana, Zhiqi Huang, Julien Lesgourgues, J. Knoche, Simon Prunet, M. Migliaccio, R. J. Davis, Tarun Souradeep, P. Bielewicz, L. A. Wade, James R. Fergusson, Daniela Paoletti, Jörg P. Rachen, F. Piacentini, Y. Giraud-Héraud, J.-P. Bernard, Ben Rusholme, Davide Pietrobon, A. Mangilli, F. Pajot, Gianmarco Maggio, Dipak Munshi, George Efstathiou, Francesca Perrotta, Soumen Basak, I. Ristorcelli, D. Herranz, W. Hovest, Torsten A. Enßlin, Monique Arnaud, Calvin B. Netterfield, X. Dupac, J. J. Bock, Peter A. R. Ade, Benjamin D. Wandelt, Julian Borrill, A. Moneti, M. Reinecke, F. Couchot, R. B. Barreiro, B. Van Tent, L. Popa, Serge Gratton, Jussi-Pekka Väliviita, Tuhin Ghosh, G. Patanchon, A. de Rosa, Hans Ulrik Nørgaard-Nielsen, A. J. Banday, F. Paci, N. Mandolesi, F.-X. Désert, E. Pierpaoli, Yabebal Fantaye, Locke D. Spencer, Andrew H. Jaffe, Philip Lubin, R. Leonardi, M. Sandri, S. Galli, L. Perotto, W. A. Holmes, M. Maris, Davide Maino, A. Chamballu, G. W. Pratt, Gianluca Morgante, D. Yvon, F. Cuttaia, P. B. Lilje, Michael Seiffert, Duncan Hanson, Pavan K. Aluri, Valeria Pettorino, Jacques Delabrouille, J. A. Murphy, R. C. Butler, D. L. Harrison, Fabio Finelli, Anna Bonaldi, Michele Liguori, Erminia Calabrese, E. Franceschi, Adam Moss, P. M. McGehee, Hao Liu, Anne Lähteenmäki, D. Santos, S. Galeotta, Guilaine Lagache, M. López-Caniego, Daniel J. Mortlock, Olivier Forni, I. D. Novikov, M.-A. Miville-Deschênes, P. de Bernardis, M. Tomasi, Marco Bersanelli, C. Rosset, Stéphane Plaszczynski, Michael P. Hobson, G. Prézeau, Yashar Akrami, Anthony Challinor, H. Dole, Subhabrata Mitra, J. A. Tauber, M. Savelainen, J. Aumont, F. K. Hansen, A. Ducout, D. Contreras, Marian Douspis, J. P. Zibin, P. Vielva, G. Hurier, Silvia Masi, B. Casaponsa, Nicola Bartolo, M. Frailis, Carlo Baccigalupi, Kevin M. Huffenberger, François Levrier, E. Hivon, Ingunn Kathrine Wehus, M. Tucci, N. Pant, A.-S. Suur-Uski, J. B. Kim, J.-F. Sygnet, Massimiliano Lattanzi, R. D. Davies, Peter Meinhold, Luca Valenziano, K. Benabed, Fabrizio Villa, J. González-Nuevo, J. R. Bond, E. Gjerløw, Alessandro Gruppuso, J. F. Macías-Pérez, W. C. Jones, Aditya Rotti, M. Bucher, Douglas Scott, Graca Rocha, J.-M. Lamarre, S. Donzelli, Radek Stompor, Giorgio Savini, Mika Juvela, A. Catalano, D. Sutton, Tiziana Trombetti, F. Noviello, Krzysztof M. Gorski, Domenico Marinucci, Hannu Kurki-Suonio, P. R. Christensen, A. Mennella, Nabila Aghanim, David L. Clements, G. Roudier, F. Elsner, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, PLANCK, Ade, P, Aghanim, N, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartlett, J, Bartolo, N, Battaner, E, Battye, R, Benabed, K, Benoit, A, Benoit-Levy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, J, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Bridges, M, Bucher, M, Burigana, C, Butler, R, Cardoso, J, Catalano, A, Challinor, A, Chamballu, A, Chary, R, Chiang, H, Chiang, L, Christensen, P, Church, S, Clements, D, Colombi, S, Colombo, L, Couchot, F, Coulais, A, Crill, B, Cruz, M, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, J, Desert, F, Diego, J, Dole, H, Donzelli, S, Dore, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Ensslin, T, Eriksen, H, Fantaye, Y, Fergusson, J, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Frommert, M, Galeotta, S, Ganga, K, Giard, M, Giardino, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, F, Hansen, M, Hanson, D, Harrison, D, Helou, G, Henrot-Versille, S, Hernandez-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihanen, E, Keskitalo, R, Kim, J, Kisner, T, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Laureijs, R, Lawrence, C, Leahy, J, Leonardi, R, Leroy, C, Lesgourgues, J, Liguori, M, Lilje, P, Linden-Vornle, M, Lopez-Caniego, M, Lubin, P, Macias-Perez, J, Maffei, B, Maino, D, Mandolesi, N, Mangilli, A, Marinucci, D, Maris, M, Marshall, D, Martin, P, Martinez-Gonzalez, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Mcewen, J, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mikkelsen, K, Mitra, S, Miville-Deschenes, M, Molinari, D, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Norgaard-Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Oxborrow, C, Paci, F, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Patanchon, G, Peiris, H, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pogosyan, D, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prezeau, G, Prunet, S, Puget, J, Rachen, J, Racine, B, Rath, C, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Rotti, A, Roudier, G, Rubino-Martin, J, Ruiz-Granados, B, Rusholme, B, Sandri, M, Santos, D, Savini, G, Scott, D, Seiffert, M, Shellard, E, Souradeep, T, Spencer, L, Starck, J, Stolyarov, V, Stompor, R, Sudiwala, R, Sureau, F, Sutter, P, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Turler, M, Valenziano, L, Valiviita, J, Van Tent, B, Varis, J, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, Wehus, I, White, M, Wilkinson, A, Yvon, D, Zacchei, A, Zonca, A, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Universidad de Cantabria, Tauber, Jan, Ade, P. A. R., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., Battye, R., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Challinor, A., Chamballu, A., Chary, R. R., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Frommert, M., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hansen, M., Hanson, D., Harrison, D. L., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kim, J., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leahy, J. P., Leonardi, R., Leroy, C., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mangilli, A., Marinucci, D., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Mcewen, J. D., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mikkelsen, K., Mitra, S., Miville Deschênes, M. A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Peiris, H. V., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pogosyan, D., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Racine, B., Räth, C., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rotti, A., Roudier, G., Rubinõ Martín, J. A., Ruiz Granados, B., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Souradeep, T., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sureau, F., Sutter, P., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wehus, I. K., White, M., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A., Anne Lähteenmäki Group, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Department of Physics, Helsinki Institute of Physics, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)

Subjects
Data Analysis, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Cosmic microwave background, Astrophysics, cosmic background radiation, CMB, Cosmic background radiation, 7. Clean energy, Cosmology: observation, Gaussian random field, HEMISPHERICAL POWER ASYMMETRY, Statistics, BACKGROUND ANISOTROPY, observations [Cosmology], Physics, Cosmology: miscellaneou, Astrophysics::Instrumentation and Methods for Astrophysics, CMB cold spot, Computer Science::Computers and Society, cosmic background radiation, cosmology: observations, cosmology: miscellaneous, Physics::Space Physics, Physical Sciences, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Kurtosis, symbols, WMAP DATA, astro-ph.CO, DEPENDENT NON-GAUSSIANITIES, cosmology: miscellaneous, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), education, MINKOWSKI FUNCTIONALS, FOS: Physical sciences, Copernican Principle, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, PRIMORDIAL NON-GAUSSIANITY, NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, DIRECTIONAL SPHERICAL WAVELETS, Cosmology: miscellaneous, Cosmology: observations, Astronomy and Astrophysics, Space and Planetary Science, Non-Gaussianity, miscellaneou [Cosmology], miscellaneous [Cosmology], Forschungsgruppe Komplexe Plasmen, Planck, Settore MAT/07 - Fisica Matematica, Science & Technology, Astronomy and Astrophysic, 115 Astronomy, Space science, MICROWAVE-ANISOTROPY-PROBE, POINT CORRELATION-FUNCTIONS, Settore MAT/06 - Probabilita' e Statistica Matematica, 0201 Astronomical And Space Sciences, COLD SPOT, Skewness, cosmology: observations, cosmology
Abstract

The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We acknowledge the use of resources from the Norewegian national super computing facilities NOTUR. The modal and KSW bispectrum estimator analysis was performed on the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. We further acknowledge the computer resources and technical assistance provided by the Spanish Supercomputing Network nodes at Universidad de Cantabria and Universidad Politecnica de Madrid as well as by the Advanced Computing and e-Science team at IFCA. Some of the results in this paper have been derived using the HEALPix package., The two fundamental assumptions of the standard cosmological model – that the initial fluctuations are statistically isotropic and Gaussian – are rigorously tested using maps of the cosmic microwave background (CMB) anisotropy from the Planck satellite. The detailed results are based on studies of four independent estimates of the CMB that are compared to simulations using a fiducial ΛCDM model and incorporating essential aspects of the Planck measurement process. Deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask choice, and frequency dependence. Many of these anomalies were previously observed in the WMAP data, and are now confirmed at similar levels of significance (about 3σ). However, we find little evidence of non-Gaussianity, with the exception of a few statistical signatures that seem to be associated with specific anomalies. In particular, we find that the quadrupole-octopole alignment is also connected to a low observed variance in the CMB signal. A power asymmetry is now found to persist on scales corresponding to about ‘ = 600 and can be described in the low-‘ regime by a phenomenological dipole modulation model. However, any primordial power asymmetry is strongly scale-dependent and does not extend to arbitrarily small angular scales. Finally, it is plausible that some of these features may be reflected in the angular power spectrum of the data, which shows a deficit of power on similar scales. Indeed, when the power spectra of two hemispheres defined by a preferred direction are considered separately, one shows evidence of a deficit in power, while its opposite contains oscillations between odd and even modes that may be related to the parity violation and phase correlations also detected in the data. Although these analyses represent a step forward in building an understanding of the anomalies, a satisfactory explanation based on physically motivated models is still lacking., European Space Agency, Centre National D'etudes Spatiales, CNRS/INSU-IN2P3-INP (France), Italian Space Agency (ASI), Italian National Research Council, Istituto Nazionale Astrofisica (INAF), National Aeronautics & Space Administration (NASA), United States Department of Energy (DOE), UKSA (UK), Consejo Superior de Investigaciones Cientificas (CSIC), Spanish Government, JA (Spain), RES (Spain), Finnish Funding Agency for Technology & Innovation (TEKES), AoF (Finland), CSC (Finland), Helmholtz Association, German Aerospace Centre (DLR), Max Planck Society, CSA (Canada), DTU Space (Denmark), SER/SSO (Switzerland), RCN (Norway), Science Foundation Ireland, Portuguese Foundation for Science and Technology, European Union (EU), Science & Technology Facilities Council (STFC) ST/G003874/1 ST/H008586/1 ST/K003674/1 ST/L001314/1 ST/M007685/1 ST/I005765/1 ST/K000985/1 ST/K002899/1 ST/K001051/1 ST/J000388/1 ST/I002006/1 ST/J005673/1 ST/H001239/1 ST/J001368/1 ST/K004131/1 ST/K00333X/1 ST/L000768/1 ST/K002805/1 ST/K000977/1 ST/J004812/1

