Author: "J.-P. Bernard" - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"J.-P. Bernard"' showing total 451 results

Start Over Author "J.-P. Bernard"

451 results on '"J.-P. Bernard"'

1. 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

2. First‐trimester diagnosis of congenital cytomegalovirus infection after maternal primary infection in early pregnancy: feasibility study of viral genome amplification by <scp>PCR</scp> on chorionic villi obtained by <scp>CVS</scp>

Author: J.-F. Magny, Jacques Fourgeaud, Yves Ville, V. Faure-Bardon, J.-P. Bernard, T. Guilleminot, Laurent Salomon, and Marianne Leruez-Ville
Subjects: Adult, medicine.medical_specialty, Amniotic fluid, Cytomegalovirus, Chorionic villus sampling, Gestational Age, Prenatal diagnosis, Genome, Viral, Polymerase Chain Reaction, Sensitivity and Specificity, Serology, 03 medical and health sciences, 0302 clinical medicine, Obstetrics and gynaecology, Pregnancy, Reference Values, Prenatal Diagnosis, medicine, Humans, Radiology, Nuclear Medicine and imaging, Prospective Studies, 030212 general & internal medicine, Pregnancy Complications, Infectious, 030219 obstetrics & reproductive medicine, Radiological and Ultrasound Technology, medicine.diagnostic_test, business.industry, Obstetrics, Obstetrics and Gynecology, Gestational age, General Medicine, Amniotic Fluid, Infectious Disease Transmission, Vertical, Pregnancy Trimester, First, medicine.anatomical_structure, Chorionic Villi Sampling, Reproductive Medicine, Cytomegalovirus Infections, Amniocentesis, Feasibility Studies, Chorionic villi, Female, Chorionic Villi, business
Abstract: Objective To evaluate the feasibility of amplification of the viral genome by polymerase chain reaction (PCR) analysis of trophoblast samples obtained by chorionic villus sampling (CVS) in cases of maternal primary infection (MPI) with cytomegalovirus (CMV) in early pregnancy. Methods This was a prospective study carried out at the Department of Obstetrics and Fetal Medicine, Hopital Necker-E.M., between October 2019 and October 2020. Following CMV serology screening in early pregnancy, CVS was offered to women at 11-14 weeks' gestation after CMV-MPI ≤ 10 weeks. Array-comparative genomic hybridization and amplification of the viral genome by PCR were performed on the trophoblasts obtained by CVS. All cases also underwent amniocentesis from 17 weeks onwards and PCR was performed on the amniotic fluid. Secondary prevention with valacyclovir was initiated as soon as MPI was diagnosed, to decrease the risk of vertical transmission. We evaluated the diagnostic performance of CMV-PCR of trophoblast obtained by CVS, using as the reference standard PCR of amniotic fluid obtained by amniocentesis. Results CVS was performed in 37 pregnancies, at a median (range) gestational age of 12.7 (11.3-14.4) weeks. CMV-PCR in chorionic villi was positive in three and negative in 34 cases. CMV-PCR following amniocentesis, performed at a median (range) gestational age of 17.6 (16.7-29.9) weeks, was positive for the three cases which were positive following CVS and, of the 34 patients with a negative finding following CVS, amniocentesis was negative in 31 and positive in three. The sensitivity of CMV-PCR analysis of trophoblast obtained by CVS for the diagnosis of CMV, using as the reference standard PCR analysis of amniotic fluid obtained by amniocentesis, was 50% (95% CI, 19-81%), specificity was 100% (95% CI, 89-100%), positive predictive value was 100% (95% CI, 44-100%) and negative predictive value was 91% (95% CI, 77-97%). Conclusions Diagnosis of placental infection following MPI in early pregnancy can be achieved by PCR amplification of the CMV genome in chorionic villi. We propose that negative CMV-PCR in the trophoblast after 12 weeks could be used to exclude CMV-related embryopathy leading to sequelae. However, this needs to be confirmed through long-term follow-up evaluation. These findings could help to establish CVS as the diagnostic test of choice following maternal serology screening in early pregnancy. © 2021 International Society of Ultrasound in Obstetrics and Gynecology.
Published: 2021

3. 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

4. The QUBIC instrument for CMB polarization measurements

Author: A. Bottani, E. Jules, A. Zullo, Federico Nati, V. Gilles, A. Baù, L. Mousset, Giampaolo Pisano, C. Perbost, C. Oriol, Damien Rambaud, G. Amico, D. Buzi, Emory F. Bunn, M. Tomasi, L. H. Arnaldi, A. Etchegoyen, S. Azzoni, F. Wicek, Marco Bersanelli, Mark McCulloch, Alejandro Almela, Mario Zannoni, M. Perciballi, Peter A. R. Ade, A. Pelosi, Maria Salatino, D. Auguste, S. Scully, M. Gómez Berisso, F. Piacentini, Andrea Tartari, M. Platino, Martin Giard, P. Chanial, Jonathan Aumont, C. Scóccola, M.-A. Bigot-Sazy, Alessandro Paiella, Lucio Piccirillo, C. Kristukat, Federico Pezzotta, Carole Tucker, A. Passerini, Sophie Henrot-Versille, J.-Ch. Hamilton, Nicola Vittorio, M. De Leo, M. Tristram, J. G. Alberro, G. D' Alessandro, L. M. Mundo, Cristian Franceschet, Massimo Gervasi, B. Maffei, L. Grandsire, M. De Petris, K. Ganga, Francesco Cavaliere, S. Marnieros, S. Loucatos, Michel Piat, D. Fracchia, J. Bonaparte, Créidhe O'Sullivan, Laurent Bergé, N. Bleurvacq, A. Mattei, J. Bonis, Gianluca Polenta, L. Mele, J.-P. Bernard, W. Marty, E. Olivieri, H. Pastoriza, Peter Timbie, D. Harari, A. Mennella, D. L. Burke, F. Columbro, Steve Torchinsky, S. Melhuish, Bruce Rafael Mellado Garcia, L.P. Ferreyro, M. Stolpovskiy, Gustavo E. Romero, M. M. Gamboa Lerena, D. T. Hoang, R. Puddu, F. Incardona, D. Bennett, Alessandro Coppolecchia, M. González, S. Spinelli, T. Louis, C. Chapron, P. de Bernardis, P. Ringegni, Marcin Gradziel, François Pajot, A. Fasciszewski, G. Stankowiak, D. Viganò, Luca Lamagna, Alessandro Schillaci, R. Charlassier, L. Dumoulin, J.-P. Thermeau, Andrew May, G. de Gasperis, S. Banfi, Y. Giraud-Heraud, Silvia Masi, J. Kaplan, M. E. García Redondo, J.D. Murphy, B. Bélier, J.M. Salum, S. Dheilly, J. A. Murphy, M. Gaspard, L. A. Montier, Elia S. Battistelli, D. Gayer, F. Voisin, D. Prêle, Gregory S. Tucker, 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 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), 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), Centre de Nanosciences et de Nanotechnologies [Orsay] (C2N), Université Paris-Sud - Paris 11 (UP11)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), 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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), Centre de Nanosciences et de Nanotechnologies (C2N), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), 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), 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 des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Mele, L, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Battistelli, E, Ba, A, B lier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvacq, N, Bonaparte, J, Bonis, J, Bottani, A, Bunn, E, Burke, D, Buzi, D, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppolecchia, A, D'Alessandro, G, Bernardis, P, Gasperis, G, Leo, M, Petris, M, Dheilly, S, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Lerena, M, Ganga, K, Garcia, B, Redondo, M, Gaspard, M, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Hamilton, J, Harari, D, Henrot-Versille, S, Hoang, D, Incardona, F, Jules, E, Kaplan, J, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Maffei, B, Marnieros, S, Marty, W, Masi, S, Mattei, A, May, A, Mcculloch, M, Melhuish, S, Mennella, A, Montier, L, Mousset, L, Mundo, L, Murphy, J, Nati, F, Olivieri, E, Oriol, C, O'Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perciballi, M, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Pr le, D, Puddu, R, Rambaud, D, Ringegni, P, Romero, G, Salatino, M, Salum, J, Schillaci, A, Scoccola, C, Scully, S, Spinelli, S, Stankowiak, G, Stolpovskiy, M, Tartari, A, Thermeau, J, Timbie, P, Tomasi, M, Torchinsky, S, Tristram, M, Tucker, G, Tucker, C, Vigan, D, Vittorio, N, Voisin, F, Wicek, F, Zannoni, M, and Zullo, A
Subjects: History, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], interferometer, Cosmic microwave background, Polarimetry, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Education, law.invention, qubic, polarimetry, bolometric interferometry, cmb, b modes, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, bolometer, law, 0103 physical sciences, Astronomical interferometer, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, 010303 astronomy & astrophysics, detector: design, ComputingMilieux_MISCELLANEOUS, Physics, polarization, business.industry, Gravitational wave, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), calibration, polarization: monitoring, Computer Science Applications, Bolometers, Cosmology, Interferometers, Inflation, Cosmic microwave background, Polarization, Interferometry, modulation, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], performance
Abstract: Measurements of cosmic microwave background (CMB) polarization may reveal the presence of a background of gravitational waves produced during cosmic inflation, providing thus a test of inflationary models. The Q&U Bolometric Interferometer for Cosmology (QUBIC) is an experiment designed to measure the CMB polarization. It is based on the novel concept of bolometric interferometry, which combines the sensitivity of bolometric detectors with the properties of beam synthesis and control of calibration offered by interferometers. To modulate and extract the input polarized signal of the CMB, QUBIC exploits Stokes polarimetry based on a rotating half-wave plate (HWP). In this work, we illustrate the design of the QUBIC instrument, focusing on the polarization modulation system, and we present preliminary results of beam calibrations and the performance of the HWP rotator at 300 K.
Published: 2021

5. The effect of composition on chlorine solubility and behavior in silicate melts

Author: W. Thomas, Richard and J. Wood, Bernard
Abstract: We have performed experiments at 1.5 GPa and 1400 °C on 25 different bulk compositions to determine the effects of major element compositions on the Cl contents of silicate melts at known fugacities of Cl2and O2. The experimental method involved mixing a “sliding” Cl buffer, a mixture of AgCl, AgI, and Ag with the silicate bulk composition and performing the experiment in a graphite capsule together with a source of CO2(AgCO3). The graphite capsules were sealed inside welded Pt tubes to maintain a CO2-CO atmosphere with oxygen fugacity fixed at the C-CO-CO2(CCO) buffer. During the experiment, the Cl buffer segregates leaving a Cl-bearing melt, which quenches to a glass. We used the results to define chloride capacity CClfor each melt at the pressure and temperature of the experiment:
Published: 2023
Full Text: View/download PDF

6. Is training sufficient for ultrasound operators to diagnose deep infiltrating endometriosis and bowel involvement by transvaginal ultrasound?

Author: A. Roséfort, Cyrille Huchon, Arnaud Fauconnier, A. Paternostre, S. Estrade, J.-P. Bernard, Service de gynécologie et obstétrique [CHI Poissy-Saint Germain], CHI Poissy-Saint-Germain, Risques cliniques et sécurité en santé des femmes et en santé périnatale (RISCQ), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Centre Hospitalier Versailles, 78000 Le Chesnay, France, and parent
Subjects: Adult, medicine.medical_specialty, [SDV]Life Sciences [q-bio], Health Personnel, Endometriosis, Diagnostic accuracy, Ultrasound operator training, Sensitivity and Specificity, 03 medical and health sciences, 0302 clinical medicine, Bowel endometriosis, medicine, Humans, Ultrasonography, 030219 obstetrics & reproductive medicine, Transvaginal ultrasonography, business.industry, Transvaginal ultrasound, Ultrasound, Rectum, Obstetrics and Gynecology, Deep infiltrating endometriosis, Confidence interval, Intestines, Reproductive Medicine, 030220 oncology & carcinogenesis, Female, Clinical Competence, Radiology, business
Abstract: International audience; Objectives: To assess and compare the diagnostic accuracy of transvaginal ultrasonography (TVUS) by trained or untrained ultrasound operators in deep infiltrating endometriosis (DIE) imaging, for diagnosing DIE and bowel involvement. Methods: This was an observational study of patients with clinically suspected DIE operated in a reference center. TVUS was performed pre-operatively by a trained or/and untrained ultrasound operator to search for DIE and rectal involvement. During surgery, DIE was diagnosed according to macroscopic and histological criteria. Sensitivity (Se), specificity (Sp) and c-index were calculated with 95% confidence intervals for trained and untrained operators, if TVUS results were significantly predictive of DIE and rectal involvement at p < 0.05. Results: 115 patients were included: 100 (87%) had DIE and 34 (29.6%) had bowel involvement. TVUS was performed by a trained ultrasound operator for 70 patients and by an untrained one for 56 patients. When performed by a trained operator, TVUS significantly predicted DIE with a Se of 58% (95% CI, 46–70), a Sp of 87.5% (95% CI, 63–100) and a c-index of 0.73 (95% CI, 0.59–0.87). TVUS performed by an untrained operator was not significantly predictive of DIE (p = 0.58). Rectal involvement was significantly predicted by TVUS performed by a trained operator with a Se of 40% (95% CI, 23–59), a Sp of 93% (95% CI, 86–100) and a c-index of 0.67 (95% CI, 0.56–0.77). None of the untrained ultrasound operators diagnosed a bowel involvement. Conclusion: TVUS is not sufficient to diagnose DIE and bowel involvement, in particular when performed by untrained ultrasound operators.
Published: 2019

7. 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
Full Text: View/download PDF

8. Calibration of QUBIC: The Q and U bolometric interferometer for cosmology (Erratum)

Author: Andrea Tartari, L. Montier, H. Pastoriza, D. Bennett, M. Wright, Bruno Maffei, Mark McCulloch, S. Marnieros, E. Rasztocky, M. Perciballi, G. S. Tucker, J. Aumont, D. Melo, J. Bonaparte, E. Olivieri, A. Pelosi, D. Auguste, M. Giard, Diego D. Harari, J. P. Bernard, B. García, D. Burke, A. Fasciszewski, L. Piccirillo, C. Kristukat, C. Tucker, J. D. Murphy, Andrew May, J. Bonis, A. Mattei, L. Bergé, D. Rambaud, V. Gilles, F. Wicek, M. R. Hampel, Benoit Belier, M. González, S. Azzoni, Sophie Henrot-Versille, F. Pajot, Giampaolo Pisano, E. Jules, C. Oriol, L. H. Arnaldi, W. Marty, L. Dumoulin, M. Gaspard, M. Gomez Berisso, and P. A. R. Ade
Subjects: Physics, Interferometry, Optics, business.industry, law, Optical engineering, Bolometer, Calibration, business, Cosmology, law.invention
Published: 2021

9. 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

10. Negative ion source development for a photoneutralization based neutral beam system for future fusion reactors

Author: A Simonin, R Agnello, S Bechu, J M Bernard, C Blondel, J P Boeuf, D Bresteau, G Cartry, W Chaibi, C Drag, B P Duval, H P L de Esch, G Fubiani, I Furno, C Grand, Ph Guittienne, A Howling, R Jacquier, C Marini, and I Morgal
Subjects: photoneutralization, helicon, inductively coupled plasma, ion beam sheet, plasma modelling, Science, Physics, QC1-999
Abstract: In parallel to the developments dedicated to the ITER neutral beam (NB) system, CEA-IRFM with laboratories in France and Switzerland are studying the feasibility of a new generation of NB system able to provide heating and current drive for the future DEMOnstration fusion reactor. For the steady-state scenario, the NB system will have to provide a high NB power level with a high wall-plug efficiency ( η ∼ 60%). Neutralization of the energetic negative ions by photodetachment (so called photoneutralization), if feasible, appears to be the ideal solution to meet these performances, in the sense that it could offer a high beam neutralization rate (>80%) and a wall-plug efficiency higher than 60%. The main challenge of this new injector concept is the achievement of a very high power photon flux which could be provided by 3 MW Fabry–Perot optical cavities implanted along the 1 MeV D ^− beam in the neutralizer stage. The beamline topology is tall and narrow to provide laminar ion beam sheets, which will be entirely illuminated by the intra-cavity photon beams propagating along the vertical axis. The paper describes the present R&D (experiments and modelling) addressing the development of a new ion source concept (Cybele source) which is based on a magnetized plasma column. Parametric studies of the source are performed using Langmuir probes in order to characterize and compare the plasma parameters in the source column with different plasma generators, such as filamented cathodes, radio-frequency driver and a helicon antenna specifically developed at SPC-EPFL satisfying the requirements for the Cybele (axial magnetic field of 10 mT, source operating pressure: 0.3 Pa in hydrogen or deuterium). The paper compares the performances of the three plasma generators. It is shown that the helicon plasma generator is a very promising candidate to provide an intense and uniform negative ion beam sheet.
Published: 2016
Full Text: View/download PDF

11. PAH and Dust Processing in Supernova Remnants

Author: J. Rho, M. Andersen, A. Tappe, W. T. Reach, J. P. Bernard, and J. Hewitt
Published: 2020

12. 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

13. 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

14. Planck intermediate results

Author: Y. Akrami, K. J. Andersen, M. Ashdown, 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, C. Burigana, R. C. Butler, E. Calabrese, B. Casaponsa, H. C. Chiang, L. P. L. Colombo, C. Combet, B. P. Crill, F. Cuttaia, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, E. Di Valentino
Published: 2020
Full Text: View/download PDF

15. 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

16. 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

17. Pilot Study of a Software-Supported Protocol for Second-Trimester Ultrasound Screening

Author: Thierry Bultez, Laurent Salomon, Yves Ville, U. Metzger, and J.-P. Bernard
Subjects: Protocol (science), medicine.medical_specialty, 030219 obstetrics & reproductive medicine, Amniotic fluid, Second trimester ultrasound, Radiological and Ultrasound Technology, business.industry, Ultrasound, Cavum septi pellucidi, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, Obstetrics and gynaecology, Sonographer, Medicine, Image acquisition, Radiology, Nuclear Medicine and imaging, Radiology, business
Abstract: Objectives To evaluate the feasibility and impact of using a software-supported protocol for routine second-trimester ultrasound scanning. Methods We conducted a comparative observational study of 2 sets of 25 randomly selected normal routine second-trimester examinations performed by the same expert sonographer before and 1 year after the introduction of a software-supported protocol. The scanning protocol was identical during both periods and conformed to International Society of Ultrasound in Obstetrics and Gynecology guidelines. Two independent expert sonographers reviewed the temporal sequences of fetal anatomic visualization. The examination duration, number of images, time per stored image, and number of recorded anatomic features according to the International Society of Ultrasound in Obstetrics and Gynecology guidelines were compared between the periods. Results The mean examination duration and the number of images stored ± SD were both significantly higher during the period with the software-supported protocol than during the previous period (18.9 ± 5.3 versus 15.3 ± 2.8 minutes, respectively; P = .005; and 52.0 ± 2.4 versus 35.2 ± 3.4; P
Published: 2017

18. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution – Survey Description and Compact Source Catalogue

Author: Karine Demyk, Mark G. Rawlings, Giuseppe Cosentino, Lixia Yuan, Gwanjeong Kim, Dimitris Stamatellos, Satoshi Ohashi, Dalei Li, Yasuo Doi, L. Harvey-Smith, Archana Soam, Anthony Peter Whitworth, Mark Thompson, Izaskun Jiménez-Serra, Gary A. Fuller, Huei-Ru Chen, Tae-Geun Ji, Oscar Morata, Chakali Eswaraiah, Jinyi Yang, Takeshi Sakai, Y. L. Yuan, Hiroko Shinnaga, David Cornu, Jonathan Rawlings, Walter Kieran Gear, Shaila Akhter, Yuri Aikawa, A. Chrysostomou, Fanyi Meng, Andrew Walsh, Christine D. Wilson, P. M. McGehee, M. Chen, Tomoya Hirota, Carsten Henkel, You-Hua Chu, E. Falgarone, S. Kim, Yuxin He, Johanna Malinen, Sung-ju Kang, Chin-Fei Lee, Xuepeng Chen, Miju Kang, Annie Hughes, V.-M. Pelkonen, Graham S. Bell, Woojin Kwon, Huawei Zhang, Bon-Chul Koo, E. Jarken, Glenn J. White, J. X. Ge, Andrew Rigby, A-Ran Lyo, Wayne S. Holland, Hong-Li Liu, Geumsook Park, Mengyao Tang, Emily Drabek-Maunder, Hee-Weon Yi, M. Liu, Tie Liu, Rebeka Bögner, J.-P. Bernard, C. P. Zhang, B. S. Wang, Manash R. Samal, Harriet Parsons, Mika Juvela, Toby J. T. Moore, Lei Zhu, Ya-Wen Tang, Guobao Zhang, Leonardo Bronfman, George J. Bendo, S. Mairs, Serena Viti, H. Wang, Tetsuo Hasegawa, Yuxin Lin, Minho Choi, Zhiyuan Ren, Ke Wang, Yi-Jehng Kuan, David Eden, I. Ristorcelli, Lei Qian, X. Chen, Paul F. Goldsmith, Jinhua He, Diego Mardones, Shih-Ping Lai, Di Li, Soojong Pak, Qizhou Zhang, Ken'ichi Tatematsu, L. Montier, Yuefang Wu, C. Zhou, Guido Garay, Patricio Sanhueza, A. Rivera-Ingraham, Nicolas Peretto, Keping Qiu, Siyi Feng, Patrick M. Koch, Neal J. Evans, Jeong-Eun Lee, Andrew Blain, A. P. Marston, Hua-bai Li, M. Fich, Chao Zhang, Eun Jung Chung, G. Luo, J. Montillaud, Derek Ward-Thompson, Jianjun Zhou, Maria Cunningham, Jungha Kim, N. Lo, Roberta Paladini, J. Di Francesco, Jongsoo Kim, Ye Xu, Xing Lu, Charlotte Vastel, Chang Won Lee, Pak Shing Li, John A. P. Lopez, Per Friberg, Sheng-Li Qin, Gerald Moriarty-Schieven, D. Alina, G. Pech, Wen Ping Chen, O. Fehér, Pei Zuo, Sheng-Yuan Liu, Jinghua Yuan, Scott Chapman, Alessio Traficante, Doug Johnstone, Jane Greaves, Do-Young Byun, Naomi Hirano, Helen J. Fraser, Jiali Wang, Koji S. Kawabata, J. G. A. Wouterloot, X. Guan, Hsien Shang, Annie Zavagno, John Richer, Kee-Tae Kim, Sarolta Zahorecz, Kate Pattle, Y. Lee, L. V. Toth, Kevin Lacaille, Department of Physics, Particle Physics and Astrophysics, Liverpool John Moores University (LJMU), 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), University of Arizona, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), and Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Milky Way, Continuum (design consultancy), SPIRAL ARMS, FOS: Physical sciences, F800, Astrophysics, 01 natural sciences, ISM: clouds, Luminosity, STAR-FORMATION, CLUMP IDENTIFICATION, symbols.namesake, surveys, 0103 physical sciences, Planck, GOULD BELT SURVEY, 010303 astronomy & astrophysics, James Clerk Maxwell Telescope, Solar and Stellar Astrophysics (astro-ph.SR), QC, QB, Physics, LEGACY SURVEY, Spiral galaxy, stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ATLASGAL, Astronomy and Astrophysics, Galactic plane, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, CLOUD, submillimetre: ISM, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], GAS, Astrophysics of Galaxies (astro-ph.GA), symbols, MILKY-WAY, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], COMPLETE SAMPLE
Abstract: We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-um continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of $N_{H_{2}}$ $>$ 5 $\times$ 10$^{21}$ cm$^{-2}$. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other., 16 pages, 13 figures, 1 table. Accepted for publication in MNRAS
Published: 2019

19. [Isolated right aortic arch: prenatal diagnosis characteristics, pregnancy outcomes and systematic review]

Author: I, Bitumba, M, Lévy, J-P, Bernard, Y, Ville, and L-J, Salomon
Subjects: Adult, Male, Aortic Arch Syndromes, Infant, Newborn, Pregnancy Outcome, Ultrasonography, Prenatal, Cleft Palate, Echocardiography, Pregnancy, Humans, Female, Palate, Soft, Gene Deletion, Retrospective Studies
Abstract: To investigate prenatal diagnosis characteristics and pregnancy outcomes associated with isolated right aortic arch (RAA).A retrospective study including fetuses with isolated RAA, managed between January 2010 and February 2018. Cases were identified from the ultrasound databases of the expert pediatric cardiologists, who made the aforementioned diagnosis. All fetuses were examined by a fetal medicine imaging expert to exclude any extracardiac abnormality. A systematic review was performed to assess the prenatal diagnosis and outcomes of fetuses with isolated RAA.Fifty-six fetuses were diagnosed with an isolated RAA. An isolated double aortic arch (DAA) was diagnosed in one fetus. Mean gestational age at diagnosis was 24 weeks. The sex ratio (boy/girl) was 0.89. No significant abnormality was detected in invasive tests (karyotype and FISH or microarray). Only one fetus was misdiagnosed with isolated RAA. He was the only symptomatic (stridor) newborn baby and was later diagnosed with DAA. Four studies were included in our systematic review representing 115 cases of isolated RAA. One significant chromosomal abnormality was detected: a 22q11 deletion in a newborn baby who had a postnatal finding of a soft palate cleft. There was one major obstetric complication: an intrauterine fetal demise at 41 gestational weeks.Diagnosis of isolated RAA can be challenging. Invasive tests are to be discussed. The diagnosis of isolated RAA should not change obstetric monitoring. Nevertheless, an echocardiography should be performed systematically in these new newborn babies within their first month of life.
Published: 2019

20. Statistical analysis of the interplay between interstellar magnetic fields and filaments hosting Planck Galactic cold clumps

Author: K. Ferrière, J.-P. Bernard, I. Ristorcelli, Ernazar Abdikamalov, L. Montier, D. Alina, Mika Juvela, Elisabetta R. Micelotta, Department of Physics, Particle Physics and Astrophysics, 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), Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, 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), and Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki
Subjects: Preferential alignment, PIPE NEBULA, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, macromolecular substances, POLARIMETRY, 01 natural sciences, STAR-FORMATION, Protein filament, Quantitative Biology::Subcellular Processes, symbols.namesake, 0103 physical sciences, Perpendicular, Planck, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, polarization, methods: statistical, 010308 nuclear & particles physics, Linear polarization, Star formation, (ISM:) dust, extinction, Astronomy and Astrophysics, Polarization (waves), equipment and supplies, 115 Astronomy, Space science, CLOUD, Magnetic field, [SDU]Sciences of the Universe [physics], Space and Planetary Science, symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract: We present a statistical study of the relative orientation in the plane of the sky between interstellar magnetic fields and filaments hosting cold clumps. For the first time, we consider both the density of the environment and the density contrast between the filaments and their environment. Moreover, we geometrically distinguish between the clumps and the remaining portions of the filaments. We infer the magnetic field orientations in the filaments and in their environment from the Stokes parameters, 1 assuming optically thin conditions. Thus, we analyse the relative orientations between filaments, embedded clumps, internal and background magnetic fields, depending on their environment and evolutionary stages. We recover the previously observed trend for filaments in low column density environments to be aligned parallel to the background magnetic field; however, we find that this trend is significant only for low-contrast filaments, whereas high-contrast filaments tend to be randomly orientated with respect to the background magnetic field. Filaments in high column density environments do not globally show any preferential orientation, although low-contrast filaments alone tend to have perpendicular relative orientation with respect to the background magnetic field. For a subsample of nearby filaments, for which volume densities can be derived, we find a clear transition in the relative orientation with increasing density, at n(H) similar to 10(3) cm(-3), changing from mostly parallel to mostly perpendicular in the off-clump portions of filaments and from even to bimodal in clumps. Our results confirm a strong interplay between interstellar magnetic fields and filaments during their formation and evolution.
Published: 2019

21. Characterization of the in-flight properties of the Planck telescope

Author: F. Cuttaia, Carlo Burigana, Luca Terenzi, Hannu Kurki-Suonio, Ken Ganga, L. Toffolatti, G. Roudier, Fabrizio Villa, J.-P. Bernard, Charles R. Lawrence, J.-L. Puget, W. C. Jones, Douglas Scott, P. H. Nielsen, B. Partridge, Carol Anne Oxborrow, Peter Meinhold, J. A. Tauber, Jon E. Gudmundsson, A. Martín-Polegre, Hans Ulrik Nørgaard-Nielsen, B. P. Crill, E. Franceschi, N. Mandolesi, M. Sandri, Department of Physics, Helsinki Institute of Physics, 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 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), 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 spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-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), 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), 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 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), ITA, USA, FRA, DEU, DNK, FIN, SWE, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), École normale supérieure - Paris (ENS-PSL), 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), 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), and 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)
Subjects: media_common.quotation_subject, Astrophysics, Grating, 01 natural sciences, law.invention, instruments [Space vehicles], Telescope, symbols.namesake, Optics, law, 0103 physical sciences, space vehicles: instruments, Planck, data analysis [Methods], 010303 astronomy & astrophysics, media_common, [PHYS]Physics [physics], Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, telescopes, Astronomy and Astrophysics, 115 Astronomy, Space science, methods: data analysis, Amplitude, Cardinal point, 13. Climate action, Space and Planetary Science, Sky, Metric (mathematics), symbols, business, Geometric modeling, Telescopes
Abstract: CSIC (Spain); MICINN (Spain); JA (Spain), Tauber, J.A., Nielsen, P.H., Martín-Polegre, A., Crill, B., Cuttaia, F., Ganga, K., Gudmundsson, J., Jones, W., Lawrence, C., Meinhold, P., Norgaard-Nielsen, H.U., Oxborrow, C.A., Partridge, B., Roudier, G., Sandri, M., Scott, D., Terenzi, L., Villa, F., Bernard, J.P., Burigana, C., Franceschi, E., Kurki-Suonio, H., Mandolesi, N., Puget, J.L., Toffolatti, L.
Published: 2019

22. Inflight performance of the PILOT balloon-borne experiment

Author: C. Engel, F. Pajot, J. Martignac, F. Bousqet, Y. Lepennec, S. Maestre, Nicolas Bray, Matthew Joseph Griffin, Peter A. R. Ade, A. Hughes, Silvia Masi, J. Narbonne, G. Foënard, René J. Laureijs, Frederi Mirc, Christopher Tibbs, J. M. Nicot, P. deBernardis, Y. André, G. Roudil, L. Rodriguez, Pierre Tapie, L. Bautista, B. Maffei, P. Etcheto, Etienne Perot, Peter Charles Hargrave, J. A. Tauber, J. P. Dubois, S. Grabarnik, B. Mot, M. Bouzit, L. Montier, O. Boulade, C. Marty, E. Doumayrou, Giampaolo Pisano, Isabelle Ristorcelli, H. Roussel, Nicolas Ponthieu, B. Leriche, A. Mangilli, X. Dupac, C. Tucker, Ph. Gelot, Y. Longval, Giorgio Savini, A. Lacourt, J. Aumont, V. Buttice, R. Misawa, M. Charra, Johan Montel, J. Pimentao, Muriel Saccoccio, W. Marty, B. Crane, M. Chaigneau, J.-P. Bernard, G. Parot, S. Stever, Maria Salatino, O. Simonella, Institut de recherche en astrophysique et planétologie (IRAP), 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), Centre National d'Études Spatiales [Toulouse] (CNES), 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), Université Grenoble Alpes (UGA), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Point spread function, High energy particle, Far infrared, Residual, 01 natural sciences, Glitches, Background, Inflight performances, Interstellar dust, PILOT, Pointing, Polarization, Responses, Straylight, 0103 physical sciences, Calibration, 010303 astronomy & astrophysics, Cosmic dust, Remote sensing, 010308 nuclear & particles physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Polarization (waves), Wavelength, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Environmental science
Abstract: International audience; The Polarized Instrument for Long-wavelength Observation of the Tenuous interstellar medium (PILOT) is a balloon-borne experiment that aims to measure the polarized emission of thermal dust at a wavelength of 240 µm (1.2 THz). A first PILOT flight of the experiment took place from Timmins, Ontario, Canada, in September 2015 and a second flight took place from Alice Springs, Australia in April 2017. In this paper, we present the inflight performance of the instrument. Here we concentrate on the instrument performance as measured during the second flight, but refer to the performance observed during the first flight, if it was significantly different. We present a short description of the instrument and the flights. We measure the time constants of the detectors using the decay of the observed signal during flight following high energy particle impacts (glitches) and switching off the instrument's internal calibration source. We use these time constants to deconvolve the timelines and analyze the optical quality of the instrument as measured on planets. We then analyze the structure and polarization of the instrumental background. We measure the detector response flat field and its time variations using the signal from the residual atmosphere and from the internal calibration source. Finally, we analyze the spectral and temporal properties of the detector noise. The inflight performance is found to be satisfactory and globally in line with expectations from ground calibrations. We conclude by assessing the expected inflight sensitivity of the instrument in light of the measured inflight performance.
Published: 2019

23. 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

24. Planck intermediate results

Author: Y. Akrami, F. Argüeso, 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, L. Bonavera, J. R. Bond, J. Borrill, F. R. Bouchet, C. Burigana, R. C. Butler, E. Calabrese, J. Carron, H. C. Chiang, C. Combet, B. P. Crill, F. Cuttaia, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, and J
Published: 2018
Full Text: View/download PDF

25. Galactic cold cores

Author: Alexander Men'shchikov, Roberta Paladini, Peter G. Martin, V.-M. Pelkonen, Douglas J. Marshall, Deborah Paradis, Mika Juvela, I. Ristorcelli, J. Malinen, A. Marston, Laurent Pagani, L. A. Montier, Nathalie Ysard, L. V. Toth, A. Rivera-Ingraham, J. Montillaud, Derek Ward-Thompson, J.-P. Bernard, Department of Physics, Institut de recherche en astrophysique et planétologie (IRAP), 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), Centre d'étude spatiale des rayonnements (CESR), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / 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), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Laboratoire de Modélisation Multi-échelles des Combustibles (LM2C), Service d'Etudes de Simulation du Comportement du combustibles (SESC), Département d'Etudes des Combustibles (DEC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Département d'Etudes des Combustibles (DEC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), 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 d’Études Spatiales [Paris] (CNES), School of Physics and Astronomy [Cardiff], Cardiff University, Universiti Brunei Darussalam, Biology Department, Universitii Brunei Darussalam, and Eötvös Loránd University (ELTE)
Subjects: FOS: Physical sciences, Context (language use), Astrophysics, macromolecular substances, 01 natural sciences, ISM: clouds, Protein filament, Quantitative Biology::Subcellular Processes, GRAVITY, NEBULA, 0103 physical sciences, FINITE SHEETS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Linear density, infrared: ISM, HERSCHEL, stars: formation, Accretion (meteorology), 010308 nuclear & particles physics, Component (thermodynamics), Star formation, extinction, STAR-FORMING FILAMENTS, Astronomy and Astrophysics, Ridge (differential geometry), 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Supercritical fluid, GRAVITATIONAL COLLAPSE, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), MOLECULAR CLOUDS, submillimeter: ISM, TURBULENCE, dust, dust, extinction, FRAGMENTATION, EMISSION
Abstract: Filaments are key for star formation models. As part of the study carried out by the Herschel GCC Programme, here we study the filament properties presented in GCC.VII in context with theoretical models of filament formation and evolution. A conservative sample of filaments at a distance D, Accepted in A&A
Published: 2017

26. The Hi-GAL compact source catalogue – I. The physical properties of the clumps in the inner Galaxy (−71$_.^circ$0 < ℓ < 67$_.^circ$0)

Author: Takahiro Hayakawa, David Eden, Melvin Hoare, Francesco Strafella, F. Piacentini, Kenneth A. Marsh, Sergio Molinari, S. E. Jaffa, Pedro García-Lario, Alessio Traficante, Peter Schilke, Kengo Tachihara, G. Joncas, J.-P. Bernard, M. R. Pestalozzi, S. Martinavarro-Armengol, Amata Mercurio, Alessandro Costa, Friedrich Wyrowski, Eva Sciacca, Robert Butora, B. Maiolo, Joseph C. Mottram, Mark Thompson, D. Polychroni, H. Yamamoto, G. Li Causi, P. Palmeirim, M. Benedettini, D. Russeil, Hidetoshi Sano, Kazi L.J. Rygl, Eugenio Schisano, Stefano Cavuoti, Annie Zavagno, Sarah Ragan, John Bally, M. Veneziani, Carla Buemi, A. P. Whitworth, K. Torii, Massimo Brescia, Péter Kacsuk, Davide Elia, Marco Molinaro, Nicola Schneider, Ugo Becciani, Rene Plume, Göran Pilbratt, A. M. di Giorgio, F. Faustini, P. Mège, Luca Calzoletti, Grazia Umana, Stefano Pezzuto, H. Arab, E. Fiorellino, Derek Ward-Thompson, S. J. Liu, Marilena Bandieramonte, M. T. Beltrán, Paolo Leto, Y. Maruccia, Roberta Paladini, Toby J. T. Moore, Giuseppe Riccio, Fabio Vitello, Luca Olmi, N. Marchili, Frédérique Motte, Corrado Trigilio, Ákos Hajnal, Yasuo Fukui, Nicolas Peretto, Alberto Noriega-Crespo, A. Baldeschi, Riccardo Cesaroni, Leonardo Testi, Lorenzo Piazzo, Manuel Merello, L. Cambrésy, Filomena Bufano, Peter G. Martin, Nicolas Billot, Meng-Lin Huang, Paolo Natoli, Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, Marilena, Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmeirim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltrán, M. T., Billot, N., Cambrésy, L., Cesaroni, R., García-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mège, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Li Causi, G., Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., Yamamoto, H., Elia, Davide, Pezzuto, S., Noriega Crespo, A., Strafella, Francesco, García Lario, P., Maiolo, BERLINDA MARIA TERESA, Maruccia, Ylenia, Ward Thompson, D., and Martinavarro Armengol, S.
Subjects: Astrophysics and Astronomy, Infrared, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, cataloghi astronomici, mezzo interstellare, osservazioni infrarosse, osservazioni submillimetriche, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB, Physics, Spiral galaxy, 010308 nuclear & particles physics, Star formation, Spectral density, Astronomy, Astronomy and Astrophysics, Galactic plane, Galaxy, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, catalogues, ISM clouds, dust, extinction, local interstellar matter, infrared ISM, submillimetre ISM, Longitude
Abstract: Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 μm. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane −71 ∘. 0 < ℓ < 67 ∘. 0. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-μm counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between ‘on-arm’ and ‘interarm’ positions. Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $\mu$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the portion of Galactic plane $-71.0^{\circ}< \ell < 67.0^{\circ}$. The band-merged catalogue contains 100922 sources with a regular SED, 24584 of which show a 70 $\mu$m counterpart and are thus considered proto-stellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterise different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in proto-stellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to proto-stellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between "on-arm" and "inter-arm" positions.
Published: 2017

27. The optical performance of the PILOT instrument from ground end‐to‐end tests

Author: Y. Longval, O. Boulade, Maria Salatino, O. Simonella, René J. Laureijs, Nicolas Ponthieu, B. Leriche, Y. André, L. Bautista, J. Narbonne, J. A. Tauber, J. P. Dubois, Muriel Saccoccio, Carole Tucker, G. Roudil, Matthew Joseph Griffin, Peter A. R. Ade, Giorgio Savini, Isabelle Ristorcelli, J. Pimentao, L. Rodriguez, A. Caillat, B. Mot, M. Bouzit, A. Hughes, Peter Charles Hargrave, C. Engel, F. Bousqet, J. Montel, B. Maffei, E. Doumayrou, Silvia Masi, J.-P. Bernard, D. Alina, S. Maestre, G. Foënard, P. de Bernardis, L. Montier, M. Chaigneau, J. Aumont, R. Misawa, M. Charra, F. Douchin, W. Marty, Etienne Perot, C. Marty, V. Buttice, S. Grabarnik, Giampaolo Pisano, F. Pajot, B. Crane, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Point spread function, Image quality, Far infrared, 01 natural sciences, 010309 optics, Optics, Polarization, 0103 physical sciences, PILOT, Straylight, 010303 astronomy & astrophysics, QB, Remote sensing, Cosmic dust, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Linear polarization, business.industry, Detector, Interstellar dust, Astronomy and Astrophysics, Space and Planetary Science, Polarization (waves), Wavelength, Cardinal point, business
Abstract: International audience; The Polarized Instrument for Long‐wavelength Observation of the Tenuous interstellar medium (PILOT) is a balloon‐borne astronomy experiment designed to study the linear polarization of thermal dust emission in two photometric bands centred at wavelengths 240 mu m (1.2 THz) and 550 mu m (545 GHz), with an angular resolution of a few arcminutes. Several end‐to‐end tests of the instrument were performed on the ground between 2012 and 2014, in order to prepare for the first scientific flight of the experiment that took place in September 2015 from Timmins, Ontario, Canada. This paper presents the results of those tests, focussing on an evaluation of the instrument's optical performance. We quantify image quality across the extent of the focal plane, and describe the tests that we conducted to determine the focal plane geometry, the optimal focus position, and sources of internal straylight. We present estimates of the detector response, obtained using an internal calibration source, and estimates of the background intensity and background polarization.
Published: 2017

28. The earliest phases of high-mass star formation, as seen in NGC 6334 by Herschel-HOBYS

Author: Pierre Didelon, L. D. Anderson, Sergio Molinari, Doris Arzoumanian, Stefano Pezzuto, Nicola Schneider, Jason M. Kirk, Q. Nguyen Luong, Vincent Minier, G. Leuleu, J. Di Francesco, F. Louvet, Pierrick Martin, M. Benedettini, K. L. J. Rygl, Annie Zavagno, D. Russeil, T. Rayner, J. Bardagi, D. Polychroni, T. Nony, Ph. André, M. Figueira, Tracey Hill, J.-P. Bernard, P. Persi, Davide Elia, Vera Konyves, A. Rivera-Ingraham, G. J. White, H. Roussel, Luigi Spinoglio, J. Tigé, Sylvain Bontemps, M. Hennemann, Frédérique Motte, Sciences pour l'environnement (SPE), Université Pascal Paoli (UPP)-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 (UMR7158 / 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), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), FORMATION STELLAIRE 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Centre National d’Études Spatiales [Paris] (CNES), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Centro de Matemática e Aplicações Fundamentais (CMAF), Universidade de Lisboa = University of Lisbon (ULISBOA), Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Faculty of Informatics [Lugano], Università della Svizzera italiana = University of Italian Switzerland (USI), School of Physics and Astronomy [Cardiff], Cardiff University, 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), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Engineering Department, University of Cambridge [UK] (CAM), Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP), 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)), 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-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidade de Lisboa (ULISBOA), Consiglio Nazionale delle Ricerche (CNR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), ITA, GBR, FRA, and CAN
Subjects: Physics, stars: formation, 010504 meteorology & atmospheric sciences, stars: protostars, Star formation, extinction, Molecular cloud, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, ISM: clouds, Spire, ISM: individual objects: NGC 6334, Space and Planetary Science, 0103 physical sciences, High mass, Protostar, submillimeter: ISM, Millimeter, dust, extinction, dust, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: Aims: To constrain models of high-mass star formation, the Herschel-HOBYS key program aims at discovering massive dense cores (MDCs) able to host the high-mass analogs of low-mass prestellar cores, which have been searched for over the past decade. We here focus on NGC 6334, one of the best-studied HOBYS molecular cloud complexes. Methods: We used Herschel/PACS and SPIRE 70-500 μm images of the NGC 6334 complex complemented with (sub)millimeter and mid-infrared data. We built a complete procedure to extract 0.1 pc dense cores with the getsources software, which simultaneously measures their far-infrared to millimeter fluxes. We carefully estimated the temperatures and masses of these dense cores from their spectral energy distributions (SEDs). We also identified the densest pc-scale cloud structures of NGC 6334, one 2 pc × 1 pc ridge and two 0.8 pc × 0.8 pc hubs, with volume-averaged densities of 105 cm-3. Results: A cross-correlation with high-mass star formation signposts suggests a mass threshold of 75 M☉ for MDCs in NGC 6334. MDCs have temperatures of 9.5-40 K, masses of 75-1000 M☉, and densities of 1 × 105-7 × 107 cm-3. Their mid-infrared emission is used to separate 6 IR-bright and 10 IR-quiet protostellar MDCs while their 70 μm emission strength, with respect to fitted SEDs, helps identify 16 starless MDC candidates. The ability of the latter to host high-mass prestellar cores is investigated here and remains questionable. An increase in mass and density from the starless to the IR-quiet and IR-bright phases suggests that the protostars and MDCs simultaneously grow in mass. The statistical lifetimes of the high-mass prestellar and protostellar core phases, estimated to be 1-7 × 104 yr and at most 3 × 105 yr respectively, suggest a dynamical scenario of high-mass star formation. Conclusions: The present study provides good mass estimates for a statistically significant sample, covering the earliest phases of high-mass star formation. High-mass prestellar cores may not exist in NGC 6334, favoring a scenario presented here, which simultaneously forms clouds, ridges, MDCs, and high-mass protostars. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Catalogs built from Tables A.1-A.12, are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/602/A77
Published: 2017

29. Molecular hydrogen emission in the interstellar medium of the Large Magellanic Cloud

Author: You-Hua Chu, Joana M. Oliveira, J.-P. Bernard, Suzanne C. Madden, J. Seok, S. Hony, J. Th. van Loon, William T. Reach, Oscar Morata, Hiroyuki Hirashita, Karl D. Gordon, Y. Yang, Margaret Meixner, Frédéric Galliano, Remy Indebetouw, N. Naslim, C. Bot, Annie Hughes, Aigen Li, Vianney Lebouteiller, Sundar Srinivasan, Masaaki Otsuka, Francisca Kemper, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Institute of Oceanology [China], 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), inconnu, Inconnu, Astrophysique Interprétation Modélisation (AIM (UMR7158 / 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), 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), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Infrared, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Excitation temperature, 7. Clean energy, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Large Magellanic Cloud, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, Physics, Photodissociation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Interstellar medium, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Excited state, Atomic physics, Mass fraction
Abstract: We present the detection and analysis of molecular hydrogen emission toward ten interstellar regions in the Large Magellanic Cloud. We examined low-resolution infrared spectral maps of twelve regions obtained with the Spitzer infrared spectrograph (IRS). The pure rotational 0--0 transitions of H$_2$ at 28.2 and 17.1${\,\rm \mu m}$ are detected in the IRS spectra for ten regions. The higher level transitions are mostly upper limit measurements except for three regions, where a 3$\sigma$ detection threshold is achieved for lines at 12.2 and 8.6${\,\rm \mu m}$. The excitation diagrams of the detected H$_2$ transitions are used to determine the warm H$_2$ gas column density and temperature. The single-temperature fits through the lower transition lines give temperatures in the range $86-137\,{\rm K}$. The bulk of the excited H$_2$ gas is found at these temperatures and contributes $\sim$5-17% to the total gas mass. We find a tight correlation of the H$_2$ surface brightness with polycyclic aromatic hydrocarbon and total infrared emission, which is a clear indication of photo-electric heating in photodissociation regions. We find the excitation of H$_2$ by this process is equally efficient in both atomic and molecular dominated regions. We also present the correlation of the warm H$_2$ physical conditions with dust properties. The warm H$_2$ mass fraction and excitation temperature show positive correlations with the average starlight intensity, again supporting H$_2$ excitation in photodissociation regions., Comment: Accepted for publication in MNRAS
Published: 2014

30. Traitement endoscopique d’une fistule colique due à une pancréatite aiguë nécrosante : à propos d’un cas

Author: L Heyries, J P Ratone, X. Truchet, and J P Bernard
Subjects: Gynecology, medicine.medical_specialty, business.industry, Medicine, Radiology, Nuclear Medicine and imaging, business
Abstract: Les pancreatites aigues severes se compliquent de fistules coliques dans environ 3 a 5 % des cas. Le traitement de reference est une prise en charge chirurgicale avec souvent derivation digestive temporaire. Nous reportons le cas d’un homme de 37 ans presentant une fistule colique apres pancreatite aigue necrosante. Avant la mise en evidence de la fistule, un pseudokyste a fait l’objet d’un drainage transgastrique perendoscopique. Devant la persistance d’un etat septique, le patient a ete adresse dans notre centre. Une necrosectomie endoscopique a ete realisee et un drain nasokystique a ete mis en place pour lavages iteratifs. Une fistule kystocolique a ete mise en evidence de maniere fortuite lors de l’opacification via ce drain. Un traitement medical a ete ensuite conduit avec antibiotiques, antifongique adaptes aux differents prelevements, derives de la somatostatine ainsi que drainage percutane sous scanner d’une collection dans le flanc gauche. Apres lavages iteratifs via les deux drains, l’opacification de controle ne montrait plus de fistule, les drains ont ete retires sans recidive a ce jour.
Published: 2014

31. Planck intermediate results: XLII. Large-scale galactic magnetic fields

Author: Rashid Sunyaev, L. P. L. Colombo, M. López-Caniego, L. A. Wade, K. Ganga, Daniela Paoletti, Jose M. Diego, Dipak Munshi, M. Bucher, Douglas Scott, Luigi Danese, X. Dupac, Valeria Pettorino, P. Vielva, Andrew W. Strong, F. Piacentini, Jacques Delabrouille, Krzysztof M. Gorski, Davide Maino, L. Pagano, P. R. Christensen, Erminia Calabrese, Sabino Matarrese, Ben Rusholme, Jussi Valiviita, T. R. Jaffe, F. Pasian, N. Bartolo, E. Franceschi, Fabio Finelli, M. Migliaccio, Charles R. Lawrence, Mariachiara Rossetti, Ted Kisner, A. Moneti, J. A. Murphy, L. Montier, Jean-François Cardoso, Anna Gregorio, Federico Nati, R. Adam, Luca Terenzi, C. Combet, Niels Oppermann, Jörg P. Rachen, Alessandro Gruppuso, Andrea Zacchei, Michele Liguori, A. Mennella, D. Yvon, Jose Alberto Rubino-Martin, D. L. Harrison, Peter A. R. Ade, M. Frailis, Olivier Doré, F. Couchot, Mika Juvela, Carlo Baccigalupi, M. Linden-Vørnle, J.-P. Bernard, Rashmikant V. Sudiwala, Michael P. Hobson, G. de Zotti, J.-L. Puget, L. Toffolatti, Franz Elsner, François Levrier, C. Hernández-Monteagudo, A. Renzi, R. Stompor, J. González-Nuevo, F. Cuttaia, Benjamin D. Wandelt, Julian Borrill, F. Van Tent, Katia Ferrière, G. Roudier, L. Perotto, François R. Bouchet, P. B. Lilje, Anthony Lasenby, A. A. Fraisse, E. Gjerløw, Rodrigo Leonardi, M. Maris, E. Keihänen, A. Benoit-Lévy, S. Galeotta, G. W. Pratt, M. Giard, Alessandro Melchiorri, A. J. Banday, Klaus Dolag, J.-F. Sygnet, J. A. Tauber, J.-M. Lamarre, Olivier Forni, E. Orlando, M. Savelainen, M. Tucci, D. Santos, Gianluca Morgante, B. P. Crill, Roberta Paladini, A.-S. Suur-Uski, Matthieu Tristram, M. Tomasi, Andrew H. Jaffe, Allan Hornstrup, Philip Lubin, C. Renault, F. K. Hansen, Marco Bersanelli, Marc-Antoine Miville-Deschênes, M. Sandri, H. K. Eriksen, Etienne Pointecouteau, Luca Valenziano, A. De Rosa, Laura Bonavera, Pavel Naselsky, G. Maggio, A. Curto, Stéphane Plaszczynski, R. J. Davis, S. R. Hildebrandt, G. Polenta, Clive Dickinson, Hannu Kurki-Suonio, Reijo Keskitalo, Carlo Burigana, Fabrizio Villa, Ingunn Kathrine Wehus, R. B. Barreiro, J. P. Leahy, Massimiliano Lattanzi, F. Pajot, K. Benabed, P. de Bernardis, R. C. Butler, W. C. Jones, J. R. Bond, Nicolas Ponthieu, A. Mangilli, N. Mandolesi, J. Aumont, G. Hurier, I. Ristorcelli, D. Herranz, E. Martínez-González, A. Catalano, M. Piat, Silvia Masi, A. Ducout, J. F. Macías-Pérez, Graca Rocha, Locke D. Spencer, V. Stolyarov, Martin Kunz, Mathieu Remazeilles, Jon E. Gudmundsson, J. Knoche, Simon Prunet, P. Bielewicz, M. Reinecke, Torsten A. Enßlin, Andrea Zonca, H. C. Chiang, M. Ashdown, Paolo Natoli, Francois Boulanger, M. I. R. Alves, Peter G. Martin, E. Battaner, Tuhin Ghosh, Hans Ulrik Nørgaard-Nielsen, Elena Pierpaoli, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), 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 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), Planck Collaboration, Adam, R., Ade, P. A. R., Alves, M. I. R., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Benabed, K., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. F., Catalano, A., Chiang, H. C., Christensen, P. R., Colombo, L. P. L., Combet, C., Couchot, F., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dolag, K., Doré, O., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Gudmundsson, J. E., Hansen, F. K., Harrison, D. L., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hobson, M., Hornstrup, A., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Kunz, M., Kurki Suonio, H., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Melchiorri, A., Mennella, A., Migliaccio, M., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Nørgaard Nielsen, H. U., Oppermann, N., Orlando, Elena, Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Pratt, G. W., Prunet, S., Puget, J. L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rossetti, M., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, R., Strong, A. W., Sudiwala, R., Sunyaev, R., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Valenziano, L., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Yvon, D., Zacchei, A., Zonca, A., Adam, R, Ade, P, Alves, M, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartolo, N, Battaner, E, Benabed, K, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bucher, M, Burigana, C, Butler, R, Calabrese, E, Cardoso, J, Catalano, A, Chiang, H, Christensen, P, Colombo, L, Combet, C, Couchot, F, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davis, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Dolag, K, Doré, O, Ducout, A, Dupac, X, Elsner, F, Enßlin, T, Eriksen, H, Ferrière, K, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Gjerløw, E, González Nuevo, J, Górski, K, Gregorio, A, Gruppuso, A, Gudmundsson, J, Hansen, F, Harrison, D, Hernández Monteagudo, C, Herranz, D, Hildebrandt, S, Hobson, M, Hornstrup, A, Hurier, G, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, T, Knoche, J, Kunz, M, Kurki Suonio, H, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leahy, J, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, López Caniego, M, Lubin, P, Macías Pérez, J, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martínez González, E, Masi, S, Matarrese, S, Melchiorri, A, Mennella, A, Migliaccio, M, Moneti, A, Montier, L, Morgante, G, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Nørgaard Nielsen, H, Oppermann, N, Orlando, E, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Pasian, F, Perotto, L, Pettorino, V, Piacentini, F, Piat, M, Pierpaoli, E, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Ristorcelli, I, Rocha, G, Rossetti, M, Roudier, G, RUBINO MARTIN, J, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Scott, D, Spencer, L, Stolyarov, V, Stompor, R, Strong, A, Sudiwala, R, Sunyaev, R, Suur Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Valenziano, L, Valiviita, J, Van Tent, F, Vielva, P, Villa, F, Wade, L, Wandelt, B, Wehus, I, Yvon, D, Zacchei, A, and Zonca, A
Subjects: magnetic field [ISM], Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, NO, symbols.namesake, ISM: magnetic field, law, Polarization, 0103 physical sciences, Faraday effect, general, ISM: magnetic fields, polarization [ISM], Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, ISM: general, QB, Physics, ISM: magnetic fields, polarization, Astronomy and Astrophysics, Space and Planetary Science, general [ISM], 010308 nuclear & particles physics, Settore FIS/05, magnetic fields [ISM], Observable, Astronomy and Astrophysic, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Synchrotron, Magnetic field, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Microwave, Lepton
Abstract: Recent models for the large-scale Galactic magnetic fields in the literature have been largely constrained by synchrotron emission and Faraday rotation measures. We use three different but representative models to compare their predicted polarized synchrotron and dust emission with that measured by the Planck satellite. We first update these models to match the Planck synchrotron products using a common model for the cosmic-ray leptons. We discuss the impact on this analysis of the ongoing problems of component separation in the Planck microwave bands and of the uncertain cosmic-ray spectrum. In particular, the inferred degree of ordering in the magnetic fields is sensitive to these systematic uncertainties, and we further show the importance of considering the expected variations in the observables in addition to their mean morphology. We then compare the resulting simulated emission to the observed dust polarization and find that the dust predictions do not match the morphology in the Planck data but underpredict the dust polarization away from the plane. We modify one of the models to roughly match both observables at high latitudes by increasing the field ordering in the thin disc near the observer. Though this specific analysis is dependent on the component separation issues, we present the improved model as a proof of concept for how these studies can be advanced in future using complementary information from ongoing and planned observational projects., Comment: 31 pages, 16 figures, updated to match accepted A&A version
Published: 2016

32. Polarization measurement analysis III. Analysis of the polarization angle dispersion function with high precision polarization data

Author: Ernazar Abdikamalov, L. A. Montier, François Levrier, D. Alina, I. Ristorcelli, and J.-P. Bernard
Subjects: Physics, Brewster's angle, 010504 meteorology & atmospheric sciences, Covariance matrix, Linear polarization, Monte Carlo method, Polarimetry, Estimator, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Covariance, Polarization (waves), 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Computational physics, symbols.namesake, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, symbols, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: High precision polarization measurements open new opportunities for the study of the magnetic field structure as traced by polarimetric measurements of the interstellar dust emission. Polarization parameters suffer from bias in the presence of measurement noise. It is critical to take into account all the information available in the data in order to accurately derive these parameters. The goal of this paper is to characterize the bias on the polarization angle dispersion function that is used to study the spatial coherence of the polarization angle. We characterize, for the first time, the bias on the conventional estimator of the polarization angle dispersion function (S hereafter) and show that it can be positive or negative depending on the true value. Monte Carlo simulations are performed in order to explore the impact of the noise properties of the polarization data, as well as the impact of the distribution of the true polarization angles on the bias. We show that in the case where the ellipticity of the noise in (Q, U) varies by less than 10 percent, one can use simplified, diagonal approximation of the noise covariance matrix. In other cases, the shape of the noise covariance matrix should be taken into account in the estimation of S. We also study new estimators such as the dichotomic and the polynomial estimators. Though the dichotomic estimator cannot be directly used to estimate S, we show that, on the one hand, it can serve as an indicator of the accuracy of the conventional estimator and, on the other hand, it can be used for deriving the polynomial estimator. We propose a method for determining the upper limit of the bias on the conventional estimator of S. The method is applicable to any linear polarization data set for which the noise covariance matrices are known., 12 pages, 12 figures. Accepted for publication to Astronomy & Astrophysics
Published: 2016

33. Hi-GAL, the Herschel infrared Galactic Plane Survey: Photometric maps and compact source catalogues: First data release for the inner Milky Way: +68° ≥ l ≥ -70°

Author: Stefano Pezzuto, Annie Zavagno, M. J. Barlow, Nicolas Peretto, S. D. Lord, Yasuo Fukui, Davide Elia, G. Polenta, D. Russeil, Sergio Molinari, Thomas P. Robitaille, R. Del Grande, G. Umana, Riccardo Cesaroni, M. Benedettini, Pascal André, Benjamin L. Schulz, Babar Ali, Pierrick Martin, David Eden, P. Natoli, Göran Pilbratt, Manuel Merello, R. Paladini, Francesco Strafella, Alessio Traficante, Luca Calzoletti, Mathieu Compiegne, Derek Ward-Thompson, Peter Schilke, Gilles Joncas, Rene Plume, Nicola Schneider, Pedro García-Lario, J.-P. Bernard, Kazi L.J. Rygl, Leonardo Testi, M. T. Beltrán, M. R. Pestalozzi, F. Piacentini, A. M. di Giorgio, Eugenio Schisano, Christopher M. Brunt, John Bally, N. Billot, Maggie A. Thompson, Sean K. Carey, Joseph C. Mottram, B. M. Swinyard, Melvin Hoare, F. Faustini, S. J. Liu, S. Martinavarro-Armengol, D. Paradis, Toby J. T. Moore, D. Polychroni, Antonella Palmese, Friedrich Wyrowski, Alberto Noriega-Crespo, Lorenzo Piazzo, Tanya Lim, M. Veneziani, Meng-Lin Huang, Bruce Sibthorpe, and Frédérique Motte
Subjects: Physics, Line-of-sight, 010308 nuclear & particles physics, Infrared, Milky Way, Bolometer, Astronomy and Astrophysics, Astrophysics, Galactic plane, dust, extinction, Galaxy: disk, infrared: ISM, methods: data analysis, stars: formation, techniques: photometric, astronomy and astrophysics, space and planetary science, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, law.invention, symbols.namesake, Wavelength, 13. Climate action, Space and Planetary Science, law, 0103 physical sciences, symbols, Spectral energy distribution, Planck, 010303 astronomy & astrophysics, QC, QB
Abstract: (Abridged) We present the first public release of high-quality data products (DR1) from Hi-GAL, the {\em Herschel} infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic Plane surveys from the near-IR to the radio, and covers five wavebands at 70, 160, 250, 350 and 500 micron, encompassing the peak of the spectral energy distribution of cold dust for 8 < T < 50K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68{\deg} > l > -70{\deg} in a |b, Comment: Astronomy & Astrophysics, accepted
Published: 2016

34. PILOT: a balloon-borne experiment to measure the polarized FIR emission of dust grains in the interstellar medium

Author: J. Pimentao, G. Parot, L. Montier, J. Aumont, Bruno Maffei, M. Bouzit, L. Bautista, R. Misawa, B. Crane, B. Leriche, S. Grabarnik, A. Caillat, Nicolas Ponthieu, M. Charra, F. Bousquet, Peter Charles Hargrave, Giampaolo Pisano, Y. Lepennec, J. Narbonne, S. Maestre, Y. André, Maria Salatino, O. Simonella, F. Mirc, F. Douchin, A. Hughes, J.-P. Bernard, Matthew Joseph Griffin, P. Etcheto, Peter A. R. Ade, J. A. Tauber, Giorgio Savini, Carole Tucker, P. Gélot, G. Foënard, G. Roudil, J. P. Crussaire, W. Marty, C. Engel, Muriel Saccoccio, M. Chaigneau, F. Pajot, J. M. Nicot, Y. Longval, Isabelle Ristorcelli, L. Rodriguez, O. Boulade, P. de Bernardis, J.-P. Torre, Silvia Masi, Johan Montel, J. Martignac, E. Pérot, Nicolas Bray, B. Mot, V. Buttice, C. Marty, E. Doumayrou, René J. Laureijs, J.-P. Dubois, and P. Tapie
Subjects: Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Cosmology, Space exploration, law.invention, 010309 optics, law, instrumentation, interstellar medium, polarization, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Pilot experiment, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Polarization (waves), Galaxy, Interstellar medium
Abstract: Future cosmology space missions will concentrate on measuring the polarization of the Cosmic Microwave Background, which potentially carries invaluable information about the earliest phases of the evolution of our universe. Such ambitious projects will ultimately be limited by the sensitivity of the instrument and by the accuracy at which polarized foreground emission from our own Galaxy can be subtracted out. We present the PILOT balloon project, which aims at characterizing one of these foreground sources, the polarized continuum emission by dust in the diffuse interstellar medium. The PILOT experiment also constitutes a test-bed for using multiplexed bolometer arrays for polarization measurements. This paper presents the instrument and its expected performances. Performance measured during ground calibrations of the instrument and in flight will be described in a forthcoming paper.
Published: 2016

35. Galactic cold cores

Author: Roberta Paladini, D. J. Marshall, L. Montier, J. Montillaud, I. Ristorcelli, J. Malinen, P. M. McGehee, C. Lefèvre, Nathalie Ysard, Peter G. Martin, V.-M. Pelkonen, A. Rivera-Ingraham, L. V. Tóth, Mika Juvela, J.-P. Bernard, Laurent Pagani, Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Institut de recherche en astrophysique et planétologie (IRAP), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / 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), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), 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 d’Études Spatiales [Paris] (CNES), Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Eötvös Loránd University (ELTE), Canadian Institute for Theoretical Astrophysics (CITA), University of Helsinki, 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), 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-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), 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), Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Finnish Centre for Astronomy with ESO (FINCA), University of Turku, 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), 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), 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 Helsinki-University of Helsinki, 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 (UMR_8112)), Observatoire de Paris, and 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)
Subjects: Opacity, Extinction (astronomy), Interstellar cloud, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: clouds, Optical depth (astrophysics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, infrared: ISM, stars: formation, stars: protostars, Star formation, extinction, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, Astrophysics::Earth and Planetary Astrophysics, dust, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The project Galactic Cold Cores has made Herschel observations of interstellar clouds where the Planck satellite survey has located cold and compact clumps. The sources range from starless clumps to protostellar cores. We examine 116 Herschel fields to estimate the submillimetre dust opacity and its variations. The submillimetre dust opacity was derived from Herschel data, and near-infrared observations of the reddening of background stars are converted into near-infrared optical depth. We studied the systematic errors affecting these parameters and used modelling to correct for the expected biases. The ratio of 250um and J band opacities is correlated with the cloud location and star formation activity. We find a median ratio of tau(250um)/tau(J)= (1.6+-0.2)*10^-3, which is more than three times the mean value in diffuse medium. Assuming a spectral index beta=1.8 instead of beta=2.0, the value would be lower by ~30%. No significant systematic variation is detected with Galactocentric distance or with Galactic height. The tau(250um)/tau(J) maps reveal six fields with clear increase of submillimetre opacity of up to tau(250um)/tau(J) ~ 4*10^-3. These are all nearby fields with spatially resolved clumps of high column density. We interpret the increase in the far-infrared opacity as a sign of grain growth in the densest and coldest regions of interstellar clouds., 28 pages, A&A, in press
Published: 2015

36. From forced collapse to H ii region expansion in Mon R2: Envelope density structure and age determination with Herschel

Author: Frédérique Motte, D. Ward-Thompson, Annie Zavagno, D. Russeil, Marc Sauvage, Pierre Didelon, M. Hennemann, J. Di Francesco, Thomas Rayner, L. D. Anderson, A. Rivera-Ingraham, F. Louvet, Glenn J. White, Doris Arzoumanian, Sacha Hony, Alexander Men'shchikov, Ph. André, Frédéric Galliano, Nicolas Peretto, J.-P. Bernard, Tracey Hill, Pascal Tremblin, Vianney Lebouteiller, Vera Könyves, P. Palmeirim, Q. Nguyen Luong, M. Benedettini, K. L. J. Rygl, Stefano Pezzuto, Vincent Minier, M. González, Patrick Hennebelle, Matthew James Griffin, Sylvain Bontemps, Nicola Schneider, Astrophysique Interprétation Modélisation (AIM (UMR7158 / 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), University of Exeter, Maison de la Simulation (MDLS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de Recherche en Informatique et en Automatique (Inria)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Joint ALMA Office, Département d'Astrophysique (ex SAP) (DAP), 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, National Radio Astronomy Observatory (NRAO), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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), FORMATION STELLAIRE 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), 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), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), National Research Council of Canada (NRC), Institut de recherche en astrophysique et planétologie (IRAP), Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), ANR-08-BLAN-0241,PROBES,Etoiles Proto-OB : recherche systématique dans notre Galaxie des cibles pour ALMA(2008), 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université Paris-Sud - Paris 11 (UP11)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA), 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 Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Ionization, H II region, ISM: individual objects: Mon R2, Numerical models, ISM: structure, Extinction (astronomy), FOS: Physical sciences, Collapse (topology), F500, Astrophysics, Isothermal process, Stars: protostars, Clouds, Quenching, H II regions, Solar and Stellar Astrophysics (astro-ph.SR), Envelope (waves), QB, Physics, Dust , extinction, Molecular cloud, Astronomy and Astrophysics, Stars, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Density of gases
Abstract: The surroundings of HII regions can have a profound influence on their development, morphology, and evolution. This paper explores the effect of the environment on H II regions in the MonR2 molecular cloud. We aim to investigate the density structure of envelopes surrounding HII regions and to determine their collapse and ionisation expansion ages. The Mon R2 molecular cloud is an ideal target since it hosts an H II region association. Column density and temperature images derived from Herschel data were used together to model the structure of HII bubbles and their surrounding envelopes. The resulting observational constraints were used to follow the development of the Mon R2 ionised regions with analytical calculations and numerical simulations. The four hot bubbles associated with H II regions are surrounded by dense, cold, and neutral gas envelopes. The radial density profiles are reminiscent of those of low-mass protostellar envelopes. The inner parts of envelopes of all four HII regions could be free-falling because they display shallow density profiles. As for their outer parts, the two compact HII regions show a density profile, which is typical of the equilibrium structure of an isothermal sphere. In contrast, the central UCHii region shows a steeper outer profile, that could be interpreted as material being forced to collapse. The size of the heated bubbles, the spectral type of the irradiating stars, and the mean initial neutral gas density are used to estimate the ionisation expansion time, texp, 0.1Myr,for the dense UCHII and compact HII regions and 0.35 Myr for the extended HII region. The envelope transition radii between the shallow and steeper density profiles are used to estimate the time elapsed since the formation of the first proto stellar embryo, Tinf : 1Myr, for the ultra-compact, 1.5 / 3Myr for the compact, and greater than 6Myr for the extended HII regions., 25pages A&A sous presse
Published: 2015

37. PAH and Dust Processing in Supernova Remnants

Author: John W. Hewitt, J.-P. Bernard, William T. Reach, Jeonghee Rho, Morten Andersen, and Achim Tappe
Subjects: Physics, Supernova, Space and Planetary Science, Primary sites, Hydrogen molecule, General Engineering, medicine, Astronomy, Astronomy and Astrophysics, Astrophysics, medicine.symptom, Spectral line, Confusion
Abstract: I present observations of shock-processed PAHs and dust in supernova remnants (SNRs). Supernova shocks are one of the primary sites destroying, fragmenting and altering interstellar PAHs and dust. Studies of PAHs through supernova shocks had been limited because of confusion with PAHