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165 results on '"J. González-Nuevo"'

1. The bright extragalactic ALMA redshift survey (BEARS) – II. Millimetre photometry of gravitational lens candidates

Author: G J Bendo, S A Urquhart, S Serjeant, T Bakx, M Hagimoto, P Cox, R Neri, M D Lehnert, H Dannerbauer, A Amvrosiadis, P Andreani, A J Baker, A Beelen, S Berta, E Borsato, V Buat, K M Butler, A Cooray, G De Zotti, L Dunne, S Dye, S Eales, A Enia, L Fan, R Gavazzi, J González-Nuevo, A I Harris, C N Herrera, D H Hughes, D Ismail, B M Jones, K Kohno, M Krips, G Lagache, L Marchetti, M Massardi, H Messias, M Negrello, A Omont, I Pérez-Fournon, D A Riechers, D Scott, M W L Smith, F Stanley, Y Tamura, P Temi, P van der Werf, A Verma, C Vlahakis, A Weiß, C Yang, and A J Young
Published: 2022
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2. The bright extragalactic ALMA redshift survey (BEARS) I: redshifts of bright gravitationally lensed galaxies from the Herschel ATLAS

Author: S A Urquhart, G J Bendo, S Serjeant, T Bakx, M Hagimoto, P Cox, R Neri, M Lehnert, C Sedgwick, C Weiner, H Dannerbauer, A Amvrosiadis, P Andreani, A J Baker, A Beelen, S Berta, E Borsato, V Buat, K M Butler, A Cooray, G De Zotti, L Dunne, S Dye, S Eales, A Enia, L Fan, R Gavazzi, J González-Nuevo, A I Harris, C N Herrera, D Hughes, D Ismail, R Ivison, S Jin, B Jones, K Kohno, M Krips, G Lagache, L Marchetti, M Massardi, H Messias, M Negrello, A Omont, I Perez-Fournon, D A Riechers, D Scott, M W L Smith, F Stanley, Y Tamura, P Temi, C Vlahakis, A Weiß, P van der Werf, A Verma, C Yang, and A J Young
Published: 2022
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3. Astrophysical and Cosmological Information from Large-scale sub-mm Surveys of Extragalactic Sources

Author: Negrello, M., Perrotta, F., Gonzalez, J. Gonzalez-Nuevo, Silva, L., De Zotti, G., Granato, G. L., Baccigalupi, C., and Danese, L.
Subjects: Astrophysics
Abstract: We present a quantitative analysis of the astrophysical and cosmological information that can be extracted from the many important wide-area, shallow surveys that will be carried out in the next few years. Our calculations combine the predictions of the physical model by Granato et al. (2004) for the formation and evolution of spheroidal galaxies with up-to-date phenomenological models for the evolution of starburst and normal late-type galaxies and of radio sources. We compute the expected number counts and the redshift distributions of these source populations separately and then focus on proto-spheroidal galaxies. For the latter objects we predict the counts and redshift distributions of strongly lensed sources at 250, 350, 500, and 850 micron, the angular correlation function of sources detected in the surveys considered, the angular power spectra due to clustering of sources below the detection limit in Herschel and Planck surveys. An optimal survey for selecting strongly lensed proto-spheroidal galaxies is described, and it is shown how they can be easily distinguished from the other source populations. We also discuss the detectability of the imprints of the 1-halo and 2-halo regimes on angular correlation functions and clustering power spectra, as well as the constraints on cosmological parameters that can be obtained from the determinations of these quantities. The novel data relevant to derive the first sub-millimeter estimates of the local luminosity functions of starburst and late-type galaxies, and the constraints on the properties of rare source populations, such as blazars, are also briefly described., Comment: 16 pages, 10 figures. Accepted for publication on MNRAS
Published: 2007
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4. Bright Extragalactic ALMA Redshift Survey (BEARS) III: Detailed study of emission lines from 71 Herschel targets

Author: M Hagimoto, T J L C Bakx, S Serjeant, G J Bendo, S A Urquhart, S Eales, K C Harrington, Y Tamura, H Umehata, S Berta, A R Cooray, P Cox, G De Zotti, M D Lehnert, D A Riechers, D Scott, P Temi, P P van der Werf, C Yang, A Amvrosiadis, P M Andreani, A J Baker, A Beelen, E Borsato, V Buat, K M Butler, H Dannerbauer, L Dunne, S Dye, A F M Enia, L Fan, R Gavazzi, J González-Nuevo, A I Harris, C N Herrera, D H Hughes, D Ismail, R J Ivison, B Jones, K Kohno, M Krips, G Lagache, L Marchetti, M Massardi, H Messias, M Negrello, R Neri, A Omont, I Perez-Fournon, C Sedgwick, M W L Smith, F Stanley, A Verma, C Vlahakis, B Ward, C Weiner, A Weiß, and A J Young
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We analyse the molecular and atomic emission lines of 71 bright Herschel-selected galaxies between redshifts 1.4 to 4.6 detected by the Atacama Large Millimetre/submillimetre Array. These lines include a total of 156 CO, [C I], and H2O emission lines. For 46 galaxies, we detect two transitions of CO lines, and for these galaxies we find gas properties similar to those of other dusty star-forming galaxy (DSFG) samples. A comparison to photo-dissociation models suggests that most of Herschel-selected galaxies have similar interstellar medium conditions as local infrared-luminous galaxies and high-redshift DSFGs, although with denser gas and more intense far-ultraviolet radiation fields than normal star-forming galaxies. The line luminosities agree with the luminosity scaling relations across five orders of magnitude, although the star-formation and gas surface density distributions (i.e., Schmidt-Kennicutt relation) suggest a different star-formation phase in our galaxies (and other DSFGs) compared to local and low-redshift gas-rich, normal star-forming systems. The gas-to-dust ratios of these galaxies are similar to Milky Way values, with no apparent redshift evolution. Four of 46 sources appear to have CO line ratios in excess of the expected maximum (thermalized) profile, suggesting a rare phase in the evolution of DSFGs. Finally, we create a deep stacked spectrum over a wide rest-frame frequency (220-890 GHz) that reveals faint transitions from HCN and CH, in line with previous stacking experiments., Comment: 30 pages, 17 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society Main Journal. Comments are warmly welcomed
Published: 2023
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5. Planck 2018 results

Author: Antony Lewis, X. Dupac, James R. Fergusson, François R. Bouchet, Diego Molinari, E. Martínez-González, Jean-François Cardoso, L. Salvati, Jörg P. Rachen, Krzysztof M. Gorski, K. Ganga, A. Marcos-Caballero, C. Combet, Hannu Kurki-Suonio, E. Di Valentino, Jose M. Diego, L. Montier, Jan Hamann, J. F. Macías-Pérez, E. Franceschi, Charles R. Lawrence, M. Douspis, Erminia Calabrese, E. P. S. Shellard, Frederico Arroja, M. Le Jeune, P. Vielva, Andrea Zacchei, Graca Rocha, Martina Gerbino, Zhiqi Huang, Davide Maino, Adam Moss, Ricardo Genova-Santos, D. Tavagnacco, M. López-Caniego, A. A. Fraisse, M. Tenti, F. Piacentini, J.-P. Bernard, P. de Bernardis, Tiziana Trombetti, L. Toffolatti, Soumen Basak, F. Elsner, J.-L. Puget, Benjamin D. Wandelt, Julian Borrill, R. B. Barreiro, Gabriel Jung, Michele Liguori, S. Galeotta, Will Handley, F. Cuttaia, G. Polenta, R. C. Butler, K. Kiiveri, Anthony Lasenby, Alessandro Melchiorri, Reijo Keskitalo, A. J. Banday, M.-A. Miville-Deschênes, A. Renzi, P. Bielewicz, F. Oppizzi, Yashar Akrami, Anthony Challinor, B. Casaponsa, E. Keihänen, Gianmarco Maggio, B. P. Crill, Nicola Bartolo, B. Van Tent, Fabrizio Villa, Francesca Perrotta, F. K. Hansen, J. B. Kim, G. Sirri, Andrei V. Frolov, Michele Maris, J. A. Tauber, M. Savelainen, D. Herranz, A.-S. Suur-Uski, Yabebal Fantaye, Sabino Matarrese, M. Migliaccio, M. Tomasi, M. Bucher, Nicola Vittorio, J. Valiviita, V. Lindholm, W. C. Jones, Douglas Scott, R. Fernandez-Cobos, D. Paoletti, Marco Bersanelli, Torsten A. Enßlin, A. Moneti, M. Frailis, Carlo Baccigalupi, V. Pettorino, François Levrier, E. Hivon, J. Aumont, B. Racine, A. Mennella, G. Patanchon, Alessandro Gruppuso, Ingunn Kathrine Wehus, M. Reinecke, J.-M. Delouis, P. D. Meerburg, Massimiliano Lattanzi, Jose Alberto Rubino-Martin, N. Mandolesi, Chiara Sirignano, Kendrick M. Smith, Andrew H. Jaffe, Peter Meinhold, J.-M. Lamarre, A. de Rosa, G. de Zotti, B. Partridge, J. González-Nuevo, A. Ducout, Locke D. Spencer, M. Ashdown, H. K. Eriksen, Martin Kunz, Mathieu Remazeilles, Jon E. Gudmundsson, L. P. L. Colombo, Jason D. McEwen, Mario Ballardini, Peter G. Martin, George Efstathiou, Serge Gratton, Carlo Burigana, Nicoletta Krachmalnicoff, Yin-Zhe Ma, Jacques Delabrouille, Fabio Finelli, L. Pagano, N. Mauri, S. Dusini, Andrea Zonca, R. A. Sunyaev, P. B. Lilje, Luca Stanco, H. C. Chiang, K. Benabed, J. R. Bond, B. Ruiz-Granados, O. Doré, Paolo Natoli, Maresuke Shiraishi, Moritz Münchmeyer, S. Galli, Gianluca Morgante, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Parma = Università degli studi di Parma [Parme, Italie], Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Patrimoine, Littérature, Histoire (PLH), Université Toulouse - Jean Jaurès (UT2J), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidade Aberta [Lisboa], Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratory for Phytosanitary Diagnostics and Forecasts, All-Russian Institute for Plant Protection, Russian Academy of Sciences [Moscow] (RAS), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), ICRA and Physics Department, Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, University of Cambridge [UK] (CAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de neurobiologie cellulaire et moléculaire (NBCM), Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Department of Physics, Helsinki Institute of Physics, Universidad de Cantabria, Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), High-Energy Frontier, Van Swinderen Institute for Particle Physics and G, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Università degli studi di Parma = University of Parma (UNIPR), Université de Toulouse (UT)-Université de Toulouse (UT), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Y. Akrami, F. Arroja, M. Ashdown, J. Aumont, C. Baccigalupi, M. Ballardini, A. J. Banday, R. B. Barreiro, N. Bartolo, S. Basak, K. Benabed, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. R. Bond, J. Borrill, F. R. Bouchet, M. Bucher, C. Burigana, R. C. Butler, E. Calabrese, J. -F. Cardoso, B. Casaponsa, A. Challinor, H. C. Chiang, L. P. L. Colombo, C. Combet, B. P. Crill, F. Cuttaia, P. de Bernardi, A. de Rosa, G. de Zotti, J. Delabrouille, J. -M. Deloui, E. Di Valentino, J. M. Diego, O. Doré, M. Douspi, A. Ducout, X. Dupac, S. Dusini, G. Efstathiou, F. Elsner, T. A. Enßlin, H. K. Eriksen, Y. Fantaye, J. Fergusson, R. Fernandez-Cobo, F. Finelli, M. Fraili, A. A. Fraisse, E. Franceschi, A. Frolov, S. Galeotta, K. Ganga, R. T. Génova-Santo, M. Gerbino, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gruppuso, J. E. Gudmundsson, J. Hamann, W. Handley, F. K. Hansen, D. Herranz, E. Hivon, Z. Huang, A. H. Jaffe, W. C. Jone, G. Jung, E. Keihänen, R. Keskitalo, K. Kiiveri, J. Kim, N. Krachmalnicoff, M. Kunz, H. Kurki-Suonio, J. -M. Lamarre, A. Lasenby, M. Lattanzi, C. R. Lawrence, M. Le Jeune, F. Levrier, A. Lewi, M. Liguori, P. B. Lilje, V. Lindholm, M. López-Caniego, Y. -Z. Ma, J. F. Macías-Pérez, G. Maggio, D. Maino, N. Mandolesi, A. Marcos-Caballero, M. Mari, P. G. Martin, E. Martínez-González, S. Matarrese, N. Mauri, J. D. McEwen, P. D. Meerburg, P. R. Meinhold, A. Melchiorri, A. Mennella, M. Migliaccio, M. -A. Miville-Deschêne, D. Molinari, A. Moneti, L. Montier, G. Morgante, A. Mo, M. Münchmeyer, P. Natoli, F. Oppizzi, L. Pagano, D. Paoletti, B. Partridge, G. Patanchon, F. Perrotta, V. Pettorino, F. Piacentini, G. Polenta, J. -L. Puget, J. P. Rachen, B. Racine, M. Reinecke, M. Remazeille, A. Renzi, G. Rocha, J. A. Rubiño-Martín, B. Ruiz-Granado, L. Salvati, M. Savelainen, D. Scott, E. P. S. Shellard, M. Shiraishi, C. Sirignano, G. Sirri, K. Smith, L. D. Spencer, L. Stanco, R. Sunyaev, A. -S. Suur-Uski, J. A. Tauber, D. Tavagnacco, M. Tenti, L. Toffolatti, M. Tomasi, T. Trombetti, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, B. D. Wandelt, I. K. Wehu, A. Zacchei, A. Zonca, 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)
Subjects: High Energy Physics - Theory, cosmological model, Astronomy, Cosmic microwave background, POLARIZATION ANISOTROPIES, cosmic background radiation: polarization, Astrophysics, cosmic background radiation, Cosmic background radiation, Early Universe, 01 natural sciences, 7. Clean energy, expansion: multipole, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), cosmology: theory, 3-POINT CORRELATION-FUNCTION, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, TEMPERATURE, Physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, formation, hep-ph, early Universe, CMB cold spot, inflation: model, High Energy Physics - Phenomenology, scale dependence, non-Gaussianity, symbols, Sunyaev-Zel'dovich effect, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], astro-ph.CO, Trispectrum, Astrophysics - Cosmology and Nongalactic Astrophysics, Particle physics, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, gr-qc, FOS: Physical sciences, PREDICTIONS, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Sunyaev–Zel'dovich effect, Separable space, NO, isocurvature, symbols.namesake, trispectrum, Settore FIS/05 - Astronomia e Astrofisica, parity: violation, gravitation: lens, statistical analysis, theory [Cosmology], Non-Gaussianity, 0103 physical sciences, BISPECTRUM, INFRARED BACKGROUND ANISOTROPIES, structure, bispectrum: scale dependence, Planck, cosmic background radiation: bispectrum, inflation, FAST ESTIMATOR, numerical calculations, non-Gaussianity: primordial, 010308 nuclear & particles physics, ISOCURVATURE PERTURBATIONS, Astronomy and Astrophysics, stability, 115 Astronomy, Space science, Inflation, methods: data analysis, boundary condition, cosmic background radiation: temperature, Cosmology: observations, Cosmology: theory, Methods: data analysis, High Energy Physics - Theory (hep-th), 13. Climate action, Space and Planetary Science, axion, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], cosmology: observations, Cosmic background radiation, Cosmology: observations, Cosmology: theory, Early Universe, Inflation, Methods: data analysis, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Bispectrum
Abstract: Planck Collaboration: et al., arXiv:1905.05697v1, We analyse the Planck full-mission cosmic microwave background (CMB) temperature and E-mode polarization maps to obtain constraints on primordial non-Gaussianity (NG). We compare estimates obtained from separable template-fitting, binned, and optimal modal bispectrum estimators, finding consistent values for the local, equilateral, and orthogonal bispectrum amplitudes. Our combined temperature and polarization analysis produces the following final results: fNLlocal = −0.9 ± 5.1; fNLequil = −26 ± 47; and fNLortho = −38 ± 24 (68% CL, statistical). These results include low-multipole (4 ≤ ℓ < 40) polarization data that are not included in our previous analysis. The results also pass an extensive battery of tests (with additional tests regarding foreground residuals compared to 2015), and they are stable with respect to our 2015 measurements (with small fluctuations, at the level of a fraction of a standard deviation, which is consistent with changes in data processing). Polarization-only bispectra display a significant improvement in robustness; they can now be used independently to set primordial NG constraints with a sensitivity comparable to WMAP temperature-based results and they give excellent agreement. In addition to the analysis of the standard local, equilateral, and orthogonal bispectrum shapes, we consider a large number of additional cases, such as scale-dependent feature and resonance bispectra, isocurvature primordial NG, and parity-breaking models, where we also place tight constraints but do not detect any signal. The non-primordial lensing bispectrum is, however, detected with an improved significance compared to 2015, excluding the null hypothesis at 3.5σ. Beyond estimates of individual shape amplitudes, we also present model-independent reconstructions and analyses of the Planck CMB bispectrum. Our final constraint on the local primordial trispectrum shape is gNLlocal = (−5.8 ± 6.5) × 104 (68% CL, statistical), while constraints for other trispectrum shapes are also determined. Exploiting the tight limits on various bispectrum and trispectrum shapes, we constrain the parameter space of different early-Universe scenarios that generate primordial NG, including general single-field models of inflation, multi-field models (e.g. curvaton models), models of inflation with axion fields producing parity-violation bispectra in the tensor sector, and inflationary models involving vector-like fields with directionally-dependent bispectra. Our results provide a high-precision test for structure-formation scenarios, showing complete agreement with the basic picture of the ΛCDM cosmology regarding the statistics of the initial conditions, with cosmic structures arising from adiabatic, passive, Gaussian, and primordial seed perturbations., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, 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 ERC and PRACE (EU).
Published: 2020

6. Supernova model discrimination with hyper-kamiokande

Author: Y. Nagao, H. Tanaka, A. Minamino, B. Navarro-Garcia, Z. Xie, L. Nascimento Machado, J. Lagoda, M. Shinoki, S. Cuen-Rochin, Arman Esmaili, F. Ballester, S. Parsa, N. McCauley, Jung-Hyun Kim, K. Frankiewicz, L. L. Kormos, Masaki Ishitsuka, M. Malek, V. Valentino, N. Kazarian, T. Wachala, E. Drakopoulou, G. Grella, V. Paolone, L. F. Thompson, A. K. Tomatani-Sánchez, A. Blanchet, R. A. Wendell, John Ellis, J. Y. Kim, N. W. Prouse, O. V. Mineev, M. R. Vagins, T. Boschi, T. Lindner, J. González-Nuevo, Hiroshi Ito, N. Skrobova, M. La Commara, L. Gialanella, F. Orozco-Luna, T. Kumita, A. Garfagnini, S. H. Jeon, A. Dergacheva, Hiroaki Menjo, A. T. Suzuki, K. Okamoto, C. E. R. Naseby, J. F. Martin, T. Iijima, M. Mezzetto, G. Ricciardi, J. R. Wilson, P. Gumplinger, Y. Takemoto, G. Galinski, K. Zaremba, T. Nakadaira, D. Vivolo, A. Carroll, C. Vilela, A. Blondel, A. Rychter, T. A. Doyle, C. Garde, G. De Rosa, A. Oshlianskyi, Hiroyuki Sekiya, R. Matsumoto, G. Pastuszak, P. J. Rajda, F. Monrabal, Yoichi Asaoka, G. Díaz López, K. L. Stankevich, C. D. Shin, Y. Fukuda, Yuto Ashida, Michal Malinský, T. Suganuma, B. Radics, Kohta Murase, Marco Grassi, P. Mehta, F. Cafagna, Ahmed Ali, L. Koerich, Vincenzo Berardi, Etam Noah, F. J. P. Soler, Alan Cosimo Ruggeri, M. Kekic, G. Vasseur, S. Wronka, M. Thiesse, B. Ferrazzi, K. Iwamoto, Yu. Kudenko, Atsushi Takeda, Kendall Mahn, David Hadley, B. Roskovec, M. Bergevin, A. Korzenev, J.J. Gómez-Cadenas, M. Batkiewicz-Kwasniak, M. Tzanov, M. Ikeda, Federico Sanchez, W. Obrębski, H. S. Jo, Y. Takeuchi, Piotr Kalaczyński, S. Chakraborty, J. C. Nugent, S. King, P. Paganini, M. Miura, F. Ameli, D. N. Yeum, C. J. Metelko, Akito Araya, T. Kajita, M. Tanaka, I. T. Lim, L. Mellet, S. Y. Kim, S. Bolognesi, A. Bravar, J. S. Jang, D. Svirida, A. Fiorentini, J. Renner, M. Chabera, L. O'Sullivan, V. Herrero, F. Iacob, K. Nakamura, Ko Okumura, Lukasz Stawarz, N. Ogawa, Laura Bonavera, Y. Maekawa, Takatomi Yano, Ll. Marti, H. J. Rose, S. El Hedri, L. Maret, G. Zarnecki, L. Bernard, S. H. Seo, H. Nakamura, H. Ozaki, A. P. Kryukov, A. Popov, Hisakazu Minakata, M. Buizza Avanzini, P. Sarmah, K. Martens, Sergio Luis Suárez Gómez, Hiroaki Aihara, V. Lezaun, G. A. Cowan, C. Riccio, S. Garode, R. Akutsu, M. Lamers James, T. Nicholls, I. Alekseev, K. Kowalik, J. Kasperek, T. Zakrzewski, S. B. Kim, T. Kutter, Evan O'Connor, B. Jamieson, F. Nova, M. Barbi, Xianguo Lu, Y. Sonoda, M. Friend, Teppei Katori, L. H. V. Anthony, A. Shaikhiev, C. J. Densham, V. Gousy-Leblanc, I. Bandac, J. H. Choi, S. Sano, A. K. Ichikawa, Magda Cicerchia, S. Valder, S. Roth, J. Kameda, M. Zito, A. Vijayvargi, S. Nakai, Y. Kotsar, K. M. Tsui, K. Hoshina, K. K. Joo, C. Pastore, T. Marchi, K. Niewczas, K. Nakayoshi, G. Fiorillo, C. McGrew, P. F. Loverre, S. Playfer, G.D. Barr, L. Labarga, T. Kobayashi, E. S. Pinzon Guerra, André Rubbia, D. Karlen, Th. A. Mueller, L. Koch, F. J. Mora, M. M. Khabibullin, Hidekazu Kakuno, Yoshitaka Itow, H. K. Tanaka, P. Adrich, Jeong-Eun Lee, S. Samani, M. G. Catanesi, M. Yu, M. J. Wilking, Robert Svoboda, P. Mijakowski, N. Kolev, Yu. Onishchuk, A. Kato, J. M. Poutissou, C. Bronner, Yutaka Nakajima, B. Richards, C. Ruggles, M. Needham, P. Jonsson, Y. Hayato, S. Mine, A. Konaka, L. Munteanu, Kunio Inoue, O. Drapier, Kenneth Long, M. McCarthy, T. Kinoshita, G. Tortone, Yuuki Nakano, T. Feusels, N. Izumi, Reetanjali Moharana, T. Dealtry, S. Hassani, G. Pronost, K. Sakashita, J. G. Learned, H. M. O'Keeffe, Shintaro Ito, E. Rondio, Toru Ogitsu, D. A. Patel, Tatiana Ovsiannikova, M. Guigue, Yusuke Koshio, T. Matsubara, S. M. Stellacci, R. J. Wilkes, G. Santucci, S. Y. Suzuki, S. D. Rountree, K. Zietara, A. A. Quiroga, M. Jakkapu, A. Boiano, L. Berns, M. O. Wascko, M. M. Vyalkov, K. Porwit, M. Taani, A. Evangelisti, I. Sashima, Michal Dziewiecki, J. Feng, Y. Seiya, M. Yonenaga, B. Spisso, B. W. Pointon, C. M. Mollo, N. Booth, S. V. Cao, N. Ospina, A. J. Finch, V. Takhistov, E. Radicioni, P. Przewlocki, S. Nakayama, S. Yen, T. Sekiguchi, Yudai Suwa, J. M. Calvo-Mozota, S. Zsoldos, C. Checchia, M. Posiadala-Zezula, E. O'Sullivan, Janusz Marzec, F. Retiere, Jan T. Sobczyk, P. Migliozzi, S. Borjabad, I. Di Palma, John Hill, K. A. Kouzakov, D. L. Wark, L. Cook, D. Sgalaberna, E. W. Miller, M. Lamoureux, M. Y. Pac, S. Russo, S. L. Cartwright, Yasunari Suzuki, D. Bose, B. Zaldivar, D. Martin, Dongsu Ryu, Z. Shan, S. Miki, M. Jiang, J. Kisiel, N. Yershov, M. Matusiak, C. Pea-Garay, K. Sato, Jesús Daniel Santos, Y. Yamaguchi, D. Bravo-Berguo, Chad Finley, T. Tashiro, Lawrence D. Brown, A. Gorin, Hiromasa Tanaka, M. Ziembicki, T. Vladisavljevic, J. Zalipska, J. Insler, C. Yanagisawa, Abinash Medhi, L. Kravchuk, W. Idrissi Ibnsalih, Hirokazu Ishino, J. Bian, K. Magar, S. Cebrian, Philippe Mermod, R. Gornea, Juan Pedro Ochoa-Ricoux, Sergei Fedotov, S. Izumiyama, C. Bozza, R. Esteve, Seiko Hirota, T. Tsukamoto, K. Skwarczynski, E. De la Fuente, T. Kikawa, M. Gonin, J. Xia, Intae Yu, Gareth J. Barker, A. Marinelli, E. Kearns, L. Lavitola, Michal Ostrowski, N. Deshmukh, Y. Kataoka, F. d. M. Blaszczyk, Carsten Rott, C. Mariani, T. Ishida, Roberto Spina, J. W. Seo, Masashi Yokoyama, F. Gramegna, K. Hultqvist, G. Collazuol, P. Spradlin, Gus Sinnis, A. Takenaka, T. Xin, M. Bellato, Yuki Fujii, Mark Scott, J. A. Hernando-Morata, P. Ferrario, A. Buchowicz, S. J. Jenkins, J. Walker, J. Toledo, Pablo Fernandez, Sandhya Choubey, S. Emery, A. Mefodiev, R.P. Kurjata, M. Mongelli, J. Dumarchez, Tsuyoshi Nakaya, M. Antonova, M. Danilov, M. Feely, A. Holin, Ara Ioannisian, B. A. Popov, K Stopa, W. G. S. Vinning, M. L. Sánchez, Masato Shiozawa, L. Ludovici, J. Gao, S. Bhadra, Koji Ishidoshiro, Hiroshi Nunokawa, V. Aushev, M. Hartz, I. Shimizu, C. S. Moon, M. B. Smy, S. Matsuno, I. Anghel, J. Migenda, T. Mondal, F. Di Lodovico, M. Tada, D. J. Payne, M. Kuze, N. C. Hastings, P. Di Meo, Y. Nishimura, M. Inomoto, L. Magaletti, C. Giganti, A. Klekotko, Patrick Dunne, J. Yoo, M. C. Sanchez, A. N. Khotjantsev, Kyujin Kwak, Lars Eklund, M. Lawe, A. Mitra, H. W. Sobel, Jürgen Pozimski, Yasuhiro Makida, A. Bubak, Jaroslaw Pasternak, B. Quilain, R. Leitner, Marco Laveder, J. P. Coleman, N. F. Calabria, H. I. Jang, S. B. Boyd, Moon Moon Devi, M. Fitton, M. Harada, Artur F. Izmaylov, J. McElwee, Shunsaku Horiuchi, P. de Perio, K. Nakagiri, Y. Kano, M. Rescigno, S. Moriyama, Masayuki Nakahata, C. Pidcott, Y. Uchida, V. Palladino, A. Longhin, A. Shaykina, Michelangelo Pari, Akimichi Taketa, Yuichi Oyama, S. Suvorov, R. P. Litchfield, D. H. Moon, Katsuki Hiraide, M. Pavin, M. Koga, R. B. Vogelaar, Enrique Fernandez-Martinez, B. L. Hartfiel, Koji Yamamoto, K. Ohta, K. Abe, Alexander Studenikin, E. Mazzucato, Elisa Bernardini, Abe, K., Adrich, P., Aihara, H., Akutsu, R., Alekseev, I., Ali, A., Ameli, F., Anghel, I., Anthony, L. H. V., Antonova, M., Araya, A., Asaoka, Y., Ashida, Y., Aushev, V., Ballester, F., Bandac, I., Barbi, M., Barker, G. J., Barr, G., Batkiewicz-Kwasniak, M., Bellato, M., Berardi, V., Bergevin, M., Bernard, L., Bernardini, E., Berns, L., Bhadra, S., Bian, J., Blanchet, A., Blaszczyk, F. D. M., Blondel, A., Boiano, A., Bolognesi, S., Bonavera, L., Booth, N., Borjabad, S., Boschi, T., Bose, D., Boyd, S. B., Bozza, C., Bravar, A., Bravo-Berguo, D., Bronner, C., Brown, L., Bubak, A., Buchowicz, A., Buizza Avanzini, M., Cafagna, F. S., Calabria, N. F., Calvo-Mozota, J. M., Cao, S., Cartwright, S. L., Carroll, A., Catanesi, M. G., Cebrian, S., Chabera, M., Chakraborty, S., Checchia, C., Choi, J. H., Choubey, S., Cicerchia, M., Coleman, J., Collazuol, G., Cook, L., Cowan, G., Cuen-Rochin, S., Danilov, M., Diaz Lopez, G., De La Fuente, E., De Perio, P., De Rosa, G., Dealtry, T., Densham, C. J., Dergacheva, A., Deshmukh, N., Devi, M. M., Di Lodovico, F., Di Meo, P., Di Palma, I., Doyle, T. A., Drakopoulou, E., Drapier, O., Dumarchez, J., Dunne, P., Dziewiecki, M., Eklund, L., El Hedri, S., Ellis, J., Emery, S., Esmaili, A., Esteve, R., Evangelisti, A., Feely, M., Fedotov, S., Feng, J., Fernandez, P., Fernandez-Martinez, E., Ferrario, P., Ferrazzi, B., Feusels, T., Finch, A., Finley, C., Fiorentini, A., Fiorillo, G., Fitton, M., Frankiewicz, K., Friend, M., Fujii, Y., Fukuda, Y., Galinski, G., Gao, J., Garde, C., Garfagnini, A., Garode, S., Gialanella, L., Giganti, C., Gomez-Cadenas, J. J., Gonin, M., Gonzalez-Nuevo, J., Gorin, A., Gornea, R., Gousy-Leblanc, V., Gramegna, F., Grassi, M., Grella, G., Guigue, M., Gumplinger, P., Hadley, D. R., Harada, M., Hartfiel, B., Hartz, M., Hassani, S., Hastings, N. C., Hayato, Y., Hernando-Morata, J. A., Herrero, V., Hill, J., Hiraide, K., Hirota, S., Holin, A., Horiuchi, S., Hoshina, K., Hultqvist, K., Iacob, F., Ichikawa, A. K., Idrissi Ibnsalih, W., Iijima, T., Ikeda, M., Inomoto, M., Inoue, K., Insler, J., Ioannisian, A., Ishida, T., Ishidoshiro, K., Ishino, H., Ishitsuka, M., Ito, H., Ito, S., Itow, Y., Iwamoto, K., Izmaylov, A., Izumi, N., Izumiyama, S., Jakkapu, M., Jamieson, B., Jang, H. I., Jang, J. S., Jenkins, S. J., Jeon, S. H., Jiang, M., Jo, H. S., Jonsson, P., Joo, K. K., Kajita, T., Kakuno, H., Kameda, J., Kano, Y., Kalaczynski, P., Karlen, D., Kasperek, J., Kataoka, Y., Kato, A., Katori, T., Kazarian, N., Kearns, E., Khabibullin, M., Khotjantsev, A., Kikawa, T., Kekic, M., Kim, J. H., Kim, J. Y., Kim, S. B., Kim, S. Y., King, S., Kinoshita, T., Kisiel, J., Klekotko, A., Kobayashi, T., Koch, L., Koga, M., Koerich, L., Kolev, N., Konaka, A., Kormos, L. L., Koshio, Y., Korzenev, A., Kotsar, Y., Kouzakov, K. A., Kowalik, K. L., Kravchuk, L., Kryukov, A. P., Kudenko, Y., Kumita, T., Kurjata, R., Kutter, T., Kuze, M., Kwak, K., La Commara, M., Labarga, L., Lagoda, J., Lamers James, M., Lamoureux, M., Laveder, M., Lavitola, L., Lawe, M., Learned, J. G., Lee, J., Leitner, R., Lezaun, V., Lim, I. T., Lindner, T., Litchfield, R. P., Long, K. R., Longhin, A., Loverre, P., Lu, X., Ludovici, L., Maekawa, Y., Magaletti, L., Magar, K., Mahn, K., Makida, Y., Malek, M., Malinsky, M., Marchi, T., Maret, L., Mariani, C., Marinelli, A., Martens, K., Marti, L., Martin, J. F., Martin, D., Marzec, J., Matsubara, T., Matsumoto, R., Matsuno, S., Matusiak, M., Mazzucato, E., Mccarthy, M., Mccauley, N., Mcelwee, J., Mcgrew, C., Mefodiev, A., Medhi, A., Mehta, P., Mellet, L., Menjo, H., Mermod, P., Metelko, C., Mezzetto, M., Migenda, J., Migliozzi, P., Mijakowski, P., Miki, S., Miller, E. W., Minakata, H., Minamino, A., Mine, S., Mineev, O., Mitra, A., Miura, M., Moharana, R., Mollo, C. M., Mondal, T., Mongelli, M., Monrabal, F., Moon, D. H., Moon, C. S., Mora, F. J., Moriyama, S., Mueller, T. A., Munteanu, L., Murase, K., Nagao, Y., Nakadaira, T., Nakagiri, K., Nakahata, M., Nakai, S., Nakajima, Y., Nakamura, K., Nakamura, K. I., Nakamura, H., Nakano, Y., Nakaya, T., Nakayama, S., Nakayoshi, K., Nascimento Machado, L., Naseby, C. E. R., Navarro-Garcia, B., Needham, M., Nicholls, T., Niewczas, K., Nishimura, Y., Noah, E., Nova, F., Nugent, J. C., Nunokawa, H., Obrebski, W., Ochoa-Ricoux, J. P., O'Connor, E., Ogawa, N., Ogitsu, T., Ohta, K., Okamoto, K., O'Keeffe, H. M., Okumura, K., Onishchuk, Y., Orozco-Luna, F., Oshlianskyi, A., Ospina, N., Ostrowski, M., O'Sullivan, E., O'Sullivan, L., Ovsiannikova, T., Oyama, Y., Ozaki, H., Pac, M. Y., Paganini, P., Palladino, V., Paolone, V., Pari, M., Parsa, S., Pasternak, J., Pastore, C., Pastuszak, G., Patel, D. A., Pavin, M., Payne, D., Pea-Garay, C., Pidcott, C., Pinzon Guerra, E., Playfer, S., Pointon, B. W., Popov, A., Popov, B., Porwit, K., Posiadala-Zezula, M., Poutissou, J. -M., Pozimski, J., Pronost, G., Prouse, N. W., Przewlocki, P., Quilain, B., Quiroga, A. A., Radicioni, E., Radics, B., Rajda, P. J., Renner, J., Rescigno, M., Retiere, F., Ricciardi, G., Riccio, C., Richards, B., Rondio, E., Rose, H. J., Roskovec, B., Roth, S., Rott, C., Rountree, S. D., Rubbia, A., Ruggeri, A. C., Ruggles, C., Russo, S., Rychter, A., Ryu, D., Sakashita, K., Samani, S., Sanchez, F., Sanchez, M. L., Sanchez, M. C., Sano, S., Santos, J. D., Santucci, G., Sarmah, P., Sashima, I., Sato, K., Scott, M., Seiya, Y., Sekiguchi, T., Sekiya, H., Seo, J. W., Seo, S. H., Sgalaberna, D., Shaikhiev, A., Shan, Z., Shaykina, A., Shimizu, I., Shin, C. D., Shinoki, M., Shiozawa, M., Sinnis, G., Skrobova, N., Skwarczynski, K., Smy, M. B., Sobczyk, J., Sobel, H. W., Soler, F. J. P., Sonoda, Y., Spina, R., Spisso, B., Spradlin, P., Stankevich, K. L., Stawarz, L., Stellacci, S. M., Stopa, K., Studenikin, A. I., Suarez Gomez, S. L., Suganuma, T., Suvorov, S., Suwa, Y., Suzuki, A. T., Suzuki, S. Y., Suzuki, Y., Svirida, D., Svoboda, R., Taani, M., Tada, M., Takeda, A., Takemoto, Y., Takenaka, A., Taketa, A., Takeuchi, Y., Takhistov, V., Tanaka, H., Tanaka, H. A., Tanaka, H. I., Tanaka, M., Tashiro, T., Thiesse, M., Thompson, L. F., Toledo, J., Tomatani-Sanchez, A. K., Tortone, G., Tsui, K. M., Tsukamoto, T., Tzanov, M., Uchida, Y., Vagins, M. R., Valder, S., Valentino, V., Vasseur, G., Vijayvargi, A., Vilela, C., Vinning, W. G. S., Vivolo, D., Vladisavljevic, T., Vogelaar, R. B., Vyalkov, M. M., Wachala, T., Walker, J., Wark, D., Wascko, M. O., Wendell, R. A., Wilkes, R. J., Wilking, M. J., Wilson, J. R., Wronka, S., Xia, J., Xie, Z., Xin, T., Yamaguchi, Y., Yamamoto, K., Yanagisawa, C., Yano, T., Yen, S., Yershov, N., Yeum, D. N., Yokoyama, M., Yonenaga, M., Yoo, J., Yu, I., Yu, M., Zakrzewski, T., Zaldivar, B., Zalipska, J., Zaremba, K., Zarnecki, G., Ziembicki, M., Zietara, K., Zito, M., Zsoldos, S., Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Hyper-Kamiokande, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics - Instrumentation and Detectors, 09.- Desarrollar infraestructuras resilientes, promover la industrialización inclusiva y sostenible, y fomentar la innovación, KAMIOKANDE, Astrophysics, 01 natural sciences, neutrino: flux, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), neutrino, accretion, black hole, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Core-collapse supernovae, neutron star, Monte Carlo, physics.ins-det, 010303 astronomy & astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Instrumentation and Detectors (physics.ins-det), 16. Peace & justice, Supernova, neutrino: detector, 07.- Asegurar el acceso a energías asequibles, fiables, sostenibles y modernas para todos, supernova, neutrino astronomy, neutrino physics, Neutrino detector, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, supernova: collapse, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Observable universe, Astrophysics::Cosmology and Extragalactic Astrophysics, Hyper-Kamiokande, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], High energy physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, hep-ex, 010308 nuclear & particles physics, supernova: model, Astronomy and Astrophysics, Galaxy, Black hole, Neutron star, Space and Planetary Science, neutrino: burst, galaxy, Neutrino astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: Autorzy: Abe K., Adrich P., Aihara H., Akutsu, R., Alekseev I., Ali A. , Ameli F., Anghel I., Anthony L. H. V., Antonova M. , Araya A., Asaoka Y., Ashida Y., Aushev V., Ballester F., Bandac I., Barbi M., Barker G. J., Barr G., Batkiewicz-Kwasniak M., Bellato M., Berardi V., Bergevin M., Bernard L., Bernardini E., Berns L., Bhadra S., Bian J., Blanchet A., Blaszczyk F. d. M., Blonde A., Boiano A., Bolognesi S., Bonavera L., Booth N., Borjabad S., Boschi, T., Bose D., Boyd S . B., Bozza C., Bravar A., Bravo-Berguño D., Bronner C., Brown L., Bubak Arkadiusz, Buchowicz A., Buizza Avanzini M., Cafagna F. S., Calabria N. F., Calvo-Mozota J. M., Cao S., Cartwright S.L., Carroll A., Catanesi M. G., Cebriàn, S., Chabera M., Chakraborty, S., Checchia C., Choi J.H., Choubey S., Cicerchia M., Coleman J., Collazuol G., Cook L., Cowan G., Cuen-Rochin, S., Danilov M., Díaz López G., De la Fuente E., de Perio P., De Rosa G., Dealtry T., Densham C. J., Dergacheva A., Deshmukh N., Devi M. M., Di Lodovico F., Di Meo, P., Di Palma I., Doyle T. A., Drakopoulou E., Drapier O., Dumarchez J., Dunne P., Dziewiecki M., Eklund L., El Hedri S., Ellis J., Emery S., Esmaili A., Esteve R., Evangelisti A., Feely M., Fedotov S., Feng J., Fernandez P., Fernández-Martinez E., Ferrario P., Ferrazzi,B., Feusels T., Finch A., Finley C., Fiorentini A., Fiorillo G., Fitton M., Frankiewicz K., Friend M., Fujii Y., Fukuda Y., Galinski G., Gao J., Garde C., Garfagnini A., Garode S., Gialanella L., Giganti C., Gomez-Cadenas J.J., Gonin M., González-Nuevo J., Gorin A., Gornea R., Gousy-Leblanc V. Gramegna F. Grassi M. Grella G. Guigue M. Gumplinger P. Hadley D.R. Harada M., Hartfiel B., Hartz M., Hassani S., Hastings N.C., Hayato Y., Hernando-Morata J.A., Herrero V., Hill J., Hiraide K., Hirota S., Holin A., Horiuchi S., Hoshina K., Hultqvist K., Iacob F., Ichikawa A.K., Idrissi Ibnsalih W., Iijima T., Ikeda M., Inomoto M., Inoue K., Insler J., Ioannisian A., Ishida T., Ishidoshiro K., Ishino H., Ishitsuka M., Ito H., Ito S., Itow Y., Iwamoto K., Izmaylov A., Izumi N., Izumiyama S., Jakkapu M., Jamieson B., Jang H.I., Jang J.S., Jenkins S.J., Jeon S.H., Jiang M., Jo H.S., Jonsson P., Joo K.K., Kajita T., Kakuno H., Kameda J., Kano Y., Kalaczynski P., Karlen D., Kasperek J., Kataoka Y., Kato A., Katori T., Kazarian N., Kearns E., Khabibullin M., Khotjantsev A., Kikawa T., Kekic M., Kim J.H., Kim J.Y., Kim S.B., Kim S.Y., King S., Kinoshita T., Kisiel Jan, Klekotko A., Kobayashi T., Koch L., Koga M., Koerich L., Kolev N., Konaka A., Kormos L.L., Koshio Y., Korzenev A., Kotsar Y., Kouzakov K.A., Kowalik K.L., Kravchuk L., Kryukov A.P., Kudenko Y., Kumita T., Kurjata R., Kutter T., Kuze M., Kwak K., La Commara M., Labarga L., Lagoda J., Lamers James J., Lamoureux M., Laveder M., Lavitola L., Lawe M., Learned J.G., Lee J., Leitner R., Lezaun V., Lim I.T., Lindner T., Litchfield R.P., Long K.R., Longhin A., Loverre P., Lu X., Ludovici L., Maekawa Y., Magaletti L., Magar K., Mahn K., Makida Y., Malek M., Malinský M., Marchi T., Maret L., Mariani C., Marinelli A., Martens K., Marti L., Martin J.F. Martin D., Marzec J., Matsubara T., Matsumoto R., Matsuno S., Matusiak M., Mazzucato E., McCarthy M., McCauley N., McElwee J., McGrew C., Mefodiev A., Medhi A., Mehta P., Mellet L., Menjo H., Mermod P., Metelko C., Mezzetto M., Migenda J., Migliozzi P., Mijakowski P., Miki S., Miller E.W., Minakata H., Minamino A., Mine S., Mineev O., Mitra A., Miura M., Moharana R., Mollo C.M., Mondal T., Mongelli M., Monrabal F., Moon D.H., Moon C.S., Mora F.J., Moriyama S., Mueller Th.A., Munteanu L., Murase K., Nagao Y., Nakadaira T., Nakagiri K., Nakahata M., Nakai S., Nakajima Y., Nakamura K., Nakamura KI., Nakamura H., Nakano Y., Nakaya T., Nakayama S., Nakayoshi K., Nascimento Machado L., Naseby C.E.R., Navarro-Garcia B., Needham M., Nicholls T., Niewczas K., Nishimura Y., Noah E., Nova F., Nugent J.C., Nunokawa H., Obrebski W., Ochoa-Ricoux J.P., O’Connor E., Ogawa N., Ogitsu T., Ohta K., Okamoto K., O’Keeffe H.M., Okumura K., Onishchuk Y., Orozco-Luna F., Oshlianskyi A., Ospina N., Ostrowski M., O’Sullivan E., O’Sullivan L., Ovsiannikova T., Oyama Y., Ozaki H., Pac M.Y., Paganini P., Palladino V., Paolone V., Pari M., Parsa S., Pasternak J., Pastore C., Pastuszak G., Patel D.A., Pavin M., Payne D., Peña-Garay C., Pidcott C., Pinzon Guerra E., Playfer S., Pointon B.W., Popov A., Popov B., Porwit Kamil, Posiadala-Zezula M., Poutissou J.M., Pozimski J., Pronost G., Prouse N.W., Przewlocki P., Quilain B., Quiroga A.A., Radicioni E., Radics B., Rajda P.J., Renner J., Rescigno M., Retiere F., Ricciardi G., Riccio C., Richards B., Rondio E., Rose H.J., Roskovec B., Roth S., Rott C., Rountree S.D., Rubbia A., Ruggeri A.C., Ruggles C., Russo S., Rychter A., Ryu D., Sakashita K., Samani S., Sánchez F., Sánchez M.L., Sanchez M.C., Sano S., Santos J.D., Santucci G., Sarmah P., Sashima I., Sato K., Scott M., Seiya Y., Sekiguchi T., Sekiya H., Seo J.W., Seo S.H., Sgalaberna D., Shaikhiev A., Shan Z., Shaykina A., Shimizu I., Shin C.D., Shinoki M., Shiozawa M., Sinnis G., Skrobova N., Skwarczynski K., Smy M.B., Sobczyk J., Sobel H.W., Soler F. J. P., Sonoda Y., Spina R., Spisso B., Spradlin B., Stankevich K.L., Stawarz L., Stellacci S.M., Stopa K., Studenikin A.I., Suárez Gómez S.L., Suganuma T., Suvorov S., Suwa Y., Suzuki A.T., Suzuki S.Y., Suzuki Y., Svirida D., Svoboda R., Taani M., Tada M., Takeda A., Takemoto Y., Takenaka A., Taketa A., Takeuchi Y., Takhistov V., Tanaka H., Tanaka H.A., Tanaka H.I., Tanaka M., Tashiro T., Thiesse M., Thompson L.F., Toledo J., Tomatani-Sánchez A.K., Tortone G., Tsui K.M., Tsukamoto T., Tzanov M., Uchida Y., Vagins M.R., Valder S., Valentino V., Vasseur G., Vijayvargi A., Vilela C., Vinning W. G. S., Vivolo D., Vladisavljevic T., Vogelaar R.B., Vyalkov M.M., Wachala T., Walker J., Wark D., Wascko M.O., Wendell R.A., Wilkes R.J., Wilking M.J., Wilson M.R., Wronka S., Xia J., Xie Z., Xin T., Yamaguchi Y., Yamamoto K., Yanagisawa C., Yano T., Yen S., Yershov N., Yeum D.N., Yokoyama M., Yonenaga M., Yoo J., Yu I., Yu M., Zakrzewski T., Zaldivar B., Zalipska J., Zaremba K., Zarnecki G., Ziembicki M., Zietara K., Zito M., Zsoldos S., Core-collapse supernovae are among the most magnificent events in the observable universe. They produce many of the chemical elements necessary for life to exist and their remnants-neutron stars and black holes-are interesting astrophysical objects in their own right. However, despite millennia of observations and almost a century of astrophysical study, the explosion mechanism of core-collapse supernovae is not yet well understood. Hyper-Kamiokande is a next-generation neutrino detector that will be able to observe the neutrino flux from the next galactic core-collapse supernova in unprecedented detail. We focus on the first 500 ms of the neutrino burst, corresponding to the accretion phase, and use a newly-developed, high-precision supernova event generator to simulate Hyper-Kamiokandeʼs response to five different supernova models. We show that Hyper-Kamiokande will be able to distinguish between these models with high accuracy for a supernova at a distance of up to 100 kpc. Once the next galactic supernova happens, this ability will be a powerful tool for guiding simulations toward a precise reproduction of the explosion mechanism observed in nature.
Published: 2022

7. CENN: A fully convolutional neural network for CMB recovery in realistic microwave sky simulations

Author: J. M. Casas, L. Bonavera, J. González-Nuevo, C. Baccigalupi, M. M. Cueli, D. Crespo, E. Goitia, J. D. Santos, M. L. Sánchez, and F. J. de Cos
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Component separation is the process with which emission sources in astrophysical maps are generally extracted by taking multi-frequency information into account. It is crucial to develop more reliable methods for component separation for future CMB experiments. We aim to develop a new method based on fully convolutional neural networks called the Cosmic microwave background Extraction Neural Network (CENN) in order to extract the CMB signal in total intensity. The frequencies used are the Planck channels 143, 217 and 353 GHz. We validate the network at all sky, and at three latitude intervals: lat1=0^{\circ}, Comment: Accepted for publication in Astronomy & Astrophysics journal. 11 pages, 6 figures
Published: 2022

8. Planck 2018 results: XII. Galactic astrophysics using polarized dust emission

Author: E. Di Valentino, A. Marcos-Caballero, M. Frailis, Carlo Baccigalupi, François Levrier, N. Mauri, Jason D. McEwen, X. Dupac, Carlo Burigana, Nicoletta Krachmalnicoff, K. Benabed, J. R. Bond, Vincent Guillet, Jose Alberto Rubino-Martin, L. Polastri, Alessandro Melchiorri, Andrea Bracco, G. de Zotti, J. González-Nuevo, P. B. Lilje, E. Martínez-González, P. de Bernardis, Yashar Akrami, S. Galli, J. Aumont, Marian Douspis, M. Maris, Martina Gerbino, L. Toffolatti, Rashid Sunyaev, E. Franceschi, Guillaume Patanchon, A. Mangilli, Edith Falgarone, J.-M. Delouis, Anthony Lasenby, Jörg P. Rachen, M. Migliaccio, M. Bucher, Douglas Scott, M. Ashdown, H. K. Eriksen, K. Ganga, Jose M. Diego, J. A. Tauber, M. Savelainen, E. Keihänen, Gianluca Morgante, B. P. Crill, F. Cuttaia, Charles R. Lawrence, C. Combet, N. Mandolesi, Fabrizio Villa, Nabila Aghanim, D. Herranz, M. Tenti, F. Vansyngel, S. Galeotta, James J. Bock, B. Van Tent, L. P. L. Colombo, Andrew H. Jaffe, Clive Dickinson, B. Ruiz-Granados, A.-S. Suur-Uski, M. Le Jeune, Philip Lubin, J. Kim, J. F. Macías-Pérez, Mario Ballardini, F. Boulanger, Davide Maino, A. A. Fraisse, W. C. Jones, Ranga-Ram Chary, Andrea Zacchei, Tiziana Trombetti, Tuhin Ghosh, M.-A. Miville-Deschênes, Graca Rocha, George Efstathiou, Sabino Matarrese, J. Valiviita, Nicola Vittorio, V. Lindholm, Valeria Pettorino, A. J. Banday, Katia Ferrière, A. Moneti, Franz Elsner, Jacques Delabrouille, Yabebal Fantaye, R. B. Barreiro, A. Mennella, N. Bartolo, L. Montier, Michele Liguori, P. Vielva, F. K. Hansen, Fabio Finelli, G. Roudier, F. Piacentini, M. Tomasi, K. Kiiveri, Erminia Calabrese, Guilaine Lagache, C. Rosset, M. I. R. Alves, M. Sandri, Jean-François Cardoso, Peter G. Martin, Marco Bersanelli, M. López-Caniego, Zhiqi Huang, Andrei V. Frolov, François R. Bouchet, Julien Carron, George Helou, L. Salvati, J.-P. Bernard, Adam Moss, Gregory M. Green, J.-L. Puget, Benjamin D. Wandelt, Julian Borrill, Will Handley, S. Basak, Ricardo Genova-Santos, Ingunn Kathrine Wehus, O. Doré, Paolo Natoli, D. Tavagnacco, Massimiliano Lattanzi, G. Polenta, A. Renzi, Diego Molinari, G. Maggio, R. Fernandez-Cobos, Reijo Keskitalo, P. Bielewicz, M. Reinecke, Martin Kunz, Mathieu Remazeilles, Jon E. Gudmundsson, C. Sirignano, Francesco Forastieri, L. Pagano, Andrea Zonca, H. C. Chiang, Francesca Perrotta, Torsten A. Enßlin, Serge Gratton, Yin-Zhe Ma, Eric Hivon, D. Paoletti, Alessandro Gruppuso, J.-M. Lamarre, A. Ducout, Hannu Kurki-Suonio, I. Ristorcelli, Krzysztof M. Gorski, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Parma = Università degli studi di Parma [Parme, Italie], Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Patrimoine, Littérature, Histoire (PLH), Université Toulouse - Jean Jaurès (UT2J), Laboratoire de Recherche en Informatique (LRI), CentraleSupélec-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CentraleSupélec, Universidade Aberta [Lisboa], Centre National d'Études Spatiales [Toulouse] (CNES), Infrared Processing and Analysis Center (IPAC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratory for Phytosanitary Diagnostics and Forecasts, All-Russian Institute for Plant Protection, Russian Academy of Sciences [Moscow] (RAS), Institut National Polytechnique (Toulouse) (Toulouse INP), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, ICRA and Physics Department, Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of Manchester [Manchester], Venetian Institute Molecular Medicine (VIMM), University of British Columbia (UBC), Laboratoire de neurobiologie cellulaire et moléculaire (NBCM), Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Aghanim N., Akrami Y., Alves M.I.R., 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., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bracco A., Bucher M., Burigana C., Calabrese E., Cardoso J.-F., Carron J., Chary R.-R., Chiang H.C., Colombo L.P.L., Combet C., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Dickinson C., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Falgarone E., Fantaye Y., Fernandez-Cobos R., Ferriere K., Finelli F., Forastieri F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Green G., Gruppuso A., Gudmundsson J.E., Guillet V., Handley W., Hansen F.K., Helou G., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Levrier F., Liguori M., Lilje P.B., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Melchiorri A., Mennella A., Migliaccio M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Natoli P., Pagano L., Paoletti D., Patanchon G., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Ristorcelli I., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Sirignano C., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Trombetti T., Valiviita J., Vansyngel F., Van Tent B., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., Zacchei A., Zonca A., Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Agence Nationale de la Recherche (France), Universidad de Cantabria, Department of Physics, Helsinki Institute of Physics, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Università degli studi di Parma = University of Parma (UNIPR), Université de Toulouse (UT)-Université de Toulouse (UT), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), Università degli Studi di Padova = University of Padua (Unipd), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), ANR-17-CE31-0022,BxB,Champs B interstellaires et modes B de l'inflation(2017), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), 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), 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), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: STARLIGHT, Astronomy, Inverse, Astrophysics, magnetic fields, 7. Clean energy, 01 natural sciences, Polarization, DISTANT STARS, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, Turbulence, extinction, ISM [Submillimeter], Astrophysics::Instrumentation and Methods for Astrophysics, MAGNETIC-FIELD, CLOUDS, Galaxy: ISM, LATITUDES, Polarization (waves), STATISTICS, Magnetic field, ISM: dust, symbols, INTERSTELLAR POLARIZATION, submillimeter: ISM, dust, local insterstellar matter, COMPONENT SEPARATION, GRAIN ALIGNMENT, Local insterstellar matter, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, polarization, turbulence, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, DISPERSION, Dust, Extinction, Local insterstellar matter, Magnetic fields, Polarization, Submillimeter: ISM, Turbulence, 0103 physical sciences, Computer Science::Symbolic Computation, Planck, Dust, extinction, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Molecular cloud, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, submillimetre: ISM, 13. Climate action, Space and Planetary Science, Sky, Magnetic fields, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Dust emission
Abstract: Planck Collaboration: et al., Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle ψ, and dispersion function of polarization angles 𝒮. The joint distribution (one-point statistics) of p and NH confirms that the mean and maximum polarization fractions decrease with increasing NH. The uncertainty on the maximum observed polarization fraction, pmax = 22.0−1.4+3.5% at 353 GHz and 80′ resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and 𝒮 found earlier is seen to be present at high latitudes. This follows the 𝒮 ∝ p−1 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, ψ, and 𝒮 for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map 𝒮 × p, looking for residual trends. While the polarization fraction p decreases by a factor of 3−4 between NH = 1020 cm−2 and NH = 2 × 1022 cm−2, out of the Galactic plane, this product 𝒮 × p only decreases by about 25%. Because 𝒮 is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with NH is determined mostly by the magnetic-field structure and not by a drop in grain alignment. This systematic trend is observed both in the diffuse interstellar medium (ISM) and in molecular clouds of the Gould Belt. Second, we look for a dependence of polarization properties on the dust temperature, as we would expect from the radiative alignment torque (RAT) theory. We find no systematic trend of 𝒮 × p with the dust temperature Td, whether in the diffuse ISM or in the molecular clouds of the Gould Belt. In the diffuse ISM, lines of sight with high polarization fraction p and low polarization angle dispersion 𝒮 tend, on the contrary, to have colder dust than lines of sight with low p and high 𝒮. We also compare the Planck thermal dust polarization with starlight polarization data in the visible at high Galactic latitudes. The agreement in polarization angles is remarkable, and is consistent with what we expect from the noise and the observed dispersion of polarization angles in the visible on the scale of the Planck beam. The two polarization emission-to-extinction ratios, RP/p and RS/V, which primarily characterize dust optical properties, have only a weak dependence on the column density, and converge towards the values previously determined for translucent lines of sight. We also determine an upper limit for the polarization fraction in extinction, pV/E(B − V), of 13% at high Galactic latitude, compatible with the polarization fraction p ≈ 20% observed at 353 GHz. Taken together, these results provide strong constraints for models of Galactic dust in diffuse gas., The research leading to these results has received funding from the European Research Council under the European Union’s Horizon 2020 Research & Innovation Framework Programme/ERC grant agreement ERC-2016-ADG-742719. This research has received funding from the Agence Nationale de la Recherche (ANR-17-CE31-0022). The Planck Collaboration acknowledges the support of ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, 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); ERC and PRACE (EU).
Published: 2020

9. Constraining the polarisation flux density and angle of point sources by training a convolutional neural network

Author: J. M. Casas, L. Bonavera, J. González-Nuevo, M. M. Cueli, D. Crespo, E. Goitia, C. González-Gutiérrez, J. D. Santos, M. L. Sánchez, and F. J. de Cos
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Constraining the polarisation properties of extragalactic point sources is a relevant task not only because they are one of the main contaminants for primordial cosmic microwave background B-mode detection if the tensor-to-scalar ratio is lower than r = 0.001, but also for a better understanding of the properties of radio-loud active galactic nuclei. We develop and train a machine learning model based on a convolutional neural network to learn how to estimate the polarisation flux density and angle of point sources embedded in cosmic microwave background images knowing only their positions. To train the neural network, we use realistic simulations of patches of area 32x32 pixels at the 217 GHz Planck channel with injected point sources at their centres. The patches also contain a realistic background composed by dust, the CMB and instrumental noise. Firstly, we study the comparison between true and estimated polarisation flux densities for P, Q and U. Secondly, we analyse the comparison between true and estimated polarisation angles. Finally, we study the performance of our model with real data and we compare our results against the PCCS2. We obtain that our model is reliable to constrain the polarisation flux above 80 mJy. For this limit, we obtain errors lower than 30%. Training the same network with Q and U, the reliability limit is above +-250 mJy for determining the polarisation angle of both Q and U sources with a 1sigma uncertainty of +-29deg and +-32deg for Q and U sources respectively. We obtain similar results to the PCCS2 for some sources, although we also find discrepancies in the 300-400 mJy flux density range with respect to the Planck catalogue. Based on these results, our model seems to be a promising tool to give estimations of the polarisation flux densities and angles of point sources above 80 mJy in any catalogue with practically null computational time., Comment: 9 pages, 9 Figures. Forthcoming article Astronomy & Astrophysics journal
Published: 2022
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10. Multi-frequency point source detection with fully convolutional networks: performance in realistic microwave sky simulations

Author: M. M. Cueli, Jesús Daniel Santos, J. González-Nuevo, Sergio Luis Suárez Gómez, Fernando Sánchez-Lasheras, D. Crespo, Mercedes Leonor Sanchez, Laura Bonavera, D. Herranz, F. J. de Cos, J. M. Casas, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Agencia Estatal de Investigación (España), and Universidad de Cantabria
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Point source, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Techniques: image processing, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cosmic background radiation, galaxies [Submillimeter], Submillimeter: galaxies, Space and Planetary Science, Sky, image processing [Techniques], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics, Remote sensing, media_common
Abstract: [Context] Point source (PS) detection is an important issue for future cosmic microwave background (CMB) experiments since they are one of the main contaminants to the recovery of CMB signal on small scales. Improving its multi-frequency detection would allow us to take into account valuable information otherwise neglected when extracting PS using a channel-by-channel approach., [Aims] We aim to develop an artificial intelligence method based on fully convolutional neural networks to detect PS in multi-frequency realistic simulations and compare its performance against one of the most popular multi-frequency PS detection methods, the matrix filters. The frequencies used in our analysis are 143, 217, and 353 GHz, and we imposed a Galactic cut of 30°., [Methods] We produced multi-frequency realistic simulations of the sky by adding contaminating signals to the PS maps as the CMB, the cosmic infrared background, the Galactic thermal emission, the thermal Sunyaev-Zel’dovich effect, and the instrumental and PS shot noises. These simulations were used to train two neural networks called flat and spectral MultiPoSeIDoNs. The first one considers PS with a flat spectrum, and the second one is more realistic and general because it takes into account the spectral behaviour of the PS. Then, we compared the performance on reliability, completeness, and flux density estimation accuracy for both MultiPoSeIDoNs and the matrix filters., [Results] Using a flux detection limit of 60 mJy, MultiPoSeIDoN successfully recovered PS reaching the 90% completeness level at 58 mJy for the flat case, and at 79, 71, and 60 mJy for the spectral case at 143, 217, and 353 GHz, respectively. The matrix filters reach the 90% completeness level at 84, 79, and 123 mJy. To reduce the number of spurious sources, we used a safer 4σ flux density detection limit for the matrix filters, the same as was used in the Planck catalogues, obtaining the 90% of completeness level at 113, 92, and 398 mJy. In all cases, MultiPoSeIDoN obtains a much lower number of spurious sources with respect to the filtering method. The recovering of the flux density of the detections, attending to the results on photometry, is better for the neural networks, which have a relative error of 10% above 100 mJy for the three frequencies, while the filter obtains a 10% relative error above 150 mJy for 143 and 217 GHz, and above 200 mJy for 353 GHz., [Conclusions] Based on the results, neural networks are the perfect candidates to substitute filtering methods to detect multi-frequency PS in future CMB experiments. Moreover, we show that a multi-frequency approach can detect sources with higher accuracy than single-frequency approaches also based on neural networks., J.M.C., J.G.N., L.B., M.M.C. and D.C. acknowledge financial support from the PGC 2018 project PGC2018-101948-B-I00 (MICINN, FEDER). DH acknowledges the Spanish MINECO and the Spanish Ministerio de Ciencia, Innovación y Universidades for partial financial support under project PGC2018-101814-B-I00. M.M.C. acknowledges PAPI-20-PF-23 (Universidad de Oviedo). J.D.C.J., M.L.S., S.L.S.G., J.D.S. and F.S.L. acknowledge financial support from the I+D 2017 project AYA2017-89121-P and support from the European Union’s Horizon 2020 research and innovation programme under the H2020-INFRAIA-2018-2020 grant agreement No 210489629.
Published: 2022

11. Galaxy cluster mass density profile derived using the submillimetre galaxies magnification bias

Author: Laura Bonavera, J. M. Casas, Andrea Lapi, M. M. Cueli, J. González-Nuevo, D. Crespo, and L. Fernandez
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, dark matter, Galactic halo, gravitational lensing: weak, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, Galaxy group, Cluster (physics), galaxies: clusters: general, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Physics, Estimator, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In this work we want to study the average mass density profile of tens to hundreds of clusters of galaxies acting as lenses that produce a magnification bias on the SMGs, and to estimate their associated masses and concentrations for different richness ranges. The background sample is composed of SMGs observed by Herschel with 1.2, Comment: 12 pages, 6 figures, accepted for publication by A&A
Published: 2022

12. Selecting a complete sample of blazars in sub-millimetre catalogues

Author: M Massardi, M Bonato, M López-Caniego, V Galluzzi, G De Zotti, L Bonavera, J González-Nuevo, A Lapi, and E Liuzzo
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), submillimetre: general, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), quasars: general, FOS: Physical sciences, Astronomy and Astrophysics, BL Lacertae objects: general, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The \textit{Herschel} Astrophysical Terahertz Large Area Survey (H-ATLAS), that has covered about 642 sq. deg. in 5 bands from 100 to 500 $\mu\rm m$, allows a blind flux-limited selection of blazars at sub-mm wavelengths. However, blazars constitute a tiny fraction of H-ATLAS sources and therefore identifying them is not a trivial task. Using the data on known blazars detected by the H-ATLAS we have defined a locus for 500\,$\mu$m selected blazars and exploited it to select blazar candidates in the H-ATLAS fields. Candidates and known blazars in the H-ATLAS equatorial and South Galactic Pole fields were followed up with the Australia Telescope Compact Array (ATCA) or with the Karl G. Jansky Very Large Array (VLA), and matched with existing radio- and mm-catalogues to reconstruct the spectral behaviour over at least 6 orders of magnitude in frequency. We identified a selection approach that, combining the information in the sub-mm and radio domains, efficiently singles out genuine blazars. In this way, we identified a sample of 39 blazars brighter than $S_{500\mu\rm m} = 35\,$mJy in the H-ATLAS fields. Tests made cross-matching the H-ATLAS catalogues with large catalogues of blazar candidates indicate that the sample is complete. The derived counts are compared with model predictions finding good consistency with the C2Ex model and with estimates based on ALMA data., Comment: 16 pages, 7 figures, accepted by MNRAS
Published: 2022

13. Quasi-stellar objects and galaxy mass density profiles derived using the submillimetre galaxies magnification bias

Author: D. Crespo, J. González-Nuevo, L. Bonavera, M. M. Cueli, J. M. Casas, and E. Goitia
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Context. The magnification bias on the submillimetre galaxies (SMGs) is a gravitational lensing effect, where the SMGs are used as background lensed galaxies. This effect can be used to investigate the mass density profiles of different types of foreground lenses. Aims. In this work, we want to exploit the magnification bias of the SMGs using two different foreground samples, quasi-stellar objects (QSOs) and galaxies. Our aim is to study and compare their mass density profiles and estimate their masses and concentrations. Methods. The background SMG sample consists of objects observed by Herschel with 1.2 z z z Results. The measurements are correctly fitted after splitting the available angular scales into an inner and an outer part using two independent mass density profiles, one for each region. In particular, for the QSOs, we obtain masses of log10(M/M⊙) = 13.51 ± 0.04 and of log10(M/M⊙) = 13.44 ± 0.17 for the inner and outer parts, respectively. The estimated masses for the galaxy sample are log10(M/M⊙) = 13.32 ± 0.08 and log10(M/M⊙) = 12.78 ± 0.21 for the inner and outer parts, respectively. The concentrations for the inner part are much higher than those for the outer region for both samples: C = 6.85 ± 0.34 (inner) and C = 0.36 ± 0.18 (outer) for the QSOs and C = 8.23 ± 0.77 (inner) and C = 1.21 ± 1.01 (outer) for the galaxies. Conclusions. In both samples, the inner part has an excess in the mass density profile with respect to the outer part for both QSOs and galaxy samples. We obtain similar values for the central mass with both samples, and they are also in agreement with those of galaxy clusters results. However, the estimated masses for the outer region and the concentrations of the inner region both vary with lens sample. We believe this to be related to the probability of galactic interactions and/or the different evolutionary stages.
Published: 2022

14. The K2-OjOS Project: New and revisited planets and candidates in K2 campaigns 5, 16, & 18

Author: M. L. Sánchez Rodríguez, J. P. de Leon, J. D. Santos Rodríguez, J. M. Recio, D. Vázquez García, N. Gómez Hernández, A. Castro-González, C. González Gutiérrez, J. Korth, J. R. Vidal Blanco, F. García Riesgo, R. Hevia Díaz, Jorge Lillo-Box, S. Fernández Menéndez, F. Sánchez Lasheras, S. Pérez Acevedo, R. Pardo Silva, R. MuÃśiz, F. García de la Cuesta, S. L. Suárezi Gómez, J. Menéndez Blanco, F. Izquierdo-Ruiz, P. Padilla Tijerin, John H. Livingston, F. J. de Cos Juez, J. Polancos Ruiz, A. Coya Lozano, E. Díez Alonso, J. González-Nuevo, Laura Bonavera, and C. Rodríguez Pereira
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Light curve, Ephemeris, 01 natural sciences, Exoplanet, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Transit (astronomy), 10. No inequality, 010303 astronomy & astrophysics, Circumstellar habitable zone, Commensurability (astronomy), Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first results of K2-OjOS, a collaborative project between professional and amateur astronomers primarily aimed to detect, characterize, and validate new extrasolar planets. For this work, 10 amateur astronomers looked for planetary signals by visually inspecting the 20 427 light curves of K2 campaign 18 (C18). They found 42 planet candidates, of which 18 are new detections and 24 had been detected in the overlapping C5 by previous works. We used archival photometric and spectroscopic observations, as well as new high-spatial resolution images in order to carry out a complete analysis of the candidates found, including a homogeneous characterization of the host stars, transit modelling, search for transit timing variations and statistical validation. As a result, we report four new planets (K2-355 b, K2-356 b, K2-357 b, and K2-358 b) and 14 planet candidates. Besides, we refine the transit ephemeris of the previously published planets and candidates by modelling C5, C16 (when available) and C18 photometric data jointly, largely improving the period and mid-transit time precision. Regarding individual systems, we highlight the new planet K2-356 b and candidate EPIC 211537087.02 being near a 2:1 period commensurability, the detection of significant TTVs in the bright star K2-184 (V = 10.35), the location of K2-103 b inside the habitable zone according to optimistic models, the detection of a new single transit in the known system K2-274, and the disposition reassignment of K2-120 b, which we consider as a planet candidate as the origin of the signal cannot be ascertained., Accepted for publication in MNRAS
Published: 2021

15. Tomography-based observational measurements of the halo mass function via the submillimeter magnification bias

Author: M. M. Cueli, L. Bonavera, J. González-Nuevo, D. Crespo, J. M. Casas, and A. Lapi
Subjects: submillimeter: galaxies, gravitational lensing: weak, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, galaxies, halos, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. The main goal of this paper is to derive observational constraints on the halo mass fuction (HMF) by performing a tomographic analysis of the magnification bias signal on a sample of background submillimeter galaxies. The results can then be compared with those from a non-tomographic study. Methods. We measure the cross-correlation function between a sample of foreground GAMA galaxies with spectroscopic redshifts in the range 0.1 z z Results. While the observational constraints on the HMF from the non-tomographic analysis are not stringent, there is a remarkable improvement in terms of uncertainty reduction when tomography is adopted. Moreover, with respect to the traditional ST triple of values from numerical simulations, the results from the three-parameter fit predict a higher number density of halos at masses below ∼1012 M⊙ h−1 at 95% credibility. The two-parameter fit yields even more restricting results, with a larger number density of halos below ∼1013 M⊙ h−1 and a lower one above ∼1014 M⊙ h−1, this time at more than 3σ credibility. Our results are therefore in disagreement with the standard N-body values for the ST fit at 2σ and 3σ, respectively.
Published: 2022

16. Joint Analysis of BICEP2/Keck ArrayandPlanckData

Author: P. A. R. Ade, N. Aghanim, Z. Ahmed, R. W. Aikin, K. D. Alexander, M. Arnaud, J. Aumont, C. Baccigalupi, A. J. Banday, D. Barkats, R. B. Barreiro, J. G. Bartlett, N. Bartolo, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, S. J. Benton, J.-P. Bernard, M. Bersanelli, P. Bielewicz, C. A. Bischoff, J. J. Bock, A. Bonaldi, L. Bonavera, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, J. A. Brevik, M. Bucher, I. Buder, E. Bullock, C. Burigana, R. C. Butler, V. Buza, E. Calabrese, J.-F. Cardoso, A. Catalano, A. Challinor, R.-R. Chary, H. C. Chiang, P. R. Christensen, L. P. L. Colombo, C. Combet, J. Connors, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, J.-M. Delouis, F.-X. Désert, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, C. D. Dowell, L. Duband, A. Ducout, J. Dunkley, X. Dupac, C. Dvorkin, G. Efstathiou, F. Elsner, T. A. Enßlin, H. K. Eriksen, E. Falgarone, J. P. Filippini, F. Finelli, S. Fliescher, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, A. Frejsel, S. Galeotta, S. Galli, K. Ganga, T. Ghosh, M. Giard, E. Gjerløw, S. R. Golwala, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, J. E. Gudmundsson, M. Halpern, F. K. Hansen, D. Hanson, D. L. Harrison, M. Hasselfield, G. Helou, S. Henrot-Versillé, D. Herranz, S. R. Hildebrandt, G. C. Hilton, E. Hivon, M. Hobson, W. A. Holmes, W. Hovest, V. V. Hristov, K. M. Huffenberger, H. Hui, G. Hurier, K. D. Irwin, A. H. Jaffe, T. R. Jaffe, J. Jewell, W. C. Jones, M. Juvela, A. Karakci, K. S. Karkare, J. P. Kaufman, B. G. Keating, S. Kefeli, E. Keihänen, S. A. Kernasovskiy, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, J. M. Kovac, N. Krachmalnicoff, M. Kunz, C. L. Kuo, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J.-M. Lamarre, A. Lasenby, M. Lattanzi, C. R. Lawrence, E. M. Leitch, R. Leonardi, F. Levrier, A. Lewis, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, M. Lueker, J. F. Macías-Pérez, B. Maffei, D. Maino, N. Mandolesi, A. Mangilli, M. Maris, P. G. Martin, E. Martínez-González, S. Masi, P. Mason, S. Matarrese, K. G. Megerian, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M.-A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, A. Moss, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, H. T. Nguyen, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, R. O’Brient, R. W. Ogburn, A. Orlando, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, B. Partridge, F. Pasian, G. Patanchon, T. J. Pearson, O. Perdereau, L. Perotto, V. Pettorino, F. Piacentini, M. Piat, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, G. W. Pratt, S. Prunet, C. Pryke, J.-L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, A. Renzi, S. Richter, I. Ristorcelli, G. Rocha, M. Rossetti, G. Roudier, M. Rowan-Robinson, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, D. Santos, M. Savelainen, G. Savini, R. Schwarz, D. Scott, M. D. Seiffert, C. D. Sheehy, L. D. Spencer, Z. K. Staniszewski, V. Stolyarov, R. Sudiwala, R. Sunyaev, D. Sutton, A.-S. Suur-Uski, J.-F. Sygnet, J. A. Tauber, G. P. Teply, L. Terenzi, K. L. Thompson, L. Toffolatti, J. E. Tolan, M. Tomasi, M. Tristram, M. Tucci, A. D. Turner, L. Valenziano, J. Valiviita, B. Van Tent, L. Vibert, P. Vielva, A. G. Vieregg, F. Villa, L. A. Wade, B. D. Wandelt, R. Watson, A. C. Weber, I. K. Wehus, M. White, S. D. M. White, J. Willmert, C. L. Wong, K. W. Yoon, D. Yvon, A. Zacchei, and A. Zonca
Published: 2015
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17. Cosmology with the submillimetre galaxies magnification bias: Tomographic analysis

Author: D. Crespo, M. M. Cueli, Laura Bonavera, T. Ronconi, J. González-Nuevo, J. M. Casas, Andrea Lapi, and M. Migliaccio
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmological parameters, Galaxies: high-redshift, FOS: Physical sciences, Order (ring theory), Astronomy and Astrophysics, Astrophysics, Halo occupation distribution, Omega, Cosmology, Redshift, Galaxy, Gravitational lens, Submillimeter: galaxies, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Gravitational lensing: weak, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: As in Gonzalez-Nuevo et al. 2017 and Bonavera et al. 2019, the high-z sub-millimetre galaxies can be used as background sample for gravitational lensing studies thanks to their magnification bias. In particular, as in Bonavera et al. 2020 the magnification bias can be exploited in order to constrain the free parameters of a Halo Occupation Distribution (HOD) model and some of the main cosmological parameters. In this work the magnification bias has been evaluated as cosmological tool in a tomographic set up. The cross-correlation function (CCF) data have been used to jointly constrain the astrophysical parameters $M_{min}$, $M_{1}$ and $\alpha$ in each one of the selected redshift bins and the $\Omega_{M}$, $\sigma_{8}$, and $H_0$ cosmological ones ($\Lambda$CDM). Moreover, we explore the possible time evolution of the dark energy density introducing also the $\omega_0, \omega_a$ parameters in the joint analysis ($\omega_0$CDM and $\omega_0\omega_a$CDM). The CCF has been measured between a foreground spectroscopic sample of GAMA galaxies that has been divided into four redshift bins (0.1-0.2, 0.2-0.3, 0.3-0.5 and 0.5-0.8) and a sample of H-ATLAS galaxies with photometric redshifts >1.2. The CCF is modelled using a description that depends on HOD and cosmological parameters that are estimated with MCMC in different cases. For the $\Lambda$CDM model, the analysis yields a maximum posterior value at 0.26 with $[0.17,0.41]$ 68\% C.I. for $\Omega_M$ and at 0.87 with $[0.75,1]$ 68\% C.I. for $\sigma_8$. With our current results $H_0$ is not yet constrained. With the $\omega_0$CDM model, the constraints on $\Omega_M$ and $\sigma_8$ are similar, but we found a maximum posterior value for $\omega_0$ at -1 with $[-1.56, -0.47]$ 68\% C.I. In the $\omega_0\omega_a$CDM model, the results are -1.09 with $[-1.72, -0.66]$ 68\% C.I. for $\omega_0$ and -0.19 with $[-1.88, 1.48]$ 68\% C.I. for $\omega_a$., Comment: accepted A&A
Published: 2021

18. A direct and robust method to observationally constrain the halo mass function via the submillimeter magnification bias: Proof of concept

Author: Laura Bonavera, M. M. Cueli, J. González-Nuevo, and Andrea Lapi
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Halo occupation distribution, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Range (statistics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxies: Halos, Gravitational lensing: Weak, Submillimeter: Galaxies, 010308 nuclear & particles physics, Halo mass function, Astronomy and Astrophysics, Observable, Galaxy, Redshift, Space and Planetary Science, Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. The main purpose of this work is to provide a method to derive tabulated observational constraints on the halo mass function (HMF) by studying the magnification bias effect on high-redshift submillimeter galaxies. Under the assumption of universality, we parametrize the HMF according to two traditional models, namely the Sheth and Tormen (ST) and Tinker fits and assess their performance in explaining the measured data within the {\Lambda} cold dark matter ({\Lambda}CDM) model. We also study the potential influence of the halo occupation distribution (HOD) parameters in this analysis and discuss two important aspects regarding the HMF parametrization. Methods. We measure the cross-correlation function between a foreground sample of GAMA galaxies with redshifts in the range $0.2, Comment: 19 pages, 13 figures, accepted by A&A
Published: 2021

19. Planck 2018 results: VI. Cosmological parameters (Corrigendum)

Author: Jose M. Diego, F. Piacentini, Soumen Basak, M. Frailis, Carlo Baccigalupi, M. Ashdown, H. K. Eriksen, François Levrier, E. Hivon, Reijo Keskitalo, L. Pagano, Hannu Kurki-Suonio, A. Renzi, F. Cuttaia, F. R. Bouchet, F. Villa, R. Fernandez-Cobos, L. Montier, Charles R. Lawrence, R. B. Barreiro, Simon D. M. White, Jean-François Cardoso, Tuhin Ghosh, A. Mennella, Nabila Aghanim, Zhiqi Huang, Hans Ulrik Nørgaard-Nielsen, P. Vielva, R. C. Butler, K. M. Górski, K. Kiiveri, Gianmarco Maggio, P. de Bernardis, Luca Valenziano, Steven Gratton, Lloyd Knox, Andrea Zacchei, Jonathan Aumont, F. K. Hansen, P. Bielewicz, Guilaine Lagache, Jörg P. Rachen, S. R. Hildebrandt, Antony Lewis, M. López-Caniego, D. Herranz, M. Le Jeune, N. Mandolesi, Julien Lesgourgues, Benjamin D. Wandelt, Julian Borrill, Peter G. Martin, Will Handley, L. Vibert, Jens Chluba, Peter Meinhold, Michele Liguori, Jan Hamann, G. Roudier, Diego Molinari, Andrei V. Frolov, J.-M. Delouis, J. González-Nuevo, Aurelien A. Fraisse, M. Sandri, Ingunn Kathrine Wehus, M. Tenti, B. P. Crill, J.-L. Puget, L. Salvati, X. Dupac, Massimiliano Lattanzi, Karim Benabed, Locke D. Spencer, Paolo Natoli, Francesco Forastieri, Nicola Bartolo, Erminia Calabrese, J.-P. Bernard, Marzieh Farhang, J. F. Macías-Pérez, Nicola Vittorio, V. Lindholm, A.-S. Suur-Uski, Adam Moss, E. Franceschi, W. C. Jones, P. Lemos, A. Karakci, D. Tavagnacco, Ricardo Genova-Santos, Tiziana Trombetti, B. Van Tent, Alessandro Gruppuso, Marius Millea, Graca Rocha, Sabino Matarrese, Theodore Kisner, Richard A. Battye, M. Martinelli, A. J. Banday, D. Contreras, J.-M. Lamarre, Ken Ganga, B. Partridge, Yabebal Fantaye, Jan Tauber, N. Mauri, J. J. Bock, Martin Kunz, E. Martínez-González, Jose Alberto Rubino-Martin, A. Ducout, Mathieu Remazeilles, S. Galeotta, Marian Douspis, Chiara Sirignano, O. Doré, Jon E. Gudmundsson, G. de Zotti, Hiranya V. Peiris, Yashar Akrami, Anthony Challinor, Michele Maris, M. Savelainen, Francesca Perrotta, P. B. Lilje, Torsten A. Enßlin, Valeria Pettorino, M. Tomasi, Jacques Delabrouille, Martin Reinecke, Marco Bersanelli, J. B. Kim, G. Sirri, Yin-Zhe Ma, E. P. S. Shellard, Fabio Finelli, S. Dusini, Andrea Zonca, H. C. Chiang, Martin White, M. Bucher, Douglas Scott, A. Mangilli, A. Marcos-Caballero, L. P. L. Colombo, Mario Ballardini, Daniela Paoletti, Jussi Valiviita, George Efstathiou, F. Boulanger, G. Polenta, Julien Carron, L. Toffolatti, Anthony Lasenby, Martina Gerbino, E. Keihänen, Andrew H. Jaffe, Marc-Antoine Miville-Deschênes, Philip Lubin, Davide Maino, M. Lilley, M. Migliaccio, J. R. Bond, B. Ruiz-Granados, Jason D. McEwen, Carlo Burigana, Nicoletta Krachmalnicoff, James R. Fergusson, Subhasish Mitra, C. Combet, R. A. Sunyaev, E. Di Valentino, G. Patanchon, L. Polastri, Alessandro Melchiorri, S. Galli, Gianluca Morgante, Franz Elsner, C. Rosset, and Universidad de Cantabria
Subjects: Physics, Numerical error, 010308 nuclear & particles physics, Astronomy, Cosmological parameters, Astronomy and Astrophysics, Astrophysics, Cosmic background radiation, 01 natural sciences, Upper and lower bounds, Errata, addenda, Combinatorics, symbols.namesake, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Optical depth (astrophysics), symbols, Planck, 010306 general physics
Abstract: Author(s): Aghanim, N; Akrami, Y; Ashdown, M; Aumont, J; Baccigalupi, C; Ballardini, M; Banday, AJ; Barreiro, RB; Bartolo, N; Basak, S; Battye, R; Benabed, K; Bernard, JP; Bersanelli, M; Bielewicz, P; Bock, JJ; Bond, JR; Borrill, J; Bouchet, FR; Boulanger, F; Bucher, M; Burigana, C; Butler, RC; Calabrese, E; Cardoso, JF; Carron, J; Challinor, A; Chiang, HC; Chluba, J; Colombo, LPL; Combet, C; Contreras, D; Crill, BP; Cuttaia, F; De Bernardis, P; De Zotti, G; Delabrouille, J; Delouis, JM; DI Valentino, E; DIego, JM; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Farhang, M; Fergusson, J; Fernandez-Cobos, R; Finelli, F; Forastieri, F; Frailis, M; Fraisse, AA; Franceschi, E; Frolov, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Gerbino, M; Ghosh, T; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gruppuso, A; Gudmundsson, JE; Hamann, J; Handley, W; Hansen, FK; Herranz, D; Hildebrandt, SR; Hivon, E; Huang, Z; Jaffe, AH; Jones, WC; Karakci, A; Keihanen, E; Keskitalo, R; Kiiveri, K; Kim, J; Kisner, TS | Abstract: In the original version, the bounds given in Eqs. (87a) and (87b) on the contribution to the early-time optical depth, (15,30), contained a numerical error in deriving the 95th percentile from the Monte Carlo samples. The corrected 95% upper bounds are: τ(15,30) l 0:018 (lowE, flat τ(15, 30), FlexKnot), (1) τ(15, 30) l 0:023 (lowE, flat knot, FlexKnot): (2) These bounds are a factor of 3 larger than the originally reported results. Consequently, the new bounds do not significantly improve upon previous results from Planck data presented in Millea a Bouchet (2018) as was stated, but are instead comparable. Equations (1) and (2) give results that are now similar to those of Heinrich a Hu (2021), who used the same Planck 2018 data to derive a 95% upper bound of 0.020 using the principal component analysis (PCA) model and uniform priors on the PCA mode amplitudes.
Published: 2021

20. Planck 2018 results

Author: Jean-François Cardoso, A. A. Fraisse, P. Vielva, A. J. Banday, Charles R. Lawrence, Yabebal Fantaye, Alessandro Gruppuso, Krzysztof M. Gorski, J.-L. Puget, B. D. Wandelt, Guilaine Lagache, A. Mangilli, M. López-Caniego, P. de Bernardis, R. B. Barreiro, M.-A. Miville-Deschênes, Matthieu Tristram, K. Kiiveri, M. Frailis, Carlo Baccigalupi, François Levrier, E. Hivon, S. Galli, J. Aumont, François R. Bouchet, A. Renzi, Reijo Keskitalo, Michele Liguori, Sabino Matarrese, Diego Molinari, M. Ashdown, A. Mennella, Nabila Aghanim, F. K. Hansen, A. Ducout, E. Martínez-González, J.-M. Lamarre, B. Partridge, Gianluca Morgante, Yashar Akrami, Anthony Challinor, H. K. Eriksen, L. P. L. Colombo, L. Pagano, L. Patrizii, Marian Douspis, J.-M. Delouis, O. Perdereau, Alessandro Melchiorri, X. Dupac, N. Mandolesi, Andrew H. Jaffe, Hannu Kurki-Suonio, J. A. Tauber, M. Savelainen, M. Tomasi, Mario Ballardini, George Efstathiou, Nicola Bartolo, Andrea Zonca, H. C. Chiang, N. Mauri, O. Doré, L. Vibert, Theodore Kisner, Steven Gratton, Marco Bersanelli, Andrei V. Frolov, L. Salvati, Erminia Calabrese, A. Moneti, L. Montier, J. B. Kim, A.-S. Suur-Uski, Martina Gerbino, G. Sirri, Tuhin Ghosh, J. F. Macías-Pérez, F. Boulanger, P. B. Lilje, J. Valiviita, G. Patanchon, Adam Moss, Ricardo Genova-Santos, M. Migliaccio, Graca Rocha, Zhiqi Huang, C. Combet, E. Falgarone, Valeria Pettorino, Ingunn Kathrine Wehus, M. Bucher, Douglas Scott, D. Tavagnacco, M. Sandri, Jacques Delabrouille, S. Mottet, G. Roudier, J. González-Nuevo, L. Toffolatti, Davide Maino, Julian Borrill, Massimiliano Lattanzi, Will Handley, Jörg P. Rachen, M. Tenti, Anthony Lasenby, Fabio Finelli, E. Keihänen, Tiziana Trombetti, E. Di Valentino, Francesca Perrotta, Sophie Henrot-Versille, E. Franceschi, Gianmarco Maggio, F. Cuttaia, Fabrizio Villa, J.-P. Bernard, Torsten A. Enßlin, D. Herranz, D. Paoletti, Paolo Natoli, A. Karakci, F. Vansyngel, P. Bielewicz, W. C. Jones, Julien Carron, Peter G. Martin, S. Galeotta, Yin-Zhe Ma, K. Benabed, K. Ganga, Jose M. Diego, J. R. Bond, F. Piacentini, Soumen Basak, M. Reinecke, R. A. Sunyaev, Chiara Sirignano, G. de Zotti, F. Couchot, Franz Elsner, B. P. Crill, B. Van Tent, Nicola Vittorio, V. Lindholm, Jason D. McEwen, Martin Kunz, Carlo Burigana, Nicoletta Krachmalnicoff, Mathieu Remazeilles, Jon E. Gudmundsson, A. de Rosa, Locke D. Spencer, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), 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), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire de l'Accélérateur Linéaire (LAL), 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), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-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 Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), 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), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Planck, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-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)-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), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Aghanim N., 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., Boulanger F., Bucher M., Burigana C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Colombo L.P.L., Combet C., Couchot F., Crill B.P., Cuttaia F., De Bernardis P., De Rosa A., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Falgarone E., Fantaye Y., Finelli F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Handley W., Hansen F.K., Henrot-Versille S., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Karakci A., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Levrier F., Liguori M., Lilje P.B., Lindholm V., Lopez-Caniego M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Melchiorri A., Mennella A., Migliaccio M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Mottet S., Natoli P., Pagano L., Paoletti D., Partridge B., Patanchon G., Patrizii L., Perdereau O., Perrotta F., Pettorino V., Piacentini F., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Roudier G., Salvati L., Sandri M., Savelainen M., Scott D., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Tristram M., Trombetti T., Valiviita J., Vansyngel F., Van Tent B., Vibert L., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., Zonca A., Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universidad de Cantabria, Department of Physics, Helsinki Institute of Physics, and Doctoral Programme in Particle Physics and Universe Sciences
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astronomy, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics, cosmic background radiation, Surveys, 01 natural sciences, Cosmology: observation, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, surveys, 0103 physical sciences, Calibration, Planck, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, Reionization, LATITUDE MOLECULAR GAS, Physics, SPECTRUM, 010308 nuclear & particles physics, cosmology: observations, methods: data analysis, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 115 Astronomy, Space science, Computational physics, MODEL, Dipole, Amplitude, SKY MAPS, Cosmic background radiation, Cosmology: observations, Methods: data analysis, Surveys, Space and Planetary Science, SEPARATION, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Methods: data analysi
Abstract: Planck Collaboration: et al., This paper presents the High Frequency Instrument (HFI) data processing procedures for the Planck 2018 release. Major improvements in mapmaking have been achieved since the previous Planck 2015 release, many of which were used and described already in an intermediate paper dedicated to the Planck polarized data at low multipoles. These improvements enabled the first significant measurement of the reionization optical depth parameter using Planck-HFI data. This paper presents an extensive analysis of systematic effects, including the use of end-to-end simulations to facilitate their removal and characterize the residuals. The polarized data, which presented a number of known problems in the 2015 Planck release, are very significantly improved, especially the leakage from intensity to polarization. Calibration, based on the cosmic microwave background (CMB) dipole, is now extremely accurate and in the frequency range 100–353 GHz reduces intensity-to-polarization leakage caused by calibration mismatch. The Solar dipole direction has been determined in the three lowest HFI frequency channels to within one arc minute, and its amplitude has an absolute uncertainty smaller than 0.35 μK, an accuracy of order 10−4. This is a major legacy from the Planck HFI for future CMB experiments. The removal of bandpass leakage has been improved for the main high-frequency foregrounds by extracting the bandpass-mismatch coefficients for each detector as part of the mapmaking process; these values in turn improve the intensity maps. This is a major change in the philosophy of “frequency maps”, which are now computed from single detector data, all adjusted to the same average bandpass response for the main foregrounds. End-to-end simulations have been shown to reproduce very well the relative gain calibration of detectors, as well as drifts within a frequency induced by the residuals of the main systematic effect (analogue-to-digital convertor non-linearity residuals). Using these simulations, we have been able to measure and correct the small frequency calibration bias induced by this systematic effect at the 10−4 level. There is no detectable sign of a residual calibration bias between the first and second acoustic peaks in the CMB channels, at the 10−3 level., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, 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); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planckcollaboration.
Published: 2020

21. The Hyper-Kamiokande Experiment -- Snowmass LOI

Author: Hyper-Kamiokande Collaboration, K. Abe, P. Adrich, H. Aihara, R. Akutsu, I. Alekseev, A. Ali, F. Ameli, L. H. V. Anthony, A. Araya, Y. Asaoka, V. Aushev, I. Bandac, M. Barbi, G. Barr, M. Batkiewicz-Kwasniak, M. Bellato, V. Berardi, L. Bernard, E. Bernardini, L. Berns, S. Bhadra, J. Bian, A. Blanchet, A. Blondel, A. Boiano, S. Bolognesi, L. Bonavera, S. Borjabad, T. Boschi, D. Bose, S . B. Boyd, C. Bozza, A. Bravar, C. Bronner, A. Bubak, A. Buchowicz, M. Buizza Avanzini, F. S. Cafagna, N. F. Calabria, J. M. Calvo-Mozota, S. Cao, M. G. Catanesi, S. Chakraborty, J. H. Choi, S. Choubey, M. Cicerchia, J. Coleman, G. Collazuol, S. Cuen-Rochin, M. Danilov, E. De la Fuente, P. de Perio, G. De Rosa, T. Dealtry, C. J. Densham, A. Dergacheva, N. Deshmukh, M. M. Devi, F. Di Lodovico, P. Di Meo, I. Di Palma, T. A. Doyle, E. Drakopoulou, O. Drapier, J. Dumarchez, L. Eklund, S. El Hedri, J. Ellis, S. Emery, A. Esmaili, S. Fedotov, J. Feng, E. Fernández-Martinez, P. Ferrario, B. Ferrazzi, A. Finch, C. Finley, G. Fiorillo, M. Fitton, M. Friend, Y. Fujii, Y. Fukuda, G. Galinski, J. Gao, C. Garde, A. Garfagnini, S. Garode, L. Gialanella, C. Giganti, J. J. Gomez-Cadenas, M. Gonin, J. González-Nuevo, A. Gorin, R. Gornea, F. Gramegna, M. Grassi, G. Grella, M. Guigue, D. R. Hadley, M. Harada, M. Hartz, S. Hassani, N. C. Hastings, Y. Hayato, K. Hiraide, K. Hoshina, K. Hultqvist, F. Iacob, A. K. Ichikawa, W. Idrissi Ibnsalih, M. Ikeda, M. Inomoto, A. Ioannisian, T. Ishida, K. Ishidoshiro, H. Ishino, M. Ishitsuka, H. Ito, S. Ito, Y. Itow, K. Iwamoto, N. Izumi, S. Izumiyama, M. Jakkapu, B. Jamieson, J. S. Jang, H. S. Jo, P. Jonsson, K. K. Joo, T. Kajita, H. Kakuno, J. Kameda, Y. Kano, D. Karlen, Y. Kataoka, A. Kato, T. Katori, N. Kazarian, M. Khabibullin, A. Khotjantsev, T. Kikawa, J. Y. Kim, S. B. Kim, S. King, T. Kinoshita, J. Kisiel, A. Klekotko, T. Kobayashi, L. Koerich, N. Kolev, A. Konaka, L. L. Kormos, Y. Koshio, Y. Kotsar, K. A. Kouzakov, K. L. Kowalik, L. Kravchuk, A. P. Kryukov, Y. Kudenko, T. Kumita, R. Kurjata, T. Kutter, M. Kuze, K. Kwak, M. La Commara, L. Labarga, J. Lagoda, M. Lamoureux, M. Laveder, L. Lavitola, J. Lee, R. Leitner, V. Lezaun, I. T. Lim, T. Lindner, R. P. Litchfield, K. R. Long, A. Longhin, P. Loverre, X. Lu, L. Ludovici, Y. Maekawa, L. Magaletti, K. Magar, Y. Makida, M. Malek, M. Malinský, T. Marchi, C. Mariani, A. Marinelli, K. Martens, Ll. Marti, J. F. Martin, D. Martin, J. Marzec, T. Matsubara, R. Matsumoto, N. McCauley, A. Medhi, P. Mehta, L. Mellet, H. Menjo, M. Mezzetto, J. Migenda, P. Migliozzi, S. Miki, A. Minamino, S. Mine, O. Mineev, A. Mitra, M. Miura, R. Moharana, C. M. Mollo, T. Mondal, M. Mongelli, F. Monrabal, D. H. Moon, C. S. Moon, S. Moriyama, T. Mueller, Y. Nagao, T. Nakadaira, K. Nakagiri, M. Nakahata, S. Nakai, Y. Nakajima, K. Nakamura, KI. Nakamura, H. Nakamura, Y. Nakano, T. Nakaya, S. Nakayama, K. Nakayoshi, L. Nascimento Machado, C. E. R. Naseby, B. Navarro-Garcia, M. Needham, K. Niewczas, Y. Nishimura, F. Nova, J. C. Nugent, H. Nunokawa, W. Obrebski, J. P. Ochoa-Ricoux, E. O'Connor, N. Ogawa, T. Ogitsu, K. Okamoto, H. M. O'Keeffe, K. Okumura, Y. Onishchuk, F. Orozco-Luna, A. Oshlianskyi, N. Ospina, M. Ostrowski, E. O'Sullivan, Y. Oyama, H. Ozaki, M. Y. Pac, P. Paganini, V. Palladino, M. Pari, J. Pasternak, C. Pastore, G. Pastuszak, D. A. Patel, M. Pavin, D. Payne, C. Peña-Garay, C. Pidcott, S. Playfer, B. W. Pointon, A. Popov, B. Popov, K. Porwit, M. Posiadala-Zezula, G. Pronost, N. W. Prouse, B. Quilain, A. A. Quiroga, E. Radicioni, B. Radics, P. J. Rajda, M. Rescigno, G. Ricciardi, B. Richards, E. Rondio, B. Roskovec, S. Roth, C. Rott, A. Rubbia, A. C. Ruggeri, S. Russo, A. Rychter, D. Ryu, K. Sakashita, S. Samani, F. Sánchez, M. L. Sánchez, S. Sano, J. D. Santos, G. Santucci, P. Sarmah, K. Sato, M. Scott, Y. Seiya, T. Sekiguchi, H. Sekiya, J. W. Seo, D. Sgalaberna, A. Shaykina, I. Shimizu, C. D. Shin, M. Shinoki, M. Shiozawa, N. Skrobova, K. Skwarczynski, M. B. Smy, J. Sobczyk, H. W. Sobel, F. J. P. Soler, Y. Sonoda, R. Spina, B. Spisso, P. Spradlin, K. L. Stankevich, L. Stawarz, S. M. Stellacci, A. I. Studenikin, S. L. Suárez Gómez, T. Suganuma, S. Suvorov, Y. Suwa, A. T. Suzuki, S. Suzuki, Y. Suzuki, D. Svirida, M. Taani, M. Tada, A. Takeda, Y. Takemoto, A. Takenaka, A. Taketa, Y. Takeuchi, H. Tanaka, H. I. Tanaka, M. Tanaka, T. Tashiro, M. Thiesse, L. F. Thompson, A. K. Tomatani-Sánchez, G. Tortone, K. M. Tsui, T. Tsukamoto, M. Tzanov, Y. Uchida, M. R. Vagins, S. Valder, V. Valentino, G. Vasseur, A. Vijayvargi, W. G. S. Vinning, D. Vivolo, R. B. Vogelaar, M. M. Vyalkov, T. Wachala, J. Walker, D. Wark, M. O. Wascko, R. A. Wendell, J. R. Wilson, S. Wronka, J. Xia, Y. Yamaguchi, K. Yamamoto, T. Yano, N. Yershov, M. Yokoyama, J. Yoo, I. Yu, T. Zakrzewski, B. Zaldivar, J. Zalipska, K. Zaremba, G. Zarnecki, M. Ziembicki, K. Zietara, M. Zito, S. Zsoldos, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Hyper-Kamiokande, HEP, INSPIRE, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Collaboration, Hyper-Kamiokande, Abe, K., Adrich, P., Aihara, H., Akutsu, R., Alekseev, I., Ali, A., Ameli, F., Anthony, L. H. V., Araya, A., Asaoka, Y., Aushev, V., Bandac, I., Barbi, M., Barr, G., Batkiewicz-Kwasniak, M., Bellato, M., Berardi, V., Bernard, L., Bernardini, E., Berns, L., Bhadra, S., Bian, J., Blanchet, A., Blondel, A., Boiano, A., Bolognesi, S., Bonavera, L., Borjabad, S., Boschi, T., Bose, D., Boyd, S . B., Bozza, C., Bravar, A., Bronner, C., Bubak, A., Buchowicz, A., Buizza Avanzini, M., Cafagna, F. S., Calabria, N. F., Calvo-Mozota, J. M., Cao, S., Catanesi, M. G., Chakraborty, S., Choi, J. H., Choubey, S., Cicerchia, M., Coleman, J., Collazuol, G., Cuen-Rochin, S., Danilov, M., De la Fuente, E., de Perio, P., De Rosa, G., Dealtry, T., Densham, C. J., Dergacheva, A., Deshmukh, N., Devi, M. M., Di Lodovico, F., Di Meo, P., Di Palma, I., Doyle, T. A., Drakopoulou, E., Drapier, O., Dumarchez, J., Eklund, L., El Hedri, S., Ellis, J., Emery, S., Esmaili, A., Fedotov, S., Feng, J., Fernández-Martinez, E., Ferrario, P., Ferrazzi, B., Finch, A., Finley, C., Fiorillo, G., Fitton, M., Friend, M., Fujii, Y., Fukuda, Y., Galinski, G., Gao, J., Garde, C., Garfagnini, A., Garode, S., Gialanella, L., Giganti, C., Gomez-Cadenas, J. J., Gonin, M., González-Nuevo, J., Gorin, A., Gornea, R., Gramegna, F., Grassi, M., Grella, G., Guigue, M., Hadley, D. R., Harada, M., Hartz, M., Hassani, S., Hastings, N. C., Hayato, Y., Hiraide, K., Hoshina, K., Hultqvist, K., Iacob, F., Ichikawa, A. K., Idrissi Ibnsalih, W., Ikeda, M., Inomoto, M., Ioannisian, A., Ishida, T., Ishidoshiro, K., Ishino, H., Ishitsuka, M., Ito, H., Ito, S., Itow, Y., Iwamoto, K., Izumi, N., Izumiyama, S., Jakkapu, M., Jamieson, B., Jang, J. S., Jo, H. S., Jonsson, P., Joo, K. K., Kajita, T., Kakuno, H., Kameda, J., Kano, Y., Karlen, D., Kataoka, Y., Kato, A., Katori, T., Kazarian, N., Khabibullin, M., Khotjantsev, A., Kikawa, T., Kim, J. Y., Kim, S. B., King, S., Kinoshita, T., Kisiel, J., Klekotko, A., Kobayashi, T., Koerich, L., Kolev, N., Konaka, A., Kormos, L. L., Koshio, Y., Kotsar, Y., Kouzakov, K. A., Kowalik, K. L., Kravchuk, L., Kryukov, A. P., Kudenko, Y., Kumita, T., Kurjata, R., Kutter, T., Kuze, M., Kwak, K., La Commara, M., Labarga, L., Lagoda, J., Lamoureux, M., Laveder, M., Lavitola, L., Lee, J., Leitner, R., Lezaun, V., Lim, I. T., Lindner, T., Litchfield, R. P., Long, K. R., Longhin, A., Loverre, P., Lu, X., Ludovici, L., Maekawa, Y., Magaletti, L., Magar, K., Makida, Y., Malek, M., Malinský, M., Marchi, T., Mariani, C., Marinelli, A., Martens, K., Marti, Ll., Martin, J. F., Martin, D., Marzec, J., Matsubara, T., Matsumoto, R., Mccauley, N., Medhi, A., Mehta, P., Mellet, L., Menjo, H., Mezzetto, M., Migenda, J., Migliozzi, P., Miki, S., Minamino, A., Mine, S., Mineev, O., Mitra, A., Miura, M., Moharana, R., Mollo, C. M., Mondal, T., Mongelli, M., Monrabal, F., Moon, D. H., Moon, C. S., Moriyama, S., Mueller, T., Nagao, Y., Nakadaira, T., Nakagiri, K., Nakahata, M., Nakai, S., Nakajima, Y., Nakamura, K., Nakamura, Ki., Nakamura, H., Nakano, Y., Nakaya, T., Nakayama, S., Nakayoshi, K., Nascimento Machado, L., Naseby, C. E. R., Navarro-Garcia, B., Needham, M., Niewczas, K., Nishimura, Y., Nova, F., Nugent, J. C., Nunokawa, H., Obrebski, W., Ochoa-Ricoux, J. P., O'Connor, E., Ogawa, N., Ogitsu, T., Okamoto, K., O'Keeffe, H. M., Okumura, K., Onishchuk, Y., Orozco-Luna, F., Oshlianskyi, A., Ospina, N., Ostrowski, M., O'Sullivan, E., Oyama, Y., Ozaki, H., Pac, M. Y., Paganini, P., Palladino, V., Pari, M., Pasternak, J., Pastore, C., Pastuszak, G., Patel, D. A., Pavin, M., Payne, D., Peña-Garay, C., Pidcott, C., Playfer, S., Pointon, B. W., Popov, A., Popov, B., Porwit, K., Posiadala-Zezula, M., Pronost, G., Prouse, N. W., Quilain, B., Quiroga, A. A., Radicioni, E., Radics, B., Rajda, P. J., Rescigno, M., Ricciardi, G., Richards, B., Rondio, E., Roskovec, B., Roth, S., Rott, C., Rubbia, A., Ruggeri, A. C., Russo, S., Rychter, A., Ryu, D., Sakashita, K., Samani, S., Sánchez, F., Sánchez, M. L., Sano, S., Santos, J. D., Santucci, G., Sarmah, P., Sato, K., Scott, M., Seiya, Y., Sekiguchi, T., Sekiya, H., Seo, J. W., Sgalaberna, D., Shaykina, A., Shimizu, I., Shin, C. D., Shinoki, M., Shiozawa, M., Skrobova, N., Skwarczynski, K., Smy, M. B., Sobczyk, J., Sobel, H. W., Soler, F. J. P., Sonoda, Y., Spina, R., Spisso, B., Spradlin, P., Stankevich, K. L., Stawarz, L., Stellacci, S. M., Studenikin, A. I., Suárez Gómez, S. L., Suganuma, T., Suvorov, S., Suwa, Y., Suzuki, A. T., Suzuki, S., Suzuki, Y., Svirida, D., Taani, M., Tada, M., Takeda, A., Takemoto, Y., Takenaka, A., Taketa, A., Takeuchi, Y., Tanaka, H., Tanaka, H. I., Tanaka, M., Tashiro, T., Thiesse, M., Thompson, L. F., Tomatani-Sánchez, A. K., Tortone, G., Tsui, K. M., Tsukamoto, T., Tzanov, M., Uchida, Y., Vagins, M. R., Valder, S., Valentino, V., Vasseur, G., Vijayvargi, A., Vinning, W. G. S., Vivolo, D., Vogelaar, R. B., Vyalkov, M. M., Wachala, T., Walker, J., Wark, D., Wascko, M. O., Wendell, R. A., Wilson, J. R., Wronka, S., Xia, J., Yamaguchi, Y., Yamamoto, K., Yano, T., Yershov, N., Yokoyama, M., Yoo, J., Yu, I., Zakrzewski, T., Zaldivar, B., Zalipska, J., Zaremba, K., Zarnecki, G., Ziembicki, M., Zietara, K., Zito, M., and Zsoldos, S.
Subjects: nucleon: decay, Physics - Instrumentation and Detectors, [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], Cherenkov counter: water, Physics::Instrumentation and Detectors, J-PARC Lab, High Energy Physics::Phenomenology, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), KAMIOKANDE, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], upgrade, High Energy Physics::Experiment, Physics - Instrumentation and Detector, neutrino: oscillation, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], activity report
Abstract: Hyper-Kamiokande is the next generation underground water Cherenkov detector that builds on the highly successful Super-Kamiokande experiment. The detector which has an 8.4~times larger effective volume than its predecessor will be located along the T2K neutrino beamline and utilize an upgraded J-PARC beam with 2.6~times beam power. Hyper-K's low energy threshold combined with the very large fiducial volume make the detector unique, that is expected to acquire an unprecedented exposure of 3.8~Mton$\cdot$year over a period of 20~years of operation. Hyper-Kamiokande combines an extremely diverse science program including nucleon decays, long-baseline neutrino oscillations, atmospheric neutrinos, and neutrinos from astrophysical origins. The scientific scope of this program is highly complementary to liquid-argon detectors for example in sensitivity to nucleon decay channels or supernova detection modes. Hyper-Kamiokande construction has started in early 2020 and the experiment is expected to start operations in 2027. The Hyper-Kamiokande collaboration is presently being formed amongst groups from 19 countries including the United States, whose community has a long history of making significant contributions to the neutrino physics program in Japan. US physicists have played leading roles in the Kamiokande, Super-Kamiokande, EGADS, K2K, and T2K programs., 6 pages, prepared as Snowmass2021 LOI
Published: 2020

22. IRAM 30-m-EMIR redshift search of z = 3-4 lensed dusty starbursts selected from the HerBS sample

Author: Steve Serjeant, Tom J. L. C. Bakx, P. van der Werf, S. Urquhart, M. W. L. Smith, J. González-Nuevo, Helmut Dannerbauer, G. de Zotti, Andrea Lapi, Zhen-Yi Cai, David L. Clements, Mattia Negrello, Ismael Perez-Fournon, Rob Ivison, Pasquale Temi, David T. Frayer, Michał J. Michałowski, and Stephen Anthony Eales
Subjects: FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Settore FIS/05 - Astronomia e Astrofisica, law, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Sample (graphics), Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), gravitational lensing: strong – galaxies: high-redshift – submillimetre: galaxies, submillimetre: galaxies
Abstract: Using the EMIR instrument on the IRAM 30m telescope, we conducted a spectroscopic redshift search of seven z$_{\rm phot}$ $\sim$ 4 sub-millimetre bright galaxies selected from the Herschel Bright Sources (HerBS) sample with fluxes at 500 $��$m greater than 80 mJy. For four sources, we obtained spectroscopic redshifts between 3.4 < z < 4.1 through the detection of multiple CO-spectral lines with J $\leq$ 3. Later, we detected low-J transitions for two of these sources with the GBT including the CO(1-0) transition. For the remaining three sources, more data are needed to determine the spectroscopic redshift unambiguously. The measured CO luminosities and line widths suggest that all these sources are gravitationally lensed. These observations demonstrate that the 2 mm window is indispensable to confirm robust spectroscopic redshifts for z < 4 sources. Finally, we present an efficient graphical method to correctly identify spectroscopic redshifts., 20 Pages, 8 Figures + 7 Appendix Figures + 1 animated figure. Resubmitted in order to reflect the version as printed in MNRAS
Published: 2020

23. SCUBA-2 overdensities associated with candidate protoclusters selected from Planck data

Author: J. Greenslade, Asantha Cooray, Pasquale Temi, Lerothodi Leonard Leeuw, Michał J. Michałowski, T. Cheng, Edo Ibar, Jingzhe Ma, J. González-Nuevo, L. Conversi, Lingyu Wang, G. de Zotti, Paola Andreani, M. N. Bremer, Helmut Dannerbauer, Douglas Scott, Hooshang Nayyeri, David L. Clements, E. van Kampen, Stephen Anthony Eales, Joseph Cairns, Mattia Vaccari, Dominik Riechers, I. Valtchanov, and Astronomy
Subjects: FOS: Physical sciences, galaxies: starburst, Astrophysics, Astronomy & Astrophysics, Intermediate level, 01 natural sciences, LYMAN BREAK GALAXIES, STAR-FORMATION, PROTO-CLUSTER, symbols.namesake, galaxies: high-redshift, 0201 Astronomical and Space Sciences, 0103 physical sciences, galaxies [submillimetre], Sample variance, Planck, 010303 astronomy & astrophysics, Physics, HERSCHEL, Science & Technology, SPECTROSCOPY, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, Star formation, starburst [galaxies], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, symbols, MORPHOLOGY, HIGH-REDSHIFT, submillimetre: galaxies, high-redshift [galaxies], COSMOLOGY LEGACY SURVEY
Abstract: We measure the 850-$\mu$m source densities of 46 candidate protoclusters selected from the Planck High-z catalogue (PHz) and the Planck Catalogue of Compact Sources (PCCS) that were followed up with Herschel-SPIRE and SCUBA-2. This paper aims to search for overdensities of 850-$\mu$m sources in order to select the fields that are most likely to be genuine protoclusters. Of the 46 candidate protoclusters, 25 have significant overdensities ($>$5 times the field counts), 11 have intermediate overdensities (3--5 times the field counts) and 10 have no overdensity ($, Comment: 8 pages, 1 figure, 1 table, accepted for publication in MNRAS
Published: 2020

24. Planck intermediate results

Author: E. Franceschi, Erminia Calabrese, Michael P. Hobson, Jose M. Diego, S. Galeotta, Yashar Akrami, L. Toffolatti, F. Piacentini, M. Tenti, X. Dupac, Paolo Natoli, M. Ashdown, A. Renzi, M. Savelainen, M. Migliaccio, N. Mandolesi, Eric Hivon, Tiziana Trombetti, J. Aumont, E. Keihänen, Peter G. Martin, Francesca Perrotta, Torsten A. Enßlin, M. López-Caniego, Fabrizio Villa, J.-P. Bernard, J. González-Nuevo, Ingunn Kathrine Wehus, G. de Zotti, Zhiqi Huang, P. Bielewicz, Valeria Pettorino, F. Cuttaia, W. C. Jones, Alessandro Gruppuso, R. Fernandez-Cobos, Julian Borrill, Will Handley, H. K. Eriksen, G. Sirri, Carlo Baccigalupi, R. B. Barreiro, Serge Gratton, J.-M. Delouis, Jacques Delabrouille, Gianluca Morgante, J.-M. Lamarre, Jan Tauber, François Levrier, M. Reinecke, B. P. Crill, Anthony Lasenby, Charles R. Lawrence, B. Van Tent, F. K. Hansen, Yin-Zhe Ma, Douglas Scott, M. Le Jeune, Hannu Kurki-Suonio, Fabio Finelli, L. A. Montier, N. Bartolo, Franz Elsner, M. Tomasi, Martin Kunz, V. Lindholm, Mathieu Remazeilles, Ken Ganga, Andrea Zacchei, P. Vielva, Ted Kisner, Krzysztof M. Gorski, G. Polenta, G. Roudier, E. Di Valentino, A. Marcos-Caballero, Diego Molinari, Jon E. Gudmundsson, Marco Bersanelli, A. De Rosa, Jason D. McEwen, G. Maggio, B. Ruiz-Granados, A.-S. Suur-Uski, François R. Bouchet, John Bond, Carlo Burigana, Nicoletta Krachmalnicoff, A. A. Fraisse, Mario Ballardini, Enrique Martínez-González, Daniela Paoletti, Locke D. Spencer, George Efstathiou, Andrei V. Frolov, N. Mauri, A. J. Banday, Karim Benabed, S. Dusini, Andrea Zonca, P. B. Lilje, H. C. Chiang, J. Kim, Reijo Keskitalo, Jussi Valiviita, M. Maris, P. Carvalho, Martina Gerbino, J. F. Macías-Pérez, Graca Rocha, S. Basak, D. Tavagnacco, A. Moneti, Mario G. Lattanzi, Jörg P. Rachen, J.-L. Puget, Sabino Matarrese, D. Herranz, B. Partridge, Universidad de Cantabria, Ministerio de Economía y Competitividad (España), European Commission, Consejo Superior de Investigaciones Científicas (España), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Brest (UBO), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Université Paris sciences et lettres (PSL), Cavendish Laboratory, University of Cambridge [UK] (CAM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), SISSA MathLab [Trieste], University of the Western Cape, Instituto de Física de Cantabria (IFCA), Universidad de Cantabria [Santander]-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, Indian Institute of Science Education and Research Thiruvananthapuram (IISER TVM), Università degli Studi di Milano [Milano] (UNIMI), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Dipartimento di Fisica e Scienze della Terra [Ferrara], Università degli Studi di Ferrara (UniFE), Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Universidade Federal de Mato Grosso (UFMT), Algorithmes Parallèles et Optimisation (IRIT-APO), Institut de recherche en informatique de Toulouse (IRIT), Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, Institut National Polytechnique (Toulouse) (Toulouse INP), Princeton University, Oskar Klein Centre [Stockholm], Stockholm University, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Helsinki Institute of Physics (HIP), University of Helsinki, Aalto University, University of British Columbia (UBC), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (INFN, Sezione di Bologna), Istituto Nazionale di Fisica Nucleare (INFN), Cardiff University, European Space Research and Technology Centre (ESTEC), INAF - Osservatorio Astronomico di Trieste (OAT), Universidad de Oviedo [Oviedo], Istituto Nazionale di Fisica Nucleare [Ferrara] (INFN), Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a,POB 64, FI-00014 Helsinki, Finland, Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Basque Centre for Climate Change (BC3), Institute of Theoretical Astrophysics [Oslo], University of Oslo (UiO), San Diego Supercomputer Center [San Diego], NASA (USA), Planck Collaboration, European Project, 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., Gonzalez-Nuevo J., Gorski 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., Keihanen 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., Levrier F., Lilje P.B., Lindholm V., Lopez-Caniego M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Mandolesi N., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez 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., École normale supérieure - Paris (ENS-PSL), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of the Western Cape (UWC), Università degli Studi di Padova = University of Padua (Unipd), Università degli Studi di Milano = University of Milan (UNIMI), Università degli Studi di Ferrara = University of Ferrara (UniFE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Toulouse Mind & Brain Institut (TMBI), Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Agence Spatiale Européenne = European Space Agency (ESA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Department of Physics, Helsinki Institute of Physics, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: Submillimeter: general, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, general [Submillimeter], 7. Clean energy, 01 natural sciences, Cosmology: observation, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Catalogs, Cosmology: observations, Submillimeter: general, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Aerospace engineering, Planck, observations [Cosmology], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Reliability (statistics), Astrophysics::Galaxy Astrophysics, Physics, HERSCHEL, 010308 nuclear & particles physics, business.industry, PE9_14, COMPONENTS, Cosmology: observations, Astronomy and Astrophysics, 115 Astronomy, Space science, Catalogs, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, astro-ph.CO, Catalog, CLUSTERS, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Planck Collaboration: et al., 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; the Herschel GAMA15-field catalogue; and the temperature- and spectral-index-reconstructed dust maps obtained with Planck’s Generalized Needlet Internal Linear Combination method. The results of the BeeP extension of PCCS2, which are made publicly available via the Planck Legacy Archive, will enable the study of the thermal properties of well-defined samples of compact Galactic and extragalactic dusty sources., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, 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 ERC and PRACE (EU).
Published: 2020

25. Missing Data Imputation for Continuous Variables Based on Multivariate Adaptive Regression Splines

Author: Esperanza García-Gonzalo, L. Toffolatti, María Luisa Fernández Sánchez, Paulino José García Nieto, Francisco Javier Rodríguez Iglesias, Jesús Daniel Santos Rodríguez, Francisco Javier de Cos Juez, F. Gomez, Fernando Las-Heras, Susana del Carmen Fernández Menéndez, Ana Sánchez, J. González-Nuevo, and Laura Bonavera
Subjects: Data set, Multivariate statistics, Mahalanobis distance, Multivariate adaptive regression splines, Mean squared error, Computer science, Statistics, Outlier, Imputation (statistics), Missing data
Abstract: The problem of missing data in a database is something that causes frequent difficulties for its processing and analysis. This research presents a new missing data methodology based on multivariate adaptive regression splines (MARS) for missing data imputation. The performance of the proposed method is checked using as input information a database created from the hourly records of environmental stations located in the city of Madrid (Spain). Data analyzed corresponds to hourly measurements from 10th February 2004 to 31st May 2010. The proposed methodology has three variants. The first of these makes use of all the available information in order to calculate different MARS models with the ability to predict missing information based on the available data. In the second case, the MARS models are trained after the removal of 1% of the most extreme cases according to Mahalanobis’ distances, as they are considered outliers. Finally, the third model proposed makes use of the information corresponding only to the previous month in order to calculate the MARS models for the missing data prediction. The results obtained outperformed those given by multivariate imputation by chained equations (MICE) when applied to the same data sets. For a data set with 20% of its information missing, the proposed algorithm outperforms MICE in RMSE values at least in 65.5% of cases, MAE in 75.2% and MAPE in 76%.
Published: 2020

26. Overdensity of SMGs in fields containing z ∼ 0.3 galaxies: Magnification bias and the implications for studies of galaxy evolution

Author: S. J. Maddox, Catherine Vlahakis, Loretta Dunne, Laura Bonavera, and J. González-Nuevo
Subjects: Physics, 010308 nuclear & particles physics, Spectral density, Magnification, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Observational evidence, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, Source counts, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report a remarkable over-density of high-redshift submillimetre galaxies (SMG), 4-7 times the background, around a statistically complete sample of twelve 250-micron selected galaxies at z=0.35, which were targeted by ALMA in a study of gas tracers. This over-density is consistent with the effect of lensing by the halos hosting the target z=0.35 galaxies. The angular cross-correlation in this sample is consistent with statistical measures of this effect made using larger sub-mm samples. The magnitude of the over-density as a function of radial separation is consistent with intermediate scale lensing by halos of order 7x 10^{13} M_o, which should host one or possibly two bright galaxies and several smaller satellites. This is supported by observational evidence of interaction with satellites in four out of the six fields with SMG, and membership of a spectroscopically defined group for a fifth. We also investigate the impact of these SMG on the reported Herschel fluxes of the z=0.35 galaxies, as they produce significant contamination in the 350 and 500-micron Herschel bands. The higher than random incidence of these boosting events implies a significantly larger bias in the sub-mm colours of Herschel sources associated with z, 18 pages, MNRAS accepted
Published: 2020

27. Planck 2018 results. VI. Cosmological parameters

Author: M. López-Caniego, Richard A. Battye, Hannu Kurki-Suonio, J. Aumont, Charles R. Lawrence, P. Vielva, E. Martínez-González, François R. Bouchet, L. Montier, K. Ganga, Francesca Perrotta, Lloyd Knox, M. Le Jeune, Jan Hamann, E. Franceschi, M. Tenti, C. Combet, Torsten A. Enßlin, Andrea Zacchei, R. A. Sunyaev, J.-M. Delouis, J. F. Macías-Pérez, Tiziana Trombetti, Zhiqi Huang, Graca Rocha, L. Polastri, Alessandro Melchiorri, A. Mennella, Nabila Aghanim, Sabino Matarrese, Jose Alberto Rubino-Martin, N. Bartolo, Theodore Kisner, Peter Meinhold, L. Salvati, Jose M. Diego, K. Benabed, J.-P. Bernard, J. González-Nuevo, M. Ashdown, H. K. Eriksen, Erminia Calabrese, Olivier Doré, Serge Gratton, G. de Zotti, L. Vibert, J. R. Bond, Marzieh Farhang, Benjamin D. Wandelt, Julian Borrill, L. Toffolatti, F. Piacentini, Yin-Zhe Ma, Will Handley, S. Galeotta, A. Karakci, A. A. Fraisse, Anthony Lasenby, M. Sandri, X. Dupac, G. Sirri, Adam Moss, B. Ruiz-Granados, D. Contreras, A.-S. Suur-Uski, Mario G. Lattanzi, Ricardo Genova-Santos, Jean-François Cardoso, Marian Douspis, G. Polenta, E. Keihänen, A. J. Banday, M. Migliaccio, R. B. Barreiro, B. P. Crill, J. Valiviita, Yabebal Fantaye, B. Van Tent, Tuhin Ghosh, D. Tavagnacco, A. Renzi, Martin White, M. Bucher, Douglas Scott, Jörg P. Rachen, Hans Ulrik Nørgaard-Nielsen, Jason D. McEwen, R. C. Butler, Locke D. Spencer, Nicola Vittorio, V. Lindholm, Fabrizio Villa, K. Kiiveri, Ingunn Kathrine Wehus, Julien Lesgourgues, Hiranya V. Peiris, Reijo Keskitalo, Krzysztof M. Gorski, S. R. Hildebrandt, E. Di Valentino, A. Marcos-Caballero, G. Patanchon, P. de Bernardis, M. Lilley, Simon D. M. White, C. Sirignano, M. Frailis, Carlo Baccigalupi, Francesco Forastieri, W. C. Jones, P. Lemos, François Levrier, E. Hivon, R. Fernandez-Cobos, Carlo Burigana, Nicoletta Krachmalnicoff, D. Herranz, Andrei V. Frolov, M. Tomasi, Marius Millea, J.-L. Puget, Paolo Natoli, James R. Fergusson, D. Paoletti, L. Pagano, M.-A. Miville-Deschênes, Julien Carron, Luca Valenziano, F. K. Hansen, S. Dusini, Andrea Zonca, Bruce Partridge, Jens Chluba, S. Basak, H. C. Chiang, Alessandro Gruppuso, Marco Bersanelli, Peter G. Martin, Martin Kunz, Valeria Pettorino, Mathieu Remazeilles, Jacques Delabrouille, Jon E. Gudmundsson, J.-M. Lamarre, P. Bielewicz, F. Cuttaia, Franz Elsner, G. Roudier, S. Galli, Michele Liguori, Gianluca Morgante, A. Ducout, Fabio Finelli, James J. Bock, M. Reinecke, C. Rosset, Yashar Akrami, Anthony Challinor, Subhabrata Mitra, J. A. Tauber, Matteo Martinelli, M. Savelainen, N. Mauri, E. P. S. Shellard, Antony Lewis, Diego Molinari, G. Maggio, P. B. Lilje, Davide Maino, A. Mangilli, L. P. L. Colombo, Mario Ballardini, N. Mandolesi, Andrew H. Jaffe, Philip Lubin, J. Kim, M. Maris, Martina Gerbino, George Efstathiou, F. Boulanger, Guilaine Lagache, Challinor, Anthony [0000-0003-3479-7823], Fergusson, James [0000-0003-4820-171X], Handley, William [0000-0002-5866-0445], Lasenby, Anthony [0000-0002-8208-6332], Apollo - University of Cambridge Repository, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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)-Université Grenoble Alpes (UGA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut Lagrange de Paris, Sorbonne Universités, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), 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), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratoire d'Océanographie Physique et Spatiale (LOPS), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University College of London [London] (UCL), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 725456, CMBSPEC)., Planck Collaboration, European Project: 616170,EC:FP7:ERC,ERC-2013-CoG,COSMOPARS(2014), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-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 des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Universita degli Studi di Padova, Sorbonne Université (SU), Science and Technology Facilities Council (STFC), Science and Technology Facilities Council, Universidad de Cantabria, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Department of Physics, Helsinki Institute of Physics, 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)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Aghanim N., Akrami Y., Ashdown M., Aumont J., Baccigalupi C., Ballardini M., Banday A.J., Barreiro R.B., Bartolo N., Basak S., Battye R., Benabed K., Bernard J.-P., Bersanelli M., Bielewicz P., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Butler R.C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Chluba J., Colombo L.P.L., Combet C., Contreras D., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Dusini S., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Farhang M., Fergusson J., Fernandez-Cobos R., Finelli F., Forastieri F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hildebrandt S.R., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Karakci A., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Knox L., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Lemos P., Lesgourgues J., Levrier F., Lewis A., Liguori M., Lilje P.B., Lilley M., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinelli M., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Meinhold P.R., Melchiorri A., Mennella A., Migliaccio M., Millea M., Mitra S., Miville-Deschenes M.-A., Molinari D., Montier L., Morgante G., Moss A., Natoli P., Norgaard-Nielsen H.U., Pagano L., Paoletti D., Partridge B., Patanchon G., Peiris H.V., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Shellard E.P.S., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Trombetti T., Valenziano L., Valiviita J., Van Tent B., Vibert L., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., White M., White S.D.M., Zacchei A., and Zonca A.
Subjects: cosmological model, Astronomy, Cosmic microwave background, INFLATIONARY PARADIGM, cosmic background radiation: polarization, Astrophysics, cosmic background radiation, baryon: oscillation: acoustic, 01 natural sciences, 7. Clean energy, Omega, Cosmology, OSCILLATION SPECTROSCOPIC SURVEY, background: geometry, GALAXY REDSHIFT SURVEY, neutrino: mass, dark energy, 010303 astronomy & astrophysics, matter: density, expansion: adiabatic, Physics, Spectral index, cosmological constant, Hubble constant, Settore FIS/05, Cosmic background radiation, Cosmological parameters, ACCURATE HALO-MODEL, statistical analysis: Bayesian, POWER-SPECTRUM, matter: fluctuation, tension, perturbation: scalar, Physical Sciences, symbols, astro-ph.CO, Neutrino, Astrophysics - Cosmology and Nongalactic Astrophysics, Particle physics, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Dark matter, FOS: Physical sciences, cosmic background radiation: spectrum, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, NO, symbols.namesake, power spectrum: scalar, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, 0201 Astronomical and Space Sciences, Planck, cosmological parameters, Astrophysics::Galaxy Astrophysics, Science & Technology, 010308 nuclear & particles physics, baryon: density, Astronomy and Astrophysics, GROWTH-RATE, stability, 115 Astronomy, Space science, cosmic background radiation: temperature, MICROWAVE BACKGROUND ANISOTROPIES, 13. Climate action, Space and Planetary Science, Cosmic background radiation, Cosmological parameters, PROBE WMAP OBSERVATIONS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BARYON ACOUSTIC-OSCILLATIONS, Hubble's law, cosmic background radiation: anisotropy
Abstract: Planck Collaboration: et al., arXiv:1807.06209v3, We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction. Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters. Improved modelling of the small-scale polarization leads to more robust constraints on many parameters, with residual modelling uncertainties estimated to affect them only at the 0.5σ level. We find good consistency with the standard spatially-flat 6-parameter ΛCDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted “base ΛCDM” in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density Ωch2 = 0.120 ± 0.001, baryon density Ωbh2 = 0.0224 ± 0.0001, scalar spectral index ns = 0.965 ± 0.004, and optical depth τ = 0.054 ± 0.007 (in this abstract we quote 68% confidence regions on measured parameters and 95% on upper limits). The angular acoustic scale is measured to 0.03% precision, with 100θ* = 1.0411 ± 0.0003. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-ΛCDM cosmology, the inferred (model-dependent) late-Universe parameters are: Hubble constant H0 = (67.4 ± 0.5) km s−1 Mpc−1; matter density parameter Ωm = 0.315 ± 0.007; and matter fluctuation amplitude σ8 = 0.811 ± 0.006. We find no compelling evidence for extensions to the base-ΛCDM model. Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter extensions) we constrain the effective extra relativistic degrees of freedom to be Neff = 2.99 ± 0.17, in agreement with the Standard Model prediction Neff = 3.046, and find that the neutrino mass is tightly constrained to ∑mν < 0.12 eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base ΛCDM at over 2σ, which pulls some parameters that affect the lensing amplitude away from the ΛCDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. The joint constraint with BAO measurements on spatial curvature is consistent with a flat universe, ΩK = 0.001 ± 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w0 = −1.03 ± 0.03, consistent with a cosmological constant. We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r0.002 < 0.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-ΛCDM cosmology are in excellent agreement with observations. The Planck base-ΛCDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey’s combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 3.6σ, tension with local measurements of the Hubble constant (which prefer a higher value). Simple model extensions that can partially resolve these tensions are not favoured by the Planck data., The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, 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); ERC and PRACE (EU).
Published: 2020

28. Planck 2018 results: V. CMB power spectra and likelihoods

Author: Francesca Perrotta, A. A. Fraisse, Torsten A. Enßlin, A. J. Banday, M. Sandri, Yabebal Fantaye, L. Toffolatti, Serge Gratton, Jean-François Cardoso, Jose Alberto Rubino-Martin, Martin Kunz, Mathieu Remazeilles, Yin-Zhe Ma, G. de Zotti, E. Martínez-González, Anthony Lasenby, E. Keihänen, Jon E. Gudmundsson, N. Mandolesi, Andrew H. Jaffe, J.-L. Puget, Philip Lubin, J. Kim, M.-A. Miville-Deschênes, M. Lilley, Charles R. Lawrence, M. Le Jeune, François R. Bouchet, F. K. Hansen, Krzysztof M. Gorski, E. Di Valentino, L. Montier, Mario G. Lattanzi, A. Moneti, Erminia Calabrese, Andrea Zacchei, B. P. Crill, N. Bartolo, B. Van Tent, Locke D. Spencer, E. Franceschi, Ted Kisner, M. Maris, Martina Gerbino, D. Herranz, A. Marcos-Caballero, N. Mauri, Adam Moss, Hannu Kurki-Suonio, M. Tomasi, Sabino Matarrese, Davide Maino, Nicola Vittorio, V. Lindholm, Ricardo Genova-Santos, Reijo Keskitalo, C. Sirignano, Zhiqi Huang, P. Bielewicz, Jörg P. Rachen, Julien Carron, Y. Giraud-Héraud, X. Dupac, K. Ganga, D. Tavagnacco, Tuhin Ghosh, L. Pagano, S. Galeotta, Hans Ulrik Nørgaard-Nielsen, L. Salvati, Marco Bersanelli, B. Partridge, Jose M. Diego, M. Reinecke, A. Renzi, Ingunn Kathrine Wehus, Benjamin D. Wandelt, Julian Borrill, Will Handley, S. Basak, Andrei V. Frolov, Marian Douspis, Rashid Sunyaev, G. Sirri, F. Piacentini, S. Dusini, Andrea Zonca, H. C. Chiang, S. Galli, Guillaume Patanchon, M. Migliaccio, Jan Hamann, P. B. Lilje, M. Bucher, O. Doré, Paolo Natoli, Douglas Scott, R. Fernandez-Cobos, F. Cuttaia, Hiranya V. Peiris, M. Tenti, James J. Bock, Peter G. Martin, Valeria Pettorino, Gianluca Morgante, Tiziana Trombetti, Jacques Delabrouille, E. P. S. Shellard, R. B. Barreiro, Alessandro Melchiorri, Antony Lewis, R. C. Butler, K. Kiiveri, J. F. Macías-Pérez, C. Combet, Fabio Finelli, Diego Molinari, G. Maggio, A. Mangilli, Graca Rocha, Fabrizio Villa, J.-P. Bernard, M. Frailis, Carlo Baccigalupi, W. C. Jones, Nabila Aghanim, François Levrier, L. P. L. Colombo, Marius Millea, Eric Hivon, Mario Ballardini, D. Paoletti, Franz Elsner, George Efstathiou, C. Rosset, G. Roudier, Alessandro Gruppuso, Michele Liguori, A. Mennella, Yashar Akrami, Anthony Challinor, J.-M. Lamarre, A. Ducout, J. A. Tauber, M. Savelainen, F. Boulanger, P. Vielva, Guilaine Lagache, M. López-Caniego, P. de Bernardis, B. Casaponsa, B. Ruiz-Granados, A.-S. Suur-Uski, J. Valiviita, J. Aumont, J.-M. Delouis, M. Ashdown, H. K. Eriksen, G. Polenta, Peter Meinhold, J. González-Nuevo, K. Benabed, J. R. Bond, A. De Rosa, Jason D. McEwen, Carlo Burigana, Nicoletta Krachmalnicoff, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Université de Brest (UBO), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut Lagrange de Paris, Sorbonne Université, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Universités, Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Universidad de Cantabria, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Laboratoire d'Océanographie Physique et Spatiale (LOPS), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, Sorbonne Université (SU), University College of London [London] (UCL), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-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), Aghanim N., 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., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Butler R.C., Calabrese E., Cardoso J.-F., Carron J., Casaponsa B., Challinor A., Chiang H.C., Colombo L.P.L., Combet C., Crill B.P., Cuttaia F., De Bernardis P., De Rosa A., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Dusini S., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Fernandez-Cobos R., Finelli F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Giraud-Heraud Y., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Levrier F., Lewis A., Liguori M., Lilje P.B., Lilley M., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Meinhold P.R., Melchiorri A., Mennella A., Migliaccio M., Millea M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Natoli P., Norgaard-Nielsen H.U., Pagano L., Paoletti D., Partridge B., Patanchon G., Peiris H.V., Perrotta F., Pettorino V., Piacentini F., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Shellard E.P.S., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., 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., Vittorio N., Wandelt B.D., Wehus I.K., Zacchei A., Zonca A., Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Department of Physics, Helsinki Institute of Physics, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, and European Space Agency
Subjects: Cosmological parameter, POLARIZATION, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astronomy, Cosmic microwave background, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Residual, Cosmic background radiation, Cosmology: observation, 01 natural sciences, 7. Clean energy, Spectral line, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Methods: data analysis, 0103 physical sciences, 0201 Astronomical and Space Sciences, Cosmology: observations, Statistical physics, MICROWAVE, Planck, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, Reionization, Cosmic background radiation, Cosmological parameters, Cosmology: observations, Methods: data analysis, Physics, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, 115 Astronomy, Space science, Polarization (waves), 13. Climate action, Space and Planetary Science, PROBE WMAP OBSERVATIONS, symbols, astro-ph.CO, SKY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Smoothing, APPROXIMATION, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Planck Collaboration: et al., We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release. The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low (ℓ < 30) and high (ℓ ≥ 30) multipoles, implementing several methodological and data-analysis refinements compared to previous releases. With more realistic simulations, and better correction and modelling of systematic effects, we can now make full use of the CMB polarization observed in the High Frequency Instrument (HFI) channels. The low-multipole EE cross-spectra from the 100 GHz and 143 GHz data give a constraint on the ΛCDM reionization optical-depth parameter τ to better than 15% (in combination with the TT low-ℓ data and the high-ℓ temperature and polarization data), tightening constraints on all parameters with posterior distributions correlated with τ. We also update the weaker constraint on τ from the joint TEB likelihood using the Low Frequency Instrument (LFI) channels, which was used in 2015 as part of our baseline analysis. At higher multipoles, the CMB temperature spectrum and likelihood are very similar to previous releases. A better model of the temperature-to-polarization leakage and corrections for the effective calibrations of the polarization channels (i.e., the polarization efficiencies) allow us to make full use of polarization spectra, improving the ΛCDM constraints on the parameters θMC, ωc, ωb, and H0 by more than 30%, and ns by more than 20% compared to TT-only constraints. Extensive tests on the robustness of the modelling of the polarization data demonstrate good consistency, with some residual modelling uncertainties. At high multipoles, we are now limited mainly by the accuracy of the polarization efficiency modelling. Using our various tests, simulations, and comparison between different high-multipole likelihood implementations, we estimate the consistency of the results to be better than the 0.5 σ level on the ΛCDM parameters, as well as classical single-parameter extensions for the joint likelihood (to be compared to the 0.3 σ levels we achieved in 2015 for the temperature data alone on ΛCDM only). Minor curiosities already present in the previous releases remain, such as the differences between the best-fit ΛCDM parameters for the ℓ < 800 and ℓ > 800 ranges of the power spectrum, or the preference for more smoothing of the power-spectrum peaks than predicted in ΛCDM fits. These are shown to be driven by the temperature power spectrum and are not significantly modified by the inclusion of the polarization data. Overall, the legacy Planck CMB likelihoods provide a robust tool for constraining the cosmological model and represent a reference for future CMB observations., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, 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 ERC and PRACE (EU).
Published: 2020

29. Cosmology with the submillimetre galaxies magnification bias: Proof of concept

Author: M. M. Cueli, Andrea Lapi, T. Ronconi, J. González-Nuevo, Mattia Negrello, Laura Bonavera, Steve Maddox, M. Migliaccio, and Loretta Dunne
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Halo occupation distribution, Cosmology, gravitational lensing: weak, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, cosmological parameters, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, Physics, Settore FIS/05, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Galaxy, Gravitational lens, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Context. As recently demonstrated, high-z submillimetre galaxies (SMGs) are the perfect background sample for tracing the mass density profiles of galaxies and clusters (baryonic and dark matter) and their time-evolution through gravitational lensing. Their magnification bias, a weak gravitational lensing effect, is a powerful tool for constraining the free parameters of a halo occupation distribution (HOD) model and potentially also some of the main cosmological parameters. Aims. The aim of this work is to test the capability of the magnification bias produced on high-z SMGs as a cosmological probe. We exploit cross-correlation data to constrain not only astrophysical parameters ($M_{min}$, $M_1$, and $\alpha$), but also some of the cosmological ones ($\Omega_m$, $\sigma_8$, and $H_0$) for this proof of concept. Methods. The measured cross-correlation function between a foreground sample of GAMA galaxies with spectroscopic redshifts in the range 0.2 < z < 0.8 and a background sample of H-ATLAS galaxies with photometric redshifts >1.2 is modelled using the traditional halo model description that depends on HOD and cosmological parameters. These parameters are then estimated by performing a Markov chain Monte Carlo analysis using different sets of priors to test the robustness of the results and to study the performance of this novel observable with the current set of data Results. With our current results, $\Omega_m$ and $H_0$ cannot be well constrained. However, we can set a lower limit of >0.24 at 95\% confidence level (CL) on $\Omega_m$ and we see a slight trend towards $H_0>70$ values. For our constraints on $\sigma_8$ we obtain only a tentative peak around 0.75, but an interesting upper limit of $\sigma_8\lesssim 1$ at 95\% CL. We also study the possibility to derive better constraints by imposing more restrictive priors on the astrophysical parameters., Comment: accepted in Astronomy & Astrophysics
Published: 2020

30. Statistics of the fractional polarization of extragalactic dusty sources in Planck HFI maps

Author: Francisco Argüeso, L. Toffolatti, Laura Bonavera, B. De Marco, and J. González-Nuevo
Subjects: Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Fractional polarization, symbols.namesake, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, symbols, media_common.cataloged_instance, European union, Planck, 010303 astronomy & astrophysics, Humanities, media_common
Abstract: We estimate the average fractional polarisation at 143, 217 and 353 GHz of a sample of 4697 extragalactic dusty sources by applying stacking technique. The sample is selected from the second version of the Planck Catalogue of Compact Sources at 857 GHz, avoiding the region inside the Planck Galactic mask (fsky ~ 60 per cent). We recover values for the mean fractional polarisation at 217 and 353 GHz of (3.10 \pm 0.75) per cent and (3.65 \pm 0.66) per cent, respectively, whereas at 143 GHz we give a tentative value of (3.52 \pm 2.48) per cent. We discuss the possible origin of the measured polarisation, comparing our new estimates with those previously obtained from a sample of radio sources. We test different distribution functions and we conclude that the fractional polarisation of dusty sources is well described by a log-normal distribution, as determined in the radio band studies. For this distribution we estimate {\mu}_{217GHz} = 0.3 \pm 0.5 (that would correspond to a median fractional polarisation of {\Pi}_{med} = (1.3 \pm 0.7) per cent) and {\mu}_{353GHz} = 0.7 \pm 0.4 ({\Pi}_{med} = (2.0 \pm 0.8) per cent), {\sigma}_{217GHz} = 1.3 \pm 0.2 and {\sigma}_{353GHz} = 1.1 \pm 0.2. With these values we estimate the source number counts in polarisation and the contribution given by these sources to the CMB B-mode angular power spectrum at 217, 353, 600 and 800 GHz. We conclude that extragalactic dusty sources might be an important contaminant for the primordial B-mode at frequencies > 217 GHz., Comment: arXiv admin note: text overlap with arXiv:1703.09952
Published: 2017

31. Broadband spectral energy distributions of SDSS-selected quasars and of their host galaxies: intense activity at the onset of AGN feedback

Author: Carlo Baccigalupi, J. González-Nuevo, Giulio Fabbian, Andrea Lapi, Federico Bianchini, Roberto Gilli, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ITA, FRA, and ESP
Subjects: QSOS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, infrared: galaxies, Settore FIS/05 - Astronomia e Astrofisica, quasars: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, galaxies: active – infrared: galaxies – quasars: general, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Luminous infrared galaxy, Star formation, Astronomy and Astrophysics, Quasar, Astrophysics - Astrophysics of Galaxies, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the mean spectral energy distribution (SED) of a sample of optically selected quasars (QSOs) at redshifts of $1 \le z \le 5$. To derive it, we exploit photometric information from SDSS, UKIDSS, and WISE surveys in combination with a stacking analysis of \textit{Herschel}, \textit{AKARI}, and \textit{Planck} maps at the location of the QSOs. The near-UV and optical parts of the reconstructed mean rest-frame SED are similar to those found in other studies. However, the SED shows an excess at 1-2 $\mu$m (when compared to the aforementioned SEDs normalized in the near-UV) and a prominent bump around 4-6 $\mu$m, followed by a decrease out to $\sim 20 \,\mu$m and a subsequent far-IR bump. From the fitted SEDs we estimate the average active galactic nuclei (AGN) luminosity $L_{\rm AGN}$ and star formation rate (SFR) as function of cosmic time, finding typical $L_{\rm AGN} \sim 10^{46} - 10^{47}$ erg/s and SFR $\sim 50 - 1000\, M_{\odot}/$yr. We develop mid-IR based criteria to split the QSO sample, finding that these allow us to move along the average relationship in the SFR vs. $L_{\rm AGN}$ diagram toward increasing AGN luminosities. When interpreted in the context of the in-situ coevolution scenario presented by Lapi et al. 2014, our results suggest that the detection in the far-IR band is an effective criterion to select objects where the star formation is on the verge of being affected by energy/momentum feedback from the central AGN., Comment: 23 pages, 9 figures, text updated to match the accepted version, ApJ in press
Published: 2019

32. SHALOS: Statistical Herschel -ATLAS lensed objects selection

Author: J. González-Nuevo, Francisco Argüeso, D. Herranz, Luisa Toffolatti, Sergio Luis Suárez Gómez, Laura Bonavera, Carlos González-Gutiérrez, Fernando Sánchez-Lasheras, F. García Riesgo, F. J. de Cos Juez, Ministerio de Economía y Competitividad (España), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), and Universidad de Cantabria
Subjects: Gravitational lensing: strong, Library science, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, strong [Gravitational lensing], 01 natural sciences, galaxies [Submillimeter], Methods: data analysis, 0103 physical sciences, media_common.cataloged_instance, European union, data analysis [Methods], 010303 astronomy & astrophysics, Selection (genetic algorithm), Astrophysics::Galaxy Astrophysics, media_common, Physics, Horizon (archaeology), 010308 nuclear & particles physics, Atlas (topology), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Submillimeter: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract: Context. The statistical analysis of large sample of strong lensing events can be a powerful tool to extract astrophysical or cosmological valuable information. Their selection using submillimetre galaxies has been demonstrated to be very effective with more than ∼200 proposed candidates in the case of Herschel-ATLAS data and several tens in the case of the South Pole Telescope. However, the number of confirmed events is still relatively low, i.e. a few tens, mostly because of the lengthy observational validation process on individual events. Aims. In this work we propose a new methodology with a statistical selection approach to increase by a factor of ∼5 the number of such events within the Herschel-ATLAS data set. Although the methodology can be applied to address several selection problems, it has particular benefits in the case of the identification of strongly lensed galaxies: objectivity, minimal initial constrains in the main parameter space, and preservation of statistical properties. Methods. The proposed methodology is based on the Bhattacharyya distance as a measure of the similarity between probability distributions of properties of two different cross-matched galaxies. The particular implementation for the aim of this work is called SHALOS and it combines the information of four different properties of the pair of galaxies: angular separation, luminosity percentile, redshift, and the ratio of the optical to the submillimetre flux densities. Results. The SHALOS method provides a ranked list of strongly lensed galaxies. The number of candidates within ∼340 deg of the Herschel-ATLAS surveyed area for the final associated probability, P > 0.7, is 447 and they have an estimated mean amplification factor of 3.12 for a halo with a typical cluster mass. Additional statistical properties of the SHALOS candidates, as the correlation function or the source number counts, are in agreement with previous results indicating the statistical lensing nature of the selected sample., JGN, LB, FA, LT, and SLSG acknowledge financial support from the I+D 2015 project AYA2015-65887-P (MINECO, FEDER) and the PGC 2018 project PGC2018-101948-B-I00 (MINECO, FEDER). JGN acknowledges financial from the Spanish MINECO for a “Ramon y Cajal” fellowship (RYC2013-13256). DH, FA, and LT acknowledge financial support from the I+D 2015 project AYA2015-64508-P (MINECO, FEDER). DH also acknowledges partial financial support from the RADIOFOREGROUNDS project, funded by the European Comission’s H2020 Research Infrastructures under the Grant Agreement 687312. JDCJ acknowledge financial support from the I+D 2017 project AYA2017-89121-P and support from the European Union’s Horizon 2020 research and innovation programme under the H2020-INFRAIA-2018- 2020 grant agreement No 210489629
Published: 2019

33. QSOs sigposting cluster size halos as gravitational lenses: halo mass, projected mass density profile and concentration at z∼0.7

Author: Federico Bianchini, Mattia Negrello, Laura Bonavera, Jesús Daniel Santos, F. J. de Cos Juez, Sergio Luis Suárez Gómez, Andrea Lapi, E. Díez Alonso, and J. González-Nuevo
Subjects: Physics, QSOS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, gravitational lensing, FOS: Physical sciences, Magnification, Astronomy and Astrophysics, Astrophysics, weak gravitational lensing, 01 natural sciences, Measure (mathematics), Galaxy, Gravitation, weak gravitational lensing, galaxy surveys, gravitational lensing, Gravitational lens, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Cluster (physics), Halo, galaxy surveys, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Magnification bias is a gravitational lensing effect that is normally overlooked because it is considered sub-optimal in comparison with the lensing shear. Thanks to the demonstrated optimal characteristics of the sub-millimetre galaxies (SMGs) for lensing analysis, in this work we were able to measure the magnification bias produced by a sample of QSOs acting as lenses, $0.2 13.6_{-0.4}^{+0.9}$, also confirmed by the mass density profile analysis ($M_{200c}\sim 10^{14} M_\odot$). These mass values indicate that we are observing the lensing effect of a cluster size halo signposted by the QSOs, as in previous studies of the magnification bias. Moreover, we were able to estimate the lensing convergence, $\kappa(\theta)$, for our magnification bias measurements down to a few kpcs. The derived mass density profile is in good agreement with a Navarro-Frank-White (NFW) profile. We also attempt an estimation of the halo mass and the concentration parameters, obtaining $M_{NFW}=1.0^{+0.4}_{-0.2}\times10^{14} M_\odot$ and $C=3.5_{-0.3}^{+0.5}$. This concentration value is rather low and it would indicate that the cluster halos around these QSOs are unrelaxed. However, higher concentration values still provides a compatible fit to the data., Comment: 30 pages, 8 figures, JCAP accepted
Published: 2019

34. Confusion noise due to clustered extragalactic point sources. Application of logarithmic cumulants for parameter estimation

Author: L. Toffolatti, Francisco Argüeso, D. Herranz, J. González-Nuevo, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), and Agencia Estatal de Investigación (España)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Logarithm, FOS: Physical sciences, Discount points, 01 natural sciences, 0103 physical sciences, medicine, Econometrics, media_common.cataloged_instance, European union, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Cumulant, 0105 earth and related environmental sciences, media_common, Confusion, Mathematics, Estimation theory, Horizon, Astronomy and Astrophysics, Noise, Space and Planetary Science, medicine.symptom, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The calculation of the characteristic function of the signal fluctuations due to clustered astrophysical sources is performed in this paper. For the typical case of power-law differential number counts and two-point angular correlation function, we present an extension of Zolotarev's theorem that allows us to compute the cumulants of the logarithm of the absolute value of the intensity. As a test, simulations based on recent observations of radio galaxies are then carried out, showing that these cumulants can be very useful for determining the fundamental parameters defining the number counts and the correlation. If the angular correlation scale of the observed source population is known, the method presented here is able to obtain estimators of the amplitude and slope of the power-law number counts with mean absolute errors that are one order of magnitude better than previous techniques, that did not take into account the correlation. Even if the scale of correlation is not well known, the method is able to estimate it and still performs much better than if the effect of correlations is not considered., 16 pages, 2 figures. Accepted for publication in PASP
Published: 2019

35. SCUBA-2 observations of candidate starbursting protoclusters selected by Planck and Herschel-SPIRE

Author: T. Cheng, Jingzhe Ma, Lingyu Wang, Helmut Dannerbauer, M. N. Bremer, E. van Kampen, Hooshang Nayyeri, J. González-Nuevo, David L. Clements, Paola Andreani, Edo Ibar, Dominik Riechers, I. Valtchanov, J. Greenslade, Pasquale Temi, Douglas Scott, Mattia Vaccari, Lerothodi Leonard Leeuw, Michał J. Michałowski, Joseph Cairns, Asantha Cooray, L. Conversi, G. de Zotti, Stephen Anthony Eales, and Astronomy
Subjects: FOS: Physical sciences, galaxies: starburst, Astronomy & Astrophysics, 01 natural sciences, LYMAN BREAK GALAXIES, STAR-FORMATION, symbols.namesake, PROTO-CLUSTER, galaxies: high-redshift, ELLIPTIC GALAXIES, BOLOMETER CAMERA, 0103 physical sciences, galaxies [submillimetre], 0201 Astronomical and Space Sciences, 14. Life underwater, Planck, DUSTY GALAXIES, 010303 astronomy & astrophysics, BLACK-HOLES, Physics, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, starburst [galaxies], Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, HIGH-REDSHIFT, submillimetre: galaxies, high-redshift [galaxies], COSMOLOGY LEGACY SURVEY
Abstract: We present SCUBA-2 850-$\mu$m observations of 13 candidate starbursting protoclusters selected using Planck and Herschel data. The cumulative number counts of the 850-$\mu$m sources in 9/13 of these candidate protoclusters show significant overdensities compared to the field, with the probability $2$ protoclusters and the peak of the cosmic star-formation rate density (SFRD). We find that the 850-$\mu$m sources in our candidate protoclusters have infrared luminosities of $L_{\mathrm{IR}}\gtrsim$10$^{12}L_{\odot}$ and star-formation rates of SFR=(500-1,500)$M_{\odot}$yr$^{-1}$. By comparing with results in the literature considering only Herschel photometry, we conclude that our 13 candidate protoclusters can be categorised into four groups: six of them being high-redshift starbursting protoclusters, one being a lower-redshift cluster/protocluster, three being protoclusters that contain lensed DSFG(s) or are rich in 850-$\mu$m sources, and three regions without significant Herschel or SCUBA-2 source overdensities. The total SFRs of the candidate protoclusters are found to be comparable or higher than those of known protoclusters, suggesting our sample contains some of the most extreme protocluster population. We infer that cross-matching Planck and Herschel data is a robust method for selecting candidate protoclusters with overdensities of 850-$\mu$m sources., Comment: 30 pages, 8 figures, 5 tables, accepted for publication in MNRAS
Published: 2019

36. Point source detection with fully convolutional networks

Author: F. J. de Cos, Jesús Daniel Santos, Laura Bonavera, M. M. Cueli, Sergio Luis Suárez Gómez, Mercedes Leonor Sanchez, Ruben Muñiz, and J. González-Nuevo
Subjects: Physics, 010308 nuclear & particles physics, Point source, media_common.quotation_subject, Cosmic background radiation, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Space and Planetary Science, Sky, 0103 physical sciences, 010303 astronomy & astrophysics, Microwave, media_common
Abstract: Context. Point sources are one of the main contaminants to the recovery of the cosmic microwave background signal at small scales, and their careful detection will be important for the next generation of cosmic microwave background experiments like LiteBird. Aims. We want to develop a method based on fully convolutional networks to detect sources in realistic simulations, and to compare its performance against one of the most used point source detection method in this context, the Mexican hat wavelet 2 (MHW2). The frequencies for our analysis are the 143, 217, and 353 GHz Planck channels. Methods. We produce realistic simulations of point sources at each frequency taking into account potential contaminating signals as the cosmic microwave background, the cosmic infrared background, the Galactic thermal emission, the thermal Sunyaev-Zel’dovich effect, and the instrumental and point source shot noises. We first produce a set of training simulations at 217 GHz to train the neural network that we named PoSeIDoN. Then we apply both PoSeIDoN and the MHW2 to recover the point sources in the validating simulations at all the frequencies, comparing the results by estimating the reliability, completeness, and flux density estimation accuracy. Moreover, the receiver operating characteristic (ROC) curves are computed in order to asses the methods’performance. Results. In the extra-galactic region with a 30° galactic cut, the neural network successfully recovers point sources at 90% completeness corresponding to 253, 126, and 250 mJy for 143, 217, and 353 GHz respectively. In the same validation simulations the wavelet with a 3σ flux density detection limit recovers point sources up to 181, 102, and 153 mJy at 90% completeness. To reduce the number of spurious sources, we also apply a safer 4σ flux density detection limit, the same as in the Planck catalogues, increasing the 90% completeness levels: 235, 137, and 192 mJy. In all cases PoSeIDoN produces a much lower number of spurious sources with respect to MHW2. As expected, the results on spurious sources for both techniques worsen when reducing the galactic cut to 10°. Conclusions. Our results suggest that using neural networks is a very promising approach for detecting point sources using data from cosmic microwave background experiments, providing overall better results in dealing with spurious sources with respect to the more usual filtering approaches. Moreover, PoSeIDoN gives competitive results even at the 217 GHz nearby channels where the network was not trained.
Published: 2021

37. Cosmological constraints on the magnification bias on sub-millimetre galaxies after large-scale bias corrections

Author: L. Toffolatti, M. Migliaccio, Francisco Argüeso, J. González-Nuevo, M. M. Cueli, Laura Bonavera, and Andrea Lapi
Subjects: Physics, Supermassive black hole, 010308 nuclear & particles physics, Magnification, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, 01 natural sciences, Galaxy, Physical cosmology, Black hole, Stars, galaxies: high-redshift – submillimeter: galaxies – gravitational lensing: weak – cosmological parameters, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, 0103 physical sciences, Millimeter, 010303 astronomy & astrophysics
Abstract: Context. The study of the magnification bias produced on high-redshift sub-millimetre galaxies by foreground galaxies through the analysis of the cross-correlation function was recently demonstrated as an interesting independent alternative to the weak-lensing shear as a cosmological probe. Aims. In the case of the proposed observable, most of the cosmological constraints mainly depend on the largest angular separation measurements. Therefore, we aim to study and correct the main large-scale biases that affect foreground and background galaxy samples to produce a robust estimation of the cross-correlation function. Then we analyse the corrected signal to derive updated cosmological constraints. Methods. We measured the large-scale, bias-corrected cross-correlation functions using a background sample of H-ATLAS galaxies with photometric redshifts > 1.2 and two different foreground samples (GAMA galaxies with spectroscopic redshifts or SDSS galaxies with photometric ones, both in the range 0.2 < z < 0.8). These measurements are modelled using the traditional halo model description that depends on both halo occupation distribution and cosmological parameters. We then estimated these parameters by performing a Markov chain Monte Carlo under multiple scenarios to study the performance of this observable and how to improve its results. Results. After the large-scale bias corrections, we obtain only minor improvements with respect to the previous magnification bias results, mainly confirming their conclusions: a lower bound on Ωm > 0.22 at 95% CL and an upper bound σ8 zspec sample). Neither the much higher surface density of the foreground photometric sample nor the assumption of Gaussian priors for the remaining unconstrained parameters significantly improve the derived constraints. However, by combining both foreground samples into a simplified tomographic analysis, we were able to obtain interesting constraints on the Ωm − σ8 plane as follows: Ωm = 0.50−0.20+0.14 and σ8 = 0.75−0.10+0.07 at 68% CL.
Published: 2021

38. Planck 2018 results. VIII. Gravitational lensing

Author: Charles R. Lawrence, L. Pagano, Andrea Zacchei, J. B. Kim, K. Benabed, E. Martínez-González, Francesco Forastieri, M. Migliaccio, Martin White, M. Bucher, J. R. Bond, B. Ruiz-Granados, Andrea Zonca, N. Mauri, J. J. Bock, Douglas Scott, Davide Maino, H. C. Chiang, Yashar Akrami, Anthony Challinor, M. Tenti, Michele Maris, J. A. Tauber, M. Savelainen, O. Doré, K. Ganga, P. Bielewicz, Tiziana Trombetti, Jose M. Diego, Jean-François Cardoso, Francesca Perrotta, J. Aumont, Torsten A. Enßlin, M. Ashdown, H. K. Eriksen, X. Dupac, P. B. Lilje, Krzysztof M. Gorski, A. Marcos-Caballero, M. Reinecke, A. Mennella, Nabila Aghanim, R. A. Sunyaev, Julien Carron, Paolo Natoli, Franz Elsner, L. Montier, A. Mangilli, F. Cuttaia, Martin Kunz, Mathieu Remazeilles, R. B. Barreiro, F. Piacentini, G. Roudier, J.-L. Puget, K. Kiiveri, Guilaine Lagache, M.-A. Miville-Deschênes, L. Salvati, J. F. Macías-Pérez, Jon E. Gudmundsson, Yin-Zhe Ma, Jason D. McEwen, Zhiqi Huang, M. López-Caniego, Jose Alberto Rubino-Martin, L. P. L. Colombo, Martina Gerbino, G. Polenta, A. Moneti, F. K. Hansen, S. Galli, Soumen Basak, Mario Ballardini, Graca Rocha, J.-P. Bernard, Carlo Burigana, Nicoletta Krachmalnicoff, Chiara Sirignano, Sabino Matarrese, G. de Zotti, A. Renzi, C. Combet, Benjamin D. Wandelt, Julian Borrill, George Efstathiou, M. Frailis, Carlo Baccigalupi, Andrei V. Frolov, Jörg P. Rachen, Antony Lewis, Valeria Pettorino, François Levrier, E. Hivon, Will Handley, E. Di Valentino, Jacques Delabrouille, N. Mandolesi, Gianluca Morgante, Andrew H. Jaffe, Philip Lubin, Ingunn Kathrine Wehus, Diego Molinari, L. Toffolatti, A. J. Banday, Fabio Finelli, Massimiliano Lattanzi, Tuhin Ghosh, P. de Bernardis, R. Fernandez-Cobos, Aurelien A. Fraisse, B. P. Crill, B. Van Tent, P. Vielva, Erminia Calabrese, C. Rosset, Michele Liguori, Fabrizio Villa, Anthony Lasenby, Adam Moss, Ricardo Genova-Santos, E. Keihänen, E. Franceschi, Yabebal Fantaye, D. Tavagnacco, Nicola Bartolo, Marian Douspis, Nicola Vittorio, A. Karakci, W. C. Jones, A.-S. Suur-Uski, V. Lindholm, J. Valiviita, Peter G. Martin, S. Galeotta, Alessandro Gruppuso, J. González-Nuevo, J.-M. Lamarre, B. Partridge, A. Ducout, D. Paoletti, Hannu Kurki-Suonio, Steven Gratton, Lloyd Knox, L. Polastri, Alessandro Melchiorri, Reijo Keskitalo, M. Tomasi, Marco Bersanelli, Jan Hamann, Simon D. M. White, M. Sandri, Gianmarco Maggio, G. Patanchon, D. Herranz, M. Le Jeune, F. Boulanger, François R. Bouchet, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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)-Université Grenoble Alpes (UGA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universidad de Cantabria, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Università degli studi di Parma = University of Parma (UNIPR), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre National d'Études Spatiales [Toulouse] (CNES), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratory for Phytosanitary Diagnostics and Forecasts, All-Russian Institute for Plant Protection, Russian Academy of Sciences [Moscow] (RAS), Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), ICRA and Physics Department, Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University of Manchester [Manchester], Venetian Institute Molecular Medicine (VIMM), University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, European Project: 616170,EC:FP7:ERC,ERC-2013-CoG,COSMOPARS(2014), 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), Aghanim N., 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., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Colombo L.P.L., Combet C., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Fernandez-Cobos R., Finelli F., Forastieri F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Karakci A., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Knox L., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Levrier F., Lewis A., Liguori M., Lilje P.B., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Melchiorri A., Mennella A., Migliaccio M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Natoli P., Pagano L., Paoletti D., Partridge B., Patanchon G., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Sirignano C., Sunyaev R., 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., Vittorio N., Wandelt B.D., Wehus I.K., White M., White S.D.M., Zacchei A., Zonca A., Department of Physics, Helsinki Institute of Physics, Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Parma = Università degli studi di Parma [Parme, Italie], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Université Fédérale Toulouse Midi-Pyrénées, Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Universita degli Studi di Padova, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Astronomy, Cosmic microwave background, Cosmological parameters, Cosmic background radiation, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: observation, 01 natural sciences, 7. Clean energy, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, HALO-MODEL, Cosmic background radiation, Cosmological parameters, Cosmology: observations, Gravitational lensing: weak, Large-scale structure of Universe, Gravitational lensing: weak, Cosmic infrared background, 0103 physical sciences, Cosmology: observations, Planck, observations [Cosmology], 010303 astronomy & astrophysics, QB, Physics, Settore FIS/05, 010308 nuclear & particles physics, POWER SPECTRA, Spectral density, Astronomy and Astrophysics, 115 Astronomy, Space science, Redshift, GALAXIES, Gravitational lens, Space and Planetary Science, CROSS-CORRELATION, Dark energy, symbols, astro-ph.CO, DARK ENERGY, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Planck Collaboration: et al., arXiv:1807.06210v2, We present measurements of the cosmic microwave background (CMB) lensing potential using the final Planck 2018 temperature and polarization data. Using polarization maps filtered to account for the noise anisotropy, we increase the significance of the detection of lensing in the polarization maps from 5σ to 9σ. Combined with temperature, lensing is detected at 40σ. We present an extensive set of tests of the robustness of the lensing-potential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles 8 ≤ L ≤ 400 (extending the range to lower L compared to 2015), which we use to constrain cosmological parameters. We find good consistency between lensing constraints and the results from the Planck CMB power spectra within the ΛCDM model. Combined with baryon density and other weak priors, the lensing analysis alone constrains σ8Ωm0.25 = 0.589 ± 0.020 (1σ errors). Also combining with baryon acoustic oscillation data, we find tight individual parameter constraints, σ8 = 0.811 ± 0.019, H0 = 67.9−1.3+1.2 km s−1 Mpc−1, and Ωm = 0.303−0.018+0.016. Combining with Planck CMB power spectrum data, we measure σ8 to better than 1% precision, finding σ8 = 0.811 ± 0.006. CMB lensing reconstruction data are complementary to galaxy lensing data at lower redshift, having a different degeneracy direction in σ8 − Ωm space; we find consistency with the lensing results from the Dark Energy Survey, and give combined lensing-only parameter constraints that are tighter than joint results using galaxy clustering. Using the Planck cosmic infrared background (CIB) maps as an additional tracer of high-redshift matter, we make a combined Planck-only estimate of the lensing potential over 60% of the sky with considerably more small-scale signal. We additionally demonstrate delensing of the Planck power spectra using the joint and individual lensing potential estimates, detecting a maximum removal of 40% of the lensing-induced power in all spectra. The improvement in the sharpening of the acoustic peaks by including both CIB and the quadratic lensing reconstruction is detected at high significance., Support is acknowledged from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. [616170], and from the Science and Technology Facilities Council [grant numbers ST/L000652/1 and ST/N000927/1, respectively]. The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, 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); ERC and PRACE (EU).
Published: 2018

39. Exploring cosmic origins with CORE:mitigation of systematic effects

Author: M. Tristram, Daniela Paoletti, Eric Hivon, Jose M. Diego, M. López-Caniego, Hannu Kurki-Suonio, D. Tramonte, J. Borrill, M. Piat, Shaul Hanany, Guillaume Patanchon, M. Bonato, Matthieu Roman, J. González-Nuevo, F. Piacentini, G. Signorelli, Stephen M. Feeney, Silvia Galli, Miguel Quartin, M. Migliaccio, François R. Bouchet, A. Bonaldi, E. Di Valentino, R. Van de Weijgaert, Ricardo Genova-Santos, L. Salvati, Zhen-Yi Cai, Nicola Bartolo, Martino Calvo, Julien Lesgourgues, Reijo Keskitalo, Alessandro Coppolecchia, Jens Chluba, Carlo Burigana, G. Castellano, Bruno Maffei, D. McCarthy, R. Banerji, Daniel Baumann, Martina Gerbino, Thomas Kitching, Alessandro Monfardini, Francois Boulanger, M. Tomasi, Carlos Hernández-Monteagudo, L. Polastri, Alessandro Melchiorri, Ted Kisner, S. Basak, Giuseppe D'Alessandro, Peter A. R. Ade, Massimiliano Lattanzi, Sebastien Clesse, Marco Bersanelli, Mario Zannoni, R. Allison, Will Handley, J. Valiviita, P. Vielva, Diego Molinari, Mathieu Remazeilles, A. Gruppuso, Matthew Hills, K. Kiiveri, A. Lewis, Mattia Negrello, Michele Liguori, Carole Tucker, Gemma Luzzi, G. Polenta, Silvia Masi, Alessandro Paiella, Giampaolo Pisano, L. Pagano, P. de Bernardis, Anthony Challinor, Sebastian Grandis, Martin Bucher, Luca Lamagna, R. Fernandez-Cobos, Tiziana Trombetti, G. de Gasperis, C. S. Carvalho, A. Tartari, Jacques Delabrouille, Nazzareno Mandolesi, C. Baccigalupi, Vivian Poulin, Ana Achúcarro, Alessio Notari, Alessandro Buzzelli, I. Colantoni, Enrique Martinez-Gonzalez, Fabio Finelli, James G. Bartlett, Francesco Forastieri, Mario Ballardini, Anthony Lasenby, Vincent Vennin, Christopher G. R. Wallis, E. Keihänen, D. T. Hoang, J. J. A. Baselmans, Jean-Baptiste Melin, M. Ashdown, Sophie Henrot-Versille, M. Kunz, S. Hagstotz, Josquin Errard, Jose Alberto Rubino-Martin, C. J. A. P. Martins, G. de Zotti, Neil Trappe, Nicola Vittorio, V. Lindholm, J. Greenslade, Karl Young, O. Perdereau, B. Van Tent, A. J. Banday, Thejs Brinckmann, Graziano Rossi, A. Pollo, C. Hervias-Caimapo, Martin Crook, Paolo Natoli, 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), 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), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut Lagrange de Paris, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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 Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), CORE, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Sorbonne Universités, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Hélium : du fondamental aux applications (NEEL - HELFA), Helsinki Institute of Physics, Department of Physics, 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), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Natoli, P, Ashdown, M, Banerji, R, Borrill, J, Buzzelli, A, de Gasperis, G, Delabrouille, J, Hivon, E, Molinari, D, Patanchon, G, Polastri, L, Tomasi, M, Bouchet, F, Henrot-Versillé, S, Hoang, D, Keskitalo, R, Kiiveri, K, Kisner, T, Lindholm, V, Mccarthy, D, Piacentini, F, Perdereau, O, Polenta, G, Tristram, M, Achucarro, A, Ade, P, Allison, R, Baccigalupi, C, Ballardini, M, Banday, A, Bartlett, J, Bartolo, N, Basak, S, Baumann, D, Bersanelli, M, Bonaldi, A, Bonato, M, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Cai, Z, Calvo, M, Carvalho, C, Castellano, M, Challinor, A, Chluba, J, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, Zotti, G, Valentino, E, Diego, J, Errard, J, Feeney, S, Fernandez-Cobos, R, Finelli, F, Forastieri, F, Galli, S, Genova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Gruppuso, A, Hagstotz, S, Hanany, S, Handley, W, Hernandez-Monteagudo, C, Hervías-Caimapo, C, Hills, M, Keihänen, E, Kitching, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Lesgourgues, J, Lewis, A, Liguori, M, López-Caniego, M, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-González, E, Martins, C, Masi, S, Matarrese, S, Melchiorri, A, Melin, J, Migliaccio, M, Monfardini, A, Negrello, M, Notari, A, Pagano, L, Paiella, A, Paoletti, D, Piat, M, Pisano, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rossi, G, Rubino-Martin, J, Salvati, L, Signorelli, G, Tartari, A, Tramonte, D, Trappe, N, Trombetti, T, Tucker, C, Valiviita, J, de Weijgaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Wallis, C, Young, K, Zannoni, M, String Theory (ITFA, IoP, FNWI), AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -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 ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-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 ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, 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 Théorique d'Orsay [Orsay] ( LPT ), and Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Astrophysics, Residual, 01 natural sciences, NOISE, Photometric calibration, CMBR experiments, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, media_common, Physics, COSMIC cancer database, INSTRUMENT, FLIGHT, Astrophysics::Instrumentation and Methods for Astrophysics, symbols, astro-ph.CO, CMBR experiment, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, CMBR polarisation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, POLARIZATION MAPS, FOS: Physical sciences, ComputerApplications_COMPUTERSINOTHERSYSTEMS, NO, LIKELIHOOD, symbols.namesake, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, Robustness (computer science), 0103 physical sciences, SPECTRA, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Planck, Instrumentation and Methods for Astrophysics (astro-ph.IM), CMBR polarization, 010308 nuclear & particles physics, MAP-MAKING ALGORITHM, Astronomy and Astrophysics, PLANCK SURVEYOR, 115 Astronomy, Space science, CMBR experiments, CMBR polarisation, gravitational waves and CMBR polarization, Reliability engineering, Future study, CMB EXPERIMENTS, Sky, astro-ph.IM, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], gravitational waves and CMBR polarization, astronomy and astrophysics
Abstract: This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We also thank CSC — IT Center for Science (Finland) for computational resources. We acknowledge financial support by ASI Grant 2016-24-H.0 and Academy of Finland grant 295113. This work has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement number 687312. CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). JGN acknowledges financial support from the Spanish MINECO for a ‘Ramon y Cajal’ fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER). GR acknowledges support from the National Research Foundation of Korea (NRF) through Grant No. 2017R1E1A1A01077508 funded by the Korean Ministry of Education, Science and Technology (MoEST), and from the faculty research fund of Sejong University in 2018. We thank Jean Kaplan for useful comments on the manuscript., Natoli, P., Ashdown, M., Banerji, R., Borrill, J., Buzzelli, A., De Gasperis, G., Delabrouille, J., Hivon, E., Molinari, D., Patanchon, G., Polastri, L., Tomasi, M., Bouchet, F.R., Henrot-Versillé, S., Hoang, D.T., Keskitalo, R., Kiiveri, K., Kisner, T., Lindholm, V., McCarthy, D., Piacentini, F., Perdereau, O., Polenta, G., Tristram, M., Achucarro, A., Ade, P., Allison, R., Baccigalupi, C., Ballardini, M., Banday, A.J., Bartlett, J., Bartolo, N., Basak, S., Baumann, D., Bersanelli, M., Bonaldi, A., Bonato, M., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Cai, Z.-Y., Calvo, M., Carvalho, C.-S., Castellano, M.G., Challinor, A., Chluba, J., Clesse, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Bernardis, P., Zotti, G.D., Valentino, E.D., Diego, J.-M., Errard, J., Feeney, S., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Galli, S., Genova-Santos, R., Gerbino, M., González-Nuevo, J., Grandis, S., Greenslade, J., Gruppuso, A., Hagstotz, S., Hanany, S., Handley, W., Hernandez-Monteagudo, C., Hervías-Caimapo, C., Hills, M., Keihänen, E., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Lesgourgues, J., Lewis, A., Liguori, M., López-Caniego, M., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-González, E., Martins, C.J.A.P., Masi, S., Matarrese, S., Melchiorri, A., Melin, J.-B., Migliaccio, M., Monfardini, A., Negrello, M., Notari, A., Pagano, L., Paiella, A., Paoletti, D., Piat, M., Pisano, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Rubino-Martin, J.-A., Salvati, L., Signorelli, G., Tartari, A., Tramonte, D., Trappe, N., Trombetti, T., Tucker, C., Valiviita, J., De Weijgaert, R.V., Tent, B.V., Vennin, V., Vielva, P., Vittorio, N., Wallis, C., Young, K., Zannoni, M.
Published: 2018

40. Exploring cosmic origins with CORE: cosmological parameters

Author: Daniela Paoletti, Nicola Bartolo, Jens Chluba, J. Greenslade, P. Vielva, Mattia Negrello, Karl Young, Matteo Bonato, Andrea Tartari, Alessandro Paiella, Alessandro Coppolecchia, Andrea Caputo, Nicola Vittorio, V. Lindholm, Anthony Challinor, Agnieszka Pollo, Francois Boulanger, Luca Lamagna, Simone Ferraro, Martin Crook, D. McCarthy, M. López-Caniego, Ted Kisner, G. de Gasperis, L. Polastri, Alessandro Melchiorri, Josquin Errard, Rien van de Weygaert, D. Tramonte, Jose Alberto Rubino-Martin, C. J. A. P. Martins, Deanna C. Hooper, Matthieu Roman, Gianfranco De Zotti, Neil Trappe, M. Piat, Daniel Baumann, Gianluca Polenta, Jussi Valiviita, M. Tomasi, Paolo de Bernardis, Christophe Ringeval, Marco De Petris, Marco Bersanelli, Mario Zannoni, Giuseppe D'Alessandro, R. Fernandez-Cobos, Julien Lesgourgues, Paolo Natoli, Laura Salvati, Miguel Quartin, Thomas Kitching, R. Allison, Antony Lewis, K. Kiiveri, Carole Tucker, Diego Molinari, M. Kunz, Joseph J. Mohr, Ricardo Genova-Santos, C. Hervias-Caimapo, Jean-Baptiste Melin, Sebastian Grandis, Sylvain Martin, Michele Liguori, Shaul Hanany, Mario Ballardini, Vincent Vennin, Eleonora Di Valentino, Enrique Martinez-Gonzalez, Jose M. Diego, Giovanni Cabass, Hannu Kurki-Suonio, Jacques Delabrouille, J. González-Nuevo, Anthony Lasenby, F. Piacentini, Jochem J. A. Baselmans, Gemma Luzzi, S. Hagstotz, Tiziana Trombetti, Stephen M. Feeney, Alessio Notari, C. S. Carvalho, Fabio Finelli, Simone Paradiso, Silvia Masi, James G. Bartlett, Carlos Hernández-Monteagudo, Massimiliano Lattanzi, A. J. Banday, Thejs Brinckmann, Cora Dvorkin, Eric Hivon, Sebastien Clesse, Alessandro Buzzelli, Vivian Poulin, Ana Achúcarro, Martina Gerbino, M. Ashdown, A. Bonaldi, Luca Pagano, Julian Borrill, Will Handley, Martino Calvo, R. Banerji, Ivan Charles, Alessandro Monfardini, Frederico Arroja, S. Basak, Mathieu Remazeilles, Giampaolo Pisano, I. Colantoni, Silvia Galli, Gérard Vermeulen, Francesco Forastieri, Elena Giusarma, Dhiraj Kumar Hazra, François R. Bouchet, Zhen-Yi Cai, Carlo Burigana, G. Castellano, Peter A. R. Ade, Matthew Hills, Bruno Maffei, Martin Bucher, Bartjan van Tent, Guillaume Patanchon, Helsinki Institute of Physics, Department of Physics, String Theory (ITFA, IoP, FNWI), Astronomy, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, 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 ), AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Département de Recherche Fondamentale sur la Matière Condensée ( DRFMC ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-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 de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), CORE, Di Valentino, E, Brinckmann, T, Gerbino, M, Poulin, V, Bouchet, F, Lesgourgues, J, Melchiorri, A, Chluba, J, Clesse, S, Delabrouille, J, Dvorkin, C, Forastieri, F, Galli, S, Hooper, D, Lattanzi, M, Martins, C, Salvati, L, Cabass, G, Caputo, A, Giusarma, E, Hivon, E, Natoli, P, Pagano, L, Paradiso, S, Rubiño-Martin, J, Achúcarro, A, Ade, P, Allison, R, Arroja, F, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartolo, N, Bartlett, J, Basak, S, Baumann, D, de Bernardis, P, Bersanelli, M, Bonaldi, A, Bonato, M, Borrill, J, Boulanger, F, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Challinor, A, Charles, I, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, De Petris, M, De Zotti, G, Diego, J, Errard, J, Feeney, S, Fernandez-Cobos, R, Ferraro, S, Finelli, F, de Gasperis, G, Génova-Santos, R, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Handley, W, Hazra, D, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lewis, A, Liguori, M, Lindholm, V, Lopez-Caniego, M, Luzzi, G, Maffei, B, Martin, S, Martinez-Gonzalez, E, Masi, S, Matarrese, S, Mccarthy, D, Melin, J, Mohr, J, Molinari, D, Monfardini, A, Negrello, M, Notari, A, Paiella, A, Paoletti, D, Patanchon, G, Piacentini, F, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Quartin, M, Remazeilles, M, Roman, M, Ringeval, C, Tartari, A, Tomasi, M, Tramonte, D, Trappe, N, Trombetti, T, Tucker, C, Väliviita, J, van de Weygaert, R, Van Tent, B, Vennin, V, Vermeulen, G, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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), 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), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Département de Recherche Fondamentale sur la Matière Condensée (DRFMC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), Hélium : du fondamental aux applications (NEEL - HELFA), Sorbonne Université (SU), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)
Subjects: gravitation: model, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, cosmological parameters from CMBR, CMBR experiments, neutrino masses from cosmology, BACKGROUND ANISOTROPIES, cosmic background radiation: polarization, Astrophysics, baryon: oscillation: acoustic, NEUTRINO MASS, 01 natural sciences, COBE FIRAS INSTRUMENT, current: constraint, DESI, High Energy Physics - Phenomenology (hep-ph), CMBR experiments, CMB POLARIZATION, dark energy, 010303 astronomy & astrophysics, general relativity and quantum cosmology, QC, cosmological parameters from CMBR, neutrino masses from cosmology, media_common, helium: primordial, QB, Physics, birefringence, hep-th, formation, Astrophysics::Instrumentation and Methods for Astrophysics, hep-ph, TEMPERATURE-REDSHIFT RELATION, high energy physics - theory, inflation: model, high energy physics - phenomenology, curvature, symbols, astro-ph.CO, CMBR experiment, FUNDAMENTAL CONSTANTS, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, ANGULAR POWER SPECTRUM, Primordial fluctuations, media_common.quotation_subject, gr-qc, Dark matter, satellite, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, NO, BROKEN LEPTON NUMBER, symbols.namesake, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, FINE-STRUCTURE CONSTANT, 0103 physical sciences, ionization, LARGE-SCALE STRUCTURE, structure, Planck, Reionization, PROBING NEUTRINO MASSES, Inflation (cosmology), 010308 nuclear & particles physics, fluctuation: primordial, Astronomy and Astrophysics, dark matter: annihilation, sensitivity, 115 Astronomy, Space science, MICROWAVE-ANISOTROPY-PROBE, Universe, recombination, COLD DARK-MATTER, High Energy Physics - Theory (hep-th), 13. Climate action, Dark energy, DIGITAL SKY SURVEY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], MICROWAVE BACKGROUND POLARIZATION
Abstract: We forecast the main cosmological parameter constraints achievable with the CORE space mission which is dedicated to mapping the polarisation of the Cosmic Microwave Background (CMB). CORE was recently submitted in response to ESA's fifth call for medium-sized mission proposals (M5). Here we report the results from our pre-submission study of the impact of various instrumental options, in particular the telescope size and sensitivity level, and review the great, transformative potential of the mission as proposed. Specifically, we assess the impact on a broad range of fundamental parameters of our Universe as a function of the expected CMB characteristics, with other papers in the series focusing on controlling astrophysical and instrumental residual systematics. In this paper, we assume that only a few central CORE frequency channels are usable for our purpose, all others being devoted to the cleaning of astrophysical contaminants. On the theoretical side, we assume LCDM as our general framework and quantify the improvement provided by CORE over the current constraints from the Planck 2015 release. We also study the joint sensitivity of CORE and of future Baryon Acoustic Oscillation and Large Scale Structure experiments like DESI and Euclid. Specific constraints on the physics of inflation are presented in another paper of the series. In addition to the six parameters of the base LCDM, which describe the matter content of a spatially flat universe with adiabatic and scalar primordial fluctuations from inflation, we derive the precision achievable on parameters like those describing curvature, neutrino physics, extra light relics, primordial helium abundance, dark matter annihilation, recombination physics, variation of fundamental constants, dark energy, modified gravity, reionization and cosmic birefringence. (ABRIDGED), Comment: 90 pages, 25 Figures. Revised version with new authors list and references
Published: 2018

41. Exploring Cosmic Origins with CORE:survey requirements and mission design

Author: Karl Young, N. Mandolesi, A. Renzi, D. McCarthy, Andrea Lapi, F. Voisin, F. Oppizzi, Mark Hindmarsh, A. Mennella, Josquin Errard, S. Martin, Jose M. Diego, Enrico Pajer, Douglas Scott, A. Da Silva, Luigi Danese, R. B. Partridge, Subodh P. Patil, Créidhe O'Sullivan, A. M. C. Le Brun, Gianluca Polenta, Deanna C. Hooper, Alessandro Buzzelli, O. Perdereau, Jose Alberto Rubino-Martin, Nicolas Ponthieu, C. J. A. P. Martins, Eric Hivon, M. De Petris, Reijo Keskitalo, Bruno Maffei, Rashid Sunyaev, Michael L. Brown, Elena Giusarma, Marek Biesiada, Joanes Lizarraga, Nicola Bartolo, F. Piacentini, Stephen M. Feeney, G. de Zotti, Neil Trappe, Bin Hu, Cristian Franceschet, Matthieu Tristram, Pasquale Mazzotta, R. Allison, Hannu Kurki-Suonio, Jens Chluba, J. Greenslade, R. Fernandez-Cobos, Alicia Gomez, Stephen Serjeant, A. Catalano, Paolo Natoli, C. S. Carvalho, K. Kiiveri, David L. Clements, Diego Molinari, S. Paradiso, Martina Gerbino, Vincent Vennin, Carole Tucker, Kaustuv Basu, Alexei A. Starobinsky, Sabino Matarrese, Andrea Ravenni, L. Salvati, Eduardo Artal, G. Vermeulen, M. Piat, M. Tucci, F. Noviello, Ingunn Kathrine Wehus, Elia S. Battistelli, Matteo Bonato, R. Banerji, Ted Kisner, Jean-Baptiste Melin, Christophe Ringeval, Christopher G. R. Wallis, Benjamin D. Wandelt, Julian Borrill, Massimiliano Lattanzi, Aurelien Bideaud, Sebastien Clesse, Tiziana Trombetti, Martin Crook, Will Handley, P. de Bernardis, Ruth Durrer, Francois Boulanger, Matthieu Roman, C. Y. Tan, Sébastien Triqueneaux, Silvia Galli, G. Signorelli, A. Tartari, Gianmassimo Tasinato, S. Basak, Nicola Vittorio, D. Tramonte, V. Lindholm, Julien Lesgourgues, J. F. Macías-Pérez, E. Di Valentino, Francesco Forastieri, G. de Gasperis, Thomas Kitching, Vincent Desjacques, François R. Bouchet, Zhen-Yi Cai, Sergio Colafrancesco, Richard A. Battye, Alessandro Monfardini, F.-X. Désert, Alessandro Paiella, Jesús Torrado, Michele Liguori, Anthony Challinor, Carlo Burigana, G. Castellano, Agnieszka Pollo, Daniel Baumann, L. Pagano, Boudewijn F. Roukema, Mathieu Remazeilles, Sophie Henrot-Versille, M. Tomasi, Enrique Martinez-Gonzalez, Giampaolo Pisano, M. Kunz, Joseph J. Mohr, Ricardo Genova-Santos, P. Vielva, Mattia Negrello, Marcella Massardi, Carlo Baccigalupi, Guilaine Lagache, Marco Bersanelli, Anthony Lasenby, S. Hagstotz, Domingos Barbosa, E. Keihänen, D. Prêle, Vivian Poulin, Mario Zannoni, Alain Benoit, Ana Achúcarro, D. T. Hoang, I. Colantoni, U. Fuskeland, D. Contreras, Giovanni Cabass, Jochem J. A. Baselmans, Johannes Goupy, Jochen Weller, I. Charles, Sebastian Grandis, Giuseppe D'Alessandro, M. Ashdown, A. Bonaldi, Frederico Arroja, Guido D'Amico, Gemma Luzzi, M. A. de Avillez, Martino Calvo, Silvia Masi, Daniela Paoletti, Alessandro Coppolecchia, Andrea Caputo, L. Polastri, Alessandro Melchiorri, Jon Urrestilla, Licia Verde, Mario Ballardini, Luisa Toffolatti, Jacques Delabrouille, Alessio Notari, Maciej Bilicki, Fabio Finelli, L. A. Montier, James G. Bartlett, Guillaume Patanchon, Carlos Hernández-Monteagudo, Miguel Quartin, Cora Dvorkin, Simon Doyle, H. K. Eriksen, C. Hervias-Caimapo, R. van de Weygaert, Clive Dickinson, Peter A. R. Ade, Matthew Hills, Luca Lamagna, B. Van Tent, A. J. Banday, Thejs Brinckmann, F. J. Casas, Martin Bucher, Shaul Hanany, Jussi Valiviita, J. González-Nuevo, Diederik Roest, String Theory (ITFA, IoP, FNWI), Universitat de Barcelona, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université Grenoble Alpes (UGA), Institut Nanosciences et Cryogénie (INAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Universités, 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), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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 Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), CORE, Department of Physics, Helsinki Institute of Physics, 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 polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-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)-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), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Grenoble Alpes (UGA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Sorbonne Université (SU), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Delabrouille, J, de Bernardis, P, Bouchet, F, Achúcarro, A, Ade, P, Allison, R, Arroja, F, Artal, E, Ashdown, M, Baccigalupi, C, Ballardini, M, Banday, A, Banerji, R, Barbosa, D, Bartlett, J, Bartolo, N, Basak, S, Baselmans, J, Basu, K, Battistelli, E, Battye, R, Baumann, D, Benoít, A, Bersanelli, M, Bideaud, A, Biesiada, M, Bilicki, M, Bonaldi, A, Bonato, M, Borrill, J, Boulanger, F, Brinckmann, T, Brown, M, Bucher, M, Burigana, C, Buzzelli, A, Cabass, G, Cai, Z, Calvo, M, Caputo, A, Carvalho, C, Casas, F, Castellano, G, Catalano, A, Challinor, A, Charles, I, Chluba, J, Clements, D, Clesse, S, Colafrancesco, S, Colantoni, I, Contreras, D, Coppolecchia, A, Crook, M, D'Alessandro, G, D'Amico, G, da Silva, A, de Avillez, M, de Gasperis, G, De Petris, M, de Zotti, G, Danese, L, Désert, F, Desjacques, V, Valentino, E, Dickinson, C, Diego, J, Doyle, S, Durrer, R, Dvorkin, C, Eriksen, H, Errard, J, Feeney, S, Fernández-Cobos, R, Finelli, F, Forastieri, F, Franceschet, C, Fuskeland, U, Galli, S, Génova-Santos, R, Gerbino, M, Giusarma, E, Gomez, A, González-Nuevo, J, Grandis, S, Greenslade, J, Goupy, J, Hagstotz, S, Hanany, S, Handley, W, Henrot-Versillé, S, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hindmarsh, M, Hivon, E, Hoang, D, Hooper, D, Hu, B, Keihänen, E, Keskitalo, R, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamagna, L, Lapi, A, Lasenby, A, Lattanzi, M, Brun, A, Lesgourgues, J, Liguori, M, Lindholm, V, Lizarraga, J, Luzzi, G, Macìas-Pérez, J, Maffei, B, Mandolesi, N, Martin, S, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Mazzotta, P, Mccarthy, D, Melchiorri, A, Melin, J, Mennella, A, Mohr, J, Molinari, D, Monfardini, A, Montier, L, Natoli, P, Negrello, M, Notari, A, Noviello, F, Oppizzi, F, O'Sullivan, C, Pagano, L, Paiella, A, Pajer, E, Paoletti, D, Paradiso, S, Partridge, R, Patanchon, G, Patil, S, Perdereau, O, Piacentini, F, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Ponthieu, N, Poulin, V, Prêle, D, Quartin, M, Ravenni, A, Remazeilles, M, Renzi, A, Ringeval, C, Roest, D, Roman, M, Roukema, B, Rubiño-Martin, J, Salvati, L, Scott, D, Serjeant, S, Signorelli, G, Starobinsky, A, Sunyaev, R, Tan, C, Tartari, A, Tasinato, G, Toffolatti, L, Tomasi, M, Torrado, J, Tramonte, D, Trappe, N, Triqueneaux, S, Tristram, M, Trombetti, T, Tucci, M, Tucker, C, Urrestilla, J, Väliviita, J, de Weygaert, R, Tent, B, Vennin, V, Verde, L, Vermeulen, G, Vielva, P, Vittorio, N, Voisin, F, Wallis, C, Wandelt, B, Wehus, I, Weller, J, Young, K, and Zannoni, M
Subjects: CMBR experiments, CMBR polarisation, gravitational lensing, physics of the early universe, POLARIZATION, Computer science, Cosmic microwave background, cosmic background radiation: polarization, CMB, 7. Clean energy, 01 natural sciences, Cosmology, Physics, Particles & Fields, cosmic flows, CMBR polarization, astronomy and astrophysics, Cosmic physics, CMBR experiments – CMBR theory – reionization – high redshift galaxies, 010303 astronomy & astrophysics, QC, QB, COSMIC cancer database, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Nuclear & Particles Physics, cryogenics, Physical Sciences, Physics::Space Physics, Systems engineering, astro-ph.CO, proposed experiment, Astrophysics::Earth and Planetary Astrophysics, CMBR experiment, Astrophysics - Instrumentation and Methods for Astrophysics, performance, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), CMBR experiments, CMBR polarisation, gravitational lensing, physics of the early universe, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, NO, HALF-WAVE PLATE, 0202 Atomic, Molecular, Nuclear, Particle And Plasma Physics, Mission design, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: design, activity report, Science & Technology, Cosmologia, 010308 nuclear & particles physics, astro-ph.IM, 115 Astronomy, Space science, sensitivity, Complementarity (physics), 0201 Astronomical And Space Sciences, angular resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Física còsmica
Abstract: The CORE collaboration thanks CNES, Thales Alenia Space, and Air Liquide Advanced Technologies for advice and technical support during the preparation of the CORE proposal. We also thank the ESA CDF team for the CMB Polarisation CDF study performed in March 2016, the results of which were extensively used to define the mission concept presented in this paper. J.G.N. acknowledges financial support from the Spanish MINECO for a Ramon y Cajal fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER). CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE. F.J.C., R.F.-C., E.M.-G. and P.V. acknowledge support from the Spanish Ministerio de Econom´ıa y Competitividad project ESP2015-70646-C2-1-R (cofinanced with EU FEDER funds), ConsoliderIngenio 2010 project CSD2010-00064 and from the CSIC “Proyecto Intramural Especial” project 201550E091. FA is supported by the National Taiwan University (NTU) under Project No. 103R4000 and by the NTU Leung Center for Cosmology and Particle Astrophysics (LeCosPA) under Project No. FI121. BFR acknowledges support from the National Science Centre, Poland, under grant 2014/13/B/ST9/00845., Macìas-Pérez, J.F., Delabrouille, J., De Bernardis, P., Bouchet, F.R., Achúcarro, A., Ade, P.A.R., Allison, R., Arroja, F., Artal, E., Ashdown, M., Baccigalupi, C., Ballardini, M., Banday, A.J., Banerji, R., Barbosa, D., Bartlett, J., Bartolo, N., Basak, S., Baselmans, J.J.A., Basu, K., Battistelli, E.S., Battye, R., Baumann, D., Benoít, A., Bersanelli, M., Bideaud, A., Biesiada, M., Bilicki, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Brinckmann, T., Brown, M.L., Bucher, M., Burigana, C., Buzzelli, A., Cabass, G., Cai, Z.-Y., Calvo, M., Caputo, A., Carvalho, C.-S., Casas, F.J., Castellano, G., Catalano, A., Challinor, A., Charles, I., Chluba, J., Clements, D.L., Clesse, S., Colafrancesco, S., Colantoni, I., Contreras, D., Coppolecchia, A., Crook, M., D'Alessandro, G., D'Amico, G., Silva, A.D., De Avillez, M., De Gasperis, G., Petris, M.D., De Zotti, G., Danese, L., Désert, F.-X., Desjacques, V., Valentino, E.D., Dickinson, C., Diego, J.M., Doyle, S., Durrer, R., Dvorkin, C., Eriksen, H.K., Errard, J., Feeney, S., Fernández-Cobos, R., Finelli, F., Forastieri, F., Franceschet, C., Fuskeland, U., Galli, S., Génova-Santos, R.T., Gerbino, M., Giusarma, E., Gomez, A., González-Nuevo, J., Grandis, S., Greenslade, J., Goupy, J., Hagstotz, S., Hanany, S., Handley, W., Henrot-Versillé, S., Hernández-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Hindmarsh, M., Hivon, E., Hoang, D.T., Hooper, D.C., Hu, B., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lapi, A., Lasenby, A., Lattanzi, M., Brun, A.M.C.L., Lesgourgues, J., Liguori, M., Lindholm, V., Lizarraga, J., Luzzi, G., Macìas-Pérez, J.F., Maffei, B., Mandolesi, N., Martin, S., Martinez-Gonzalez, E., Martins, C.J.A.P., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., McCarthy, D., Melchiorri, A., Melin, J.-B., Mennella, A., Mohr, J., Molinari, D., Monfardini, A., Montier, L., Natoli, P., Negrello, M., Notari, A., Noviello, F., Oppizzi, F., O'Sullivan, C., Pagano, L., Paiella, A., Pajer, E., Paoletti, D., Paradiso, S., Partridge, R.B., Patanchon, G., Patil, S.P., Perdereau, O., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Ponthieu, N., Poulin, V., Prêle, D., Quartin, M., Ravenni, A., Remazeilles, M., Renzi, A., Ringeval, C., Roest, D., Roman, M., Roukema, B.F., Rubiño-Martin, J.-A., Salvati, L., Scott, D., Serjeant, S., Signorelli, G., Starobinsky, A.A., Sunyaev, R., Tan, C.Y., Tartari, A., Tasinato, G., Toffolatti, L., Tomasi, M., Torrado, J., Tramonte, D., Trappe, N., Triqueneaux, S., Tristram, M., Trombetti, T., Tucci, M., Tucker, C., Urrestilla, J., Väliviita, J., De Weygaert, R.V., Tent, B.V., Vennin, V., Verde, L., Vermeulen, G., Vielva, P., Vittorio, N., Voisin, F., Wallis, C., Wandelt, B., Wehus, I.K., Weller, J., Young, K., Zannoni, M.
Published: 2018

42. Exploring cosmic origins with CORE: Inflation

Author: F. Finelli, M. Bucher, A. Achúcarro, M. Ballardini, N. Bartolo, D. Baumann, S. Clesse, J. Errard, W. Handley, M. Hindmarsh, K. Kiiveri, M. Kunz, A. Lasenby, M. Liguori, D. Paoletti, C. Ringeval, J. Väliviita, B. van Tent, V. Vennin, P. Ade, R. Allison, F. Arroja, M. Ashdown, A.J. Banday, R. Banerji, J.G. Bartlett, S. Basak, P. de Bernardis, M. Bersanelli, A. Bonaldi, J. Borril, F.R. Bouchet, F. Boulanger, T. Brinckmann, C. Burigana, A. Buzzelli, Z.-Y. Cai, M. Calvo, C.S. Carvalho, G. Castellano, A. Challinor, J. Chluba, I. Colantoni, A. Coppolecchia, M. Crook, G. D'Alessandro, G. D'Amico, J. Delabrouille, V. Desjacques, G. De Zotti, J.M. Diego, E. Di Valentino, S. Feeney, J.R. Fergusson, R. Fernandez-Cobos, S. Ferraro, F. Forastieri, S. Galli, J. García-Bellido, G. de Gasperis, R.T. Génova-Santos, M. Gerbino, J. González-Nuevo, S. Grandis, J. Greenslade, S. Hagstotz, S. Hanany, D.K. Hazra, C. Hernández-Monteagudo, C. Hervias-Caimapo, M. Hills, E. Hivon, B. Hu, T. Kisner, T. Kitching, E.D. Kovetz, H. Kurki-Suonio, L. Lamagna, M. Lattanzi, J. Lesgourgues, A. Lewis, V. Lindholm, J. Lizarraga, M. López-Caniego, G. Luzzi, B. Maffei, N. Mandolesi, E. Martínez-González, C.J.A.P. Martins, S. Masi, D. McCarthy, S. Matarrese, A. Melchiorri, J.-B. Melin, D. Molinari, A. Monfardini, P. Natoli, M. Negrello, A. Notari, F. Oppizzi, A. Paiella, E. Pajer, G. Patanchon, S.P. Patil, M. Piat, G. Pisano, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, A. Ravenni, M. Remazeilles, A. Renzi, D. Roest, M. Roman, J.A. Rubiño-Martin, L. Salvati, A.A. Starobinsky, A. Tartari, G. Tasinato, M. Tomasi, J. Torrado, N. Trappe, T. Trombetti, M. Tucci, C. Tucker, J. Urrestilla, R. van de Weygaert, P. Vielva, N. Vittorio, K. Young, M. Zannoni, ITA, 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut Lagrange de Paris, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Pierre et Marie Curie - Paris 6 (UPMC), 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), CORE, Department of Physics, Helsinki Institute of Physics, 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), Sorbonne Universités, Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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)-Université Grenoble Alpes (UGA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Finelli, F, Bucher, M, Achúcarro, A, Ballardini, M, Bartolo, N, Baumann, D, Clesse, S, Errard, J, Handley, W, Hindmarsh, M, Kiiveri, K, Kunz, M, Lasenby, A, Liguori, M, Paoletti, D, Ringeval, C, Väliviita, J, Tent, B, Vennin, V, Ade, P, Allison, R, Arroja, F, Ashdown, M, Banday, A, Banerji, R, Bartlett, J, Basak, S, de Bernardis, P, Bersanelli, M, Bonaldi, A, Borril, J, Bouchet, F, Boulanger, F, Brinckmann, T, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Challinor, A, Chluba, J, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, D'Amico, G, Delabrouille, J, Desjacques, V, Zotti, G, Diego, J, Valentino, E, Feeney, S, Fergusson, J, Fernandez-Cobos, R, Ferraro, S, Forastieri, F, Galli, S, García-Bellido, J, de Gasperis, G, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Hazra, D, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hivon, E, Hu, B, Kisner, T, Kitching, T, Kovetz, E, Kurki-Suonio, H, Lamagna, L, Lattanzi, M, Lesgourgues, J, Lewis, A, Lindholm, V, Lizarraga, J, López-Caniego, M, Luzzi, G, Maffei, B, Mandolesi, N, Martínez-González, E, Martins, C, Masi, S, Mccarthy, D, Matarrese, S, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Oppizzi, F, Paiella, A, Pajer, E, Patanchon, G, Patil, S, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Ravenni, A, Remazeilles, M, Renzi, A, Roest, D, Roman, M, Rubiño-Martin, J, Salvati, L, Starobinsky, A, Tartari, A, Tasinato, G, Tomasi, M, Torrado, J, Trappe, N, Trombetti, T, Tucci, M, Tucker, C, Urrestilla, J, de Weygaert, R, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Finelli F., Bucher M., Achucarro A., Ballardini M., Bartolo N., Baumann D., Clesse S., Errard J., Handley W., Hindmarsh M., Kiiveri K., Kunz M., Lasenby A., Liguori M., Paoletti D., Ringeval C., Valiviita J., Tent B.V., Vennin V., Ade P., Allison R., Arroja F., Ashdown M., Banday A.J., Banerji R., Bartlett J.G., Basak S., De Bernardis P., Bersanelli M., Bonaldi A., Borril J., Bouchet F.R., Boulanger F., Brinckmann T., Burigana C., Buzzelli A., Cai Z.-Y., Calvo M., Carvalho C.S., Castellano G., Challinor A., Chluba J., Colantoni I., Coppolecchia A., Crook M., D'Alessandro G., D'Amico G., Delabrouille J., Desjacques V., Zotti G.D., Diego J.M., Valentino E.D., Feeney S., Fergusson J.R., Fernandez-Cobos R., Ferraro S., Forastieri F., Galli S., Garcia-Bellido J., De Gasperis G., Genova-Santos R.T., Gerbino M., Gonzalez-Nuevo J., Grandis S., Greenslade J., Hagstotz S., Hanany S., Hazra D.K., Hernandez-Monteagudo C., Hervias-Caimapo C., Hills M., Hivon E., Hu B., Kisner T., Kitching T., Kovetz E.D., Kurki-Suonio H., Lamagna L., Lattanzi M., Lesgourgues J., Lewis A., Lindholm V., Lizarraga J., Lopez-Caniego M., Luzzi G., Maffei B., Mandolesi N., Martinez-Gonzalez E., Martins C.J.A.P., Masi S., McCarthy D., Matarrese S., Melchiorri A., Melin J.-B., Molinari D., Monfardini A., Natoli P., Negrello M., Notari A., Oppizzi F., Paiella A., Pajer E., Patanchon G., Patil S.P., Piat M., Pisano G., Polastri L., Polenta G., Pollo A., Poulin V., Quartin M., Ravenni A., Remazeilles M., Renzi A., Roest D., Roman M., Rubino-Martin J.A., Salvati L., Starobinsky A.A., Tartari A., Tasinato G., Tomasi M., Torrado J., Trappe N., Trombetti T., Tucci M., Tucker C., Urrestilla J., De Weygaert R.V., Vielva P., Vittorio N., Young K., Zannoni M., String Theory (ITFA, IoP, FNWI), High-Energy Frontier, Astronomy, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), and Hélium : du fondamental aux applications (NEEL - HELFA)
Subjects: cosmological model, reheating, Cosmic microwave background, cosmic background radiation: polarization, SPECTRAL DISTORTIONS, astro-ph.CO, Astrophysics, cosmic background radiation, 7. Clean energy, 01 natural sciences, GRAVITATIONAL-WAVES, law.invention, law, 010303 astronomy & astrophysics, CMBR theory, ination, Astronomy and Astrophysics, CMBR theory, inflation, QC, QB, Physics, COSMIC cancer database, ST/J005673/1, ST/H008586/1, inflation: model, MICROWAVE BACKGROUND ANISOTROPY, Core inflation, Astrophysics - Cosmology and Nongalactic Astrophysics, Big Bang, scale: grand unified theory, Astrophysics and Astronomy, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), STANDARD MODEL, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, isocurvature: perturbation, frequency: high, PRIMORDIAL NON-GAUSSIANITY, NO, Telescope, power spectrum: primordial, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, LARGE-SCALE STRUCTURE, 0103 physical sciences, inflation, cosmic string, STFC, MODEL SELECTION, Inflation (cosmology), non-Gaussianity: primordial, ST/K00333X/1, ISOCURVATURE PERTURBATIONS, 010308 nuclear & particles physics, string tension, big bang, inflation: slow-roll approximation, RCUK, Spectral density, 115 Astronomy, Space science, cosmic background radiation: temperature, Cosmic string, detector: sensitivity, angular resolution, 13. Climate action, PRE-BIG-BANG, BAYESIAN-INFERENCE, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract: We forecast the scientific capabilities to improve our understanding of cosmic inflation of CORE, a proposed CMB space satellite submitted in response to the ESA fifth call for a medium-size mission opportunity. The CORE satellite will map the CMB anisotropies in temperature and polarization in 19 frequency channels spanning the range 60-600 GHz. CORE will have an aggregate noise sensitivity of $1.7 ��$K$\cdot \,$arcmin and an angular resolution of 5' at 200 GHz. We explore the impact of telescope size and noise sensitivity on the inflation science return by making forecasts for several instrumental configurations. This study assumes that the lower and higher frequency channels suffice to remove foreground contaminations and complements other related studies of component separation and systematic effects, which will be reported in other papers of the series "Exploring Cosmic Origins with CORE." We forecast the capability to determine key inflationary parameters, to lower the detection limit for the tensor-to-scalar ratio down to the $10^{-3}$ level, to chart the landscape of single field slow-roll inflationary models, to constrain the epoch of reheating, thus connecting inflation to the standard radiation-matter dominated Big Bang era, to reconstruct the primordial power spectrum, to constrain the contribution from isocurvature perturbations to the $10^{-3}$ level, to improve constraints on the cosmic string tension to a level below the presumptive GUT scale, and to improve the current measurements of primordial non-Gaussianities down to the $f_{NL}^{\rm local} < 1$ level. For all the models explored, CORE alone will improve significantly on the present constraints on the physics of inflation. Its capabilities will be further enhanced by combining with complementary future cosmological observations., Latex 107 pages, revised with updated author list and minor modifications
Published: 2018

43. Two planetary systems with transiting Earth-sized and super-Earth planets orbiting late-type dwarf stars

Author: Sergio Luis Suárez Gómez, A. Suárez Mascareño, Javier Gracia, D S Aguado, B. Toledo Padron, A. Cabrera-Lavers, Rafael Rebolo, F. J. de Cos Juez, E. Díez Alonso, C. González Gutiérrez, J. González-Nuevo, and J. I. González Hernández
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Super-Earth, 010308 nuclear & particles physics, Late type, Resonance, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Stars, Amplitude, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Earth (classical element), Astrophysics - Earth and Planetary Astrophysics
Abstract: We present two new planetary systems found around cool dwarf stars with data from the K2 mission. The first system was found in K2-239 (EPIC 248545986), char- acterized in this work as M3.0V and observed in the 14th campaign of K2. It consists of three Earth-size transiting planets with radii of 1.1, 1.0 and 1.1 R Earth, showing a compact configuration with orbital periods of 5.24, 7.78 and 10.1 days, close to 2:3:4 resonance. The second was found in K2-240 (EPIC 249801827), characterized in this work as M0.5V and observed in the 15th campaign. It consists of two transiting super-Earths with radii 2.0 and 1.8 R Earth and orbital periods of 6.03 and 20.5 days. The equilibrium temperatures of the atmospheres of these planets are estimated to be in the range of 380-600 K and the amplitudes of signals in transmission spectroscopy are estimated at ~10 ppm., Comment: Accepted for publication in MNRAS letters
Published: 2018

44. Forecasting the Contribution of Polarized Extragalactic Radio Sources in CMB Observations

Author: Francesca Perrotta, Giuseppe Puglisi, Vincenzo Galluzzi, J. González-Nuevo, Laura Bonavera, Marcella Massardi, Luigi Danese, Carlo Baccigalupi, Annalisa Celotti, and Andrea Lapi
Subjects: Physics, radio continuum: galaxies, polarization, 010308 nuclear & particles physics, Settore FIS/05, Cosmic microwave background, Cosmic background radiation, cosmic background radiation, cosmology: observations, quasars: general, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, 010303 astronomy & astrophysics
Abstract: We combine the latest data sets obtained with different surveys to study the frequency dependence of polarized emission coming from extragalactic radio sources (ERS). We consider data over a very wide frequency range starting from 1.4 GHz up to 217 GHz. This range is particularly interesting since it overlaps the frequencies of the current and forthcoming cosmic microwave background (CMB) experiments. Current data suggest that at high radio frequencies (ν ≥ 20 GHz) the fractional polarization of ERS does not depend on the total flux density. Conversely, recent data sets indicate a moderate increase of polarization fraction as a function of frequency, physically motivated by the fact that Faraday depolarization is expected to be less relevant at high radio frequencies. We compute ERS number counts using updated models based on recent data, and we forecast the contribution of unresolved ERS in CMB polarization spectra. Given the expected sensitivities and the observational patch sizes of forthcoming CMB experiments, about ∼200 (up to ∼2000) polarized ERS are expected to be detected. Finally, we assess that polarized ERS can contaminate the cosmological B-mode polarization if the tensor-to-scalar ratio is
Published: 2018
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45. Exploring Cosmic Origins with CORE: Cluster Science

Author: Alessandro Monfardini, Karl Young, Mario Ballardini, E. Di Valentino, Massimiliano Lattanzi, Sebastien Clesse, Mathieu Remazeilles, Giampaolo Pisano, Michele Liguori, Alessandro Buzzelli, Tiziana Trombetti, Joseph J. Mohr, Ricardo Genova-Santos, François R. Bouchet, Jose M. Diego, Zhen-Yi Cai, Carlo Burigana, J. Borrill, Jean-Baptiste Melin, Stephen M. Feeney, Josquin Errard, C. S. Carvalho, Ted Kisner, M. Kunz, Nicola Bartolo, Kaustuv Basu, Jose Alberto Rubino-Martin, Jens Chluba, S. Triqueneaux, C. J. A. P. Martins, G. de Gasperis, G. de Zotti, P. Vielva, Bruno Maffei, A. M. C. Le Brun, Neil Trappe, D. McCarthy, Enrique Martinez-Gonzalez, J. Greenslade, G. Polenta, Anthony Lasenby, Nicola Vittorio, V. Lindholm, Daniel Baumann, Carlos Hernández-Monteagudo, Vincent Vennin, M. López-Caniego, Diego Molinari, R. Allison, Alessandro Coppolecchia, Luca Lamagna, D. Tramonte, Simone Ferraro, A. Lewis, K. Kiiveri, L. Polastri, Alessandro Melchiorri, Carole Tucker, S. Hagstotz, R. Fernandez-Cobos, Silvia Galli, P. de Bernardis, Alessandro Paiella, A. Tartari, Daniela Paoletti, Francois Boulanger, Anthony Challinor, Jacques Delabrouille, Giuseppe D'Alessandro, Alessio Notari, M. Tomasi, Fabio Finelli, Marco Castellano, Martina Gerbino, Marco Bersanelli, James G. Bartlett, J. J. A. Baselmans, Francesco Forastieri, Richard A. Battye, Mario Zannoni, Paolo Natoli, M. Piat, M. Ashdown, Will Handley, A. Bonaldi, J. Valiviita, Martin Crook, Martino Calvo, Vivian Poulin, Ana Achúcarro, Peter A. R. Ade, Mattia Negrello, S. Colafrancesco, R. Banerji, Miguel Quartin, S. Basak, R. van de Weygaert, Sebastian Grandis, Matthew Hills, Martin Bucher, Guillaume Patanchon, M. Bonato, Hannu Kurki-Suonio, B. Van Tent, A. J. Banday, Thejs Brinckmann, Shaul Hanany, J. González-Nuevo, Eric Hivon, M. De Petris, A. Pollo, C. Hervias-Caimapo, Matthieu Roman, Julien Lesgourgues, Thomas Kitching, L. Salvati, J. F. Macías-Pérez, I. Colantoni, Jochen Weller, Gemma Luzzi, Silvia Masi, Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut Lagrange de Paris, Sorbonne Université (SU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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 Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), CORE, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Sorbonne Universités, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Universitat de Barcelona, Melin, J, Bonaldi, A, Remazeilles, M, Hagstotz, S, Diego, J, Hernández-Monteagudo, C, Génova-Santos, R, Luzzi, G, Martins, C, Grandis, S, Mohr, J, Bartlett, J, Delabrouille, J, Ferraro, S, Tramonte, D, Rubiño-Martín, J, Macìas-Pérez, J, Achúcarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartolo, N, Basak, S, Basu, K, Battye, R, Baumann, D, Bersanelli, M, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, M, Challinor, A, Chluba, J, Clesse, S, Colafrancesco, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Petris, M, Zotti, G, Valentino, E, Errard, J, Feeney, S, Fernández-Cobos, R, Finelli, F, Forastieri, F, Galli, S, Gerbino, M, González-Nuevo, J, Greenslade, J, Hanany, S, Handley, W, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Brun, A, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Lopez-Caniego, M, Maffei, B, Martinez-Gonzalez, E, Masi, S, Mazzotta, P, Mccarthy, D, Melchiorri, A, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Paiella, A, Paoletti, D, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Roman, M, Salvati, L, Tartari, A, Tomasi, M, Trappe, N, Triqueneaux, S, Trombetti, T, Tucker, C, Väliviita, J, de Weygaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Weller, J, Young, K, Zannoni, M, 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), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Département de Physique des Particules (ex SPP) (DPhP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Hélium : du fondamental aux applications (NEEL - HELFA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astronomy, String Theory (ITFA, IoP, FNWI), Helsinki Institute of Physics, and Department of Physics
Subjects: cluster count, Cosmic microwave background, MICROWAVE BACKGROUND COMPTONIZATION, Astrophysics, 01 natural sciences, HOT GAS, law.invention, law, cluster counts, CMBR experiments, galaxy clusters, Sunyaev-Zeldovich effect, CMBR experiments, Sunyaev-Zeldovich effect, cluster counts, galaxy clusters, WEAK-LENSING MASSES, MASSIVE GALAXY CLUSTERS, 010303 astronomy & astrophysics, TEMPERATURE, QC, QB, Physics, Clusters of galaxies, Settore FIS/05, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmology, symbols, astro-ph.CO, Halo, CMBR experiment, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxy cluster, Cúmuls de galàxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMOLOGICAL PARAMETERS, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, Primary mirror, Telescope, SUNYAEV-ZELDOVICH MAPS, symbols.namesake, FIS/05 - ASTRONOMIA E ASTROFISICA, 0103 physical sciences, Cluster (physics), Planck, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Cosmologia, RELATIVISTIC CORRECTIONS, 010308 nuclear & particles physics, Astronomy and Astrophysics, 115 Astronomy, Space science, Redshift, EVOLUTION, RADIATION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We thank the anonymous referee for useful comments, which helped to clarify the paper. Some of the results in this paper have been derived using the HEALPix package. Parts of the cosmological analysis was made using Cosmo MC, CLASS and MontePython. C.H.-M. acknowledges financial support of the Spanish Ministry of Economy and Competitiveness via I+D project AYA-2015-66211-C2-2-P. CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE. J.G.N. acknowledges financial support from the Spanish MINECO for a ‘Ramon y Cajal’ fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER)., Melin, J.-B., Bonaldi, A., Remazeilles, M., Hagstotz, S., Diego, J.M., Hernández-Monteagudo, C., Génova-Santos, R.T., Luzzi, G., Martins, C.J.A.P., Grandis, S., Mohr, J.J., Bartlett, J.G., Delabrouille, J., Ferraro, S., Tramonte, D., Rubiño-Martín, J.A., Macìas-Pérez, J.F., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A.J., Banerji, R., Bartolo, N., Basak, S., Basu, K., Battye, R.A., Baumann, D., Bersanelli, M., Bonato, M., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Cai, Z.-Y., Calvo, M., Carvalho, C.S., Castellano, M.G., Challinor, A., Chluba, J., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Bernardis, P., De Gasperis, G., Petris, M.D., Zotti, G.D., Valentino, E.D., Errard, J., Feeney, S.M., Fernández-Cobos, R., Finelli, F., Forastieri, F., Galli, S., Gerbino, M., González-Nuevo, J., Greenslade, J., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Brun, A.M.C.L., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Lopez-Caniego, M., Maffei, B., Martinez-Gonzalez, E., Masi, S., Mazzotta, P., McCarthy, D., Melchiorri, A., Molinari, D., Monfardini, A., Natoli, P., Negrello, M., Notari, A., Paiella, A., Paoletti, D., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Roman, M., Salvati, L., Tartari, A., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucker, C., Väliviita, J., De Weygaert, R.V., Tent, B.V., Vennin, V., Vielva, P., Vittorio, N., Weller, J., Young, K., Zannoni, M.
Published: 2018

46. Herschel-ATLAS : The spatial clustering of low and high redshift submillimetre galaxies

Author: J. Greenslade, Elisabetta Valiante, C. Tai-An, Stephen Anthony Eales, Matthew Smith, E. van Kampen, Lingyu Wang, G. de Zotti, Michał J. Michałowski, Loretta Dunne, J. González-Nuevo, Mattia Negrello, P. Andreani, Steve Maddox, Aristeidis Amvrosiadis, and Astronomy
Subjects: Terahertz radiation, media_common.quotation_subject, DATA RELEASE, Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, EXPLORER, NUMBER COUNTS, 010303 astronomy & astrophysics, POPULATION, media_common, BRIGHT, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, COUNTERPARTS, Astrophysics - Astrophysics of Galaxies, Universe, Galaxy, Redshift, MODEL, Wavelength, BIAS, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, Halo, large-scale structure of Universe, galaxies: evolution, SKY SURVEY, submillimetre: galaxies, COSMOLOGY LEGACY SURVEY
Abstract: We present measurements of the angular correlation function of sub-millimeter (sub-mm) galaxies (SMGs) identified in four out of the five fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) - GAMA-9h, GAMA-12h, GAMA-15h and NGP - with flux densities $S_{250��m}$>30 mJy at 250 ��m. We show that galaxies selected at this wavelength trace the underlying matter distribution differently at low and high redshifts. We study the evolution of the clustering finding that at low redshifts sub-mm galaxies exhibit clustering strengths of $r_0$ $\sim$ 2 - 3 $h^{-1}$ Mpc, below z < 0.3. At high redshifts, on the other hand, we find that sub-mm galaxies are more strongly clustered with correlation lengths $r_0$ = 8.1 $\pm$ 0.5, 8.8 $\pm$ 0.8 and 13.9 $\pm$ 3.9 $h^{-1}$Mpc at z = 1 - 2, 2 - 3 and 3 - 5, respectively. We show that sub-mm galaxies across the redshift range 1 < z < 5, typically reside in dark-matter halos of mass of the order of ~ $10^{12.5}$ - $10^{13.0}$ $h^{-1} \, M_{\odot}$ and are consistent with being the progenitors of local massive elliptical galaxies that we see in the local Universe., 17 pages, 11 figures, 3 tables. Accepted for publication in MNRAS
Published: 2018
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47. Exploring cosmic origins with CORE: Gravitational lensing of the CMB

Author: A. Challinor, R. Allison, J. Carron, J. Errard, S. Feeney, T. Kitching, J. Lesgourgues, A. Lewis, Í. Zubeldía, A. Achucarro, P. Ade, M. Ashdown, M. Ballardini, A.J. Banday, R. Banerji, J. Bartlett, N. Bartolo, S. Basak, D. Baumann, M. Bersanelli, A. Bonaldi, M. Bonato, J. Borrill, F. Bouchet, F. Boulanger, T. Brinckmann, M. Bucher, C. Burigana, A. Buzzelli, Z.-Y. Cai, M. Calvo, C.-S. Carvalho, G. Castellano, J. Chluba, S. Clesse, I. Colantoni, A. Coppolecchia, M. Crook, G. d'Alessandro, P. de Bernardis, G. de Gasperis, G. De Zotti, J. Delabrouille, E. Di Valentino, J.-M. Diego, R. Fernandez-Cobos, S. Ferraro, F. Finelli, F. Forastieri, S. Galli, R. Genova-Santos, M. Gerbino, J. González-Nuevo, S. Grandis, J. Greenslade, S. Hagstotz, S. Hanany, W. Handley, C. Hernandez-Monteagudo, C. Hervías-Caimapo, M. Hills, E. Hivon, K. Kiiveri, T. Kisner, M. Kunz, H. Kurki-Suonio, L. Lamagna, A. Lasenby, M. Lattanzi, M. Liguori, V. Lindholm, M. López-Caniego, G. Luzzi, B. Maffei, E. Martinez-González, C.J.A.P. Martins, S. Masi, S. Matarrese, D. McCarthy, A. Melchiorri, J.-B. Melin, D. Molinari, A. Monfardini, P. Natoli, M. Negrello, A. Notari, A. Paiella, D. Paoletti, G. Patanchon, M. Piat, G. Pisano, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, M. Remazeilles, M. Roman, J.-A. Rubino-Martin, L. Salvati, A. Tartari, M. Tomasi, D. Tramonte, N. Trappe, T. Trombetti, C. Tucker, J. Valiviita, R. Van de Weijgaert, B. van Tent, V. Vennin, P. Vielva, N. Vittorio, K. Young, M. Zannoni, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Universités, 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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 Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), CORE, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Challinor, A, Allison, R, Carron, J, Errard, J, Feeney, S, Kitching, T, Lesgourgues, J, Lewis, A, Zubeldía, Í, Achucarro, A, Ade, P, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Baumann, D, Bersanelli, M, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Chluba, J, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Zotti, G, Delabrouille, J, Valentino, E, Diego, J, Fernandez-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Genova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Handley, W, Hernandez-Monteagudo, C, Hervías-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Liguori, M, Lindholm, V, López-Caniego, M, Luzzi, G, Maffei, B, Martinez-González, E, Martins, C, Masi, S, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Paiella, A, Paoletti, D, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rubino-Martin, J, Salvati, L, Tartari, A, Tomasi, M, Tramonte, D, Trappe, N, Trombetti, T, Tucker, C, Valiviita, J, de Weijgaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Department of Physics, String Theory (ITFA, IoP, FNWI), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), and Hélium : du fondamental aux applications (NEEL - HELFA)
Subjects: deflection, Cosmic microwave background, cosmic background radiation: polarization, astro-ph.CO, Astrophysics, ST/N000927/1, ST/L000652/1, 7. Clean energy, 01 natural sciences, CMBR polarisation, gravitational lensing, inflation, neutrino masses from cosmology, ART. NO. 023003, estimator, neutrino: mass, 010303 astronomy & astrophysics, Physics, FLUCTUATIONS, GRAVITY-WAVES, Amplitude, non-Gaussianity, galaxy: cluster, Halo, gravitational radiation: power spectrum, Neutrino, CMBR polarization, gravitational lensing, ination, neutrino masses from cosmology, Astronomy and Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, CMBR polarisation, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), B-mode: lens, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, NO, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ddc:530, RECONSTRUCTION, inflation, Galaxy cluster, STFC, halo: mass, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, RCUK, 115 Astronomy, Space science, redshift, calibration, Redshift, Gravitational lens, CROSS-CORRELATION, RADIATION, neutrino: oscillation, GALAXY CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], MICROWAVE BACKGROUND POLARIZATION, MATTER
Abstract: Lensing of the CMB is now a well-developed probe of large-scale clustering over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission can produce a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that it will enable. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous BAO measurements, three times smaller than the minimum total mass allowed by neutrino oscillations. In the search for B-mode polarization from primordial gravitational waves with CORE, lens-induced B-modes will dominate over instrument noise, limiting constraints on the gravitational wave power spectrum amplitude. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60%. This improves to 70% by combining lensing and CIB measurements from CORE, reducing the error on the gravitational wave amplitude by 2.5 compared to no delensing (in the null hypothesis). Lensing measurements from CORE will allow calibration of the halo masses of the 40000 galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. CORE can accurately remove Galactic emission from CMB maps with its 19 frequency channels. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE. [abridged], 44 pages, 12 figures
Published: 2018

48. H-ATLAS/GAMA: magnification bias tomography. Astrophysical constraints above ~1 arcmin

Author: Rob Ivison, C. Furlanetto, Asantha Cooray, Laura Bonavera, Steve Maddox, Andrea Lapi, Nathan Bourne, J. González-Nuevo, Loretta Dunne, Mattia Negrello, Elisabetta Valiante, Luigi Danese, Simon Dye, Stephen Anthony Eales, Jon Loveday, G. de Zotti, and Matthew Smith
Subjects: gravitational lensing, FOS: Physical sciences, Minimum mass, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, weak gravitational lensing, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Atlas (anatomy), Galaxy group, 0103 physical sciences, medicine, Satellite galaxy, Range (statistics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, medicine.anatomical_structure, galaxy clustering, Astrophysics of Galaxies (astro-ph.GA), Halo
Abstract: In this work we measure and study the cross-correlation signal between a foreground sample of GAMA galaxies with spectroscopic redshifts in the range $0.2, Comment: 31 pages, 9 figures, accepted version to be published in JCAP
Published: 2017

49. Galaxy Evolution in the Radio Band: The Role of Starforming Galaxies and Active Galactic Nuclei

Author: L. Danese, F. Perrotta, Annalisa Celotti, A. Bressan, I. Obi, Isabella Prandoni, J. González-Nuevo, Claudia Mancuso, and Andrea Lapi
Subjects: Active galactic nucleus, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio spectrum, Cosmology, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Galaxy formation and evolution, media_common.cataloged_instance, Astrophysics::Solar and Stellar Astrophysics, European union, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Horizon, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Universe, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution | galaxies: statistics | quasars: general | radiation mechanisms: general | radio continuum: galaxies
Abstract: We investigate the astrophysics of radio-emitting star-forming galaxies and ac- tive galactic nuclei (AGNs), and elucidate their statistical properties in the radio band including luminosity functions, redshift distributions, and number counts at sub-mJy flux levels, that will be crucially probed by next-generation radio continuum surveys. Specifically, we exploit the model-independent approach by Mancuso et al. (2016a,b) to compute the star formation rate functions, the AGN duty cycles and the conditional probability of a star-forming galaxy to host an AGN with given bolometric luminosity. Coupling these ingredients with the radio emission properties associated to star formation and nuclear activity, we compute relevant statistics at different radio frequencies, and disentangle the relative con- tribution of star-forming galaxies and AGNs in different radio luminosity, radio flux, and redshift ranges. Finally, we highlight that radio-emitting star-forming galaxies and AGNs are expected to host supermassive black holes accreting with different Eddington ratio distributions, and to occupy different loci in the galaxy main sequence diagrams. These specific predictions are consistent with current datasets, but need to be tested with larger statistics via future radio data with multi-band coverage on wide areas, as it will become routinely achievable with the advent of the SKA and its precursors., Comment: 50 pages, 16 figures, Accepted by ApJ
Published: 2017
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50. Statistics of the fractional polarization of compact radio sources in Planck maps

Author: Laura Bonavera, L. Toffolatti, Francisco Argüeso, and J. González-Nuevo
Subjects: Physics, 010308 nuclear & particles physics, media_common.quotation_subject, FOS: Physical sciences, Sigma, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Fractional polarization, symbols.namesake, Distribution (mathematics), Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, symbols, Range (statistics), Planck, Constant (mathematics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: In this work we apply the stacking technique to estimate the average fractional polarisation from 30 to 353 GHz of a primary sample of 1560 compact sources - essentially all radio sources - detected in the 30 GHz Planck all-sky map and listed in the second version of the Planck Catalogue of Compact Sources (PCCS2). We divide our primary sample in two subsamples according to whether the sources lay (679 sources) or not (881 sources) inside the sky region defined by the Planck Galactic mask (fsky ~ 60 per cent) and the area around the Magellanic Clouds. We find that the average fractional polarisation of compact sources is approximately constant (with frequency) in both samples (with a weighted mean over all the channels of 3.08 per cent outside and 3.54 per cent inside the Planck mask). In the sky region outside the adopted mask, we also estimate the {\mu} and {\sigma} parameters for the log-normal distribution of the fractional polarisation, finding a weighted mean value over all the Planck frequency range of 1.0 for {\sigma} and 0.7 for {\mu} (that would imply a weighted mean value for the median fractional polarisation of 1.9 per cent)., Comment: 12 pages, 7 figures, 2 tables, MNRAS in press
Published: 2017

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