Published
2014
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4. The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths

Author

F. Dodu, S. Leach, J. P. Bernard, S. Ricciardi, L. Toffolatti, B. M. Schaefer, Soumen Basak, François R. Bouchet, A. Da Silva, M. Ashdown, Simon Prunet, Bruce Partridge, G. de Zotti, A. J. Banday, Klaus Dolag, J. Lesgourgues, Marc-Antoine Miville-Deschênes, Matthieu Roman, Roberta Paladini, M. Le Jeune, Jean-Baptiste Melin, Sabino Matarrese, S. Mottet, J. González-Nuevo, Clive Dickinson, R. Piffaretti, Michele Liguori, Franz Elsner, Carlo Baccigalupi, J. F. Macías-Pérez, G. Castex, G. Giardino, Marc Betoule, David L. Clements, Pasquale Mazzotta, J. Aumont, Gilles Faÿ, Marcella Massardi, G. Prézeau, Jacques Delabrouille, L. A. Montier, L. Fauvet, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Planck, European Research Council, Science and Technology Facilities Council (UK), APC - Gravitation (APC-Gravitation), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Mathématiques Appliquées aux Systèmes - EA 4037 (MAS), Ecole Centrale Paris, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PLANCK, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Point source, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, radio continuum: general, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, general [Submillimeter], Cosmic background radiation, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Cosmic infrared background, 0103 physical sciences, miscellaneous [Cosmology], Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, ISM: general, Physics, general [ISM], 010308 nuclear & particles physics, Spinning dust, general [Radio continuum], Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy and Astrophysics, submillimeter: general, general [Galaxies], galaxies: general, Galaxy, Cosmology, Miscellaneous, Cosmology: miscellaneous, Galaxies: general, Radio continuum: general, Submillimeter: general, Space and Planetary Science, Sky, cosmology: miscellaneous, radio continuum: general, submillimeter: general, cosmic background radiation, ISM: general, galaxies: general, symbols, cosmology: miscellaneous, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

J. Delabrouille et al., We present the Planck Sky Model (PSM), a parametric model for generating all-sky, few arcminute resolution maps of sky emission at submillimetre to centimetre wavelengths, in both intensity and polarisation. Several options are implemented to model the cosmic microwave background, Galactic diffuse emission (synchrotron, free-free, thermal and spinning dust, CO lines), Galactic H ii regions, extragalactic radio sources, dusty galaxies, and thermal and kinetic Sunyaev-Zeldovich signals from clusters of galaxies. Each component is simulated by means of educated interpolations/extrapolations of data sets available at the time of the launch of the Planck mission, complemented by state-of-the-art models of the emission. Distinctive features of the simulations are spatially varying spectral properties of synchrotron and dust; different spectral parameters for each point source; modelling of the clustering properties of extragalactic sources and of the power spectrum of fluctuations in the cosmic infrared background. The PSM enables the production of random realisations of the sky emission, constrained to match observational data within their uncertainties. It is implemented in a software package that is regularly updated with incoming information from observations. The model is expected to serve as a useful tool for optimising planned microwave and sub-millimetre surveys and testing data processing and analysis pipelines. It is, in particular, used to develop and validate data analysis pipelines within the Planck collaboration. A version of the software that can be used for simulating the observations for a variety of experiments is made available on a dedicated website. © 2013 ESO., SB has been supported by a postdoctoral grant from the “Physique des deux Infinis” (P2I) Consortium. CD acknowledges an STFC Advanced Fellowship and an ERC IRG grant under the FP7.

Published
2013
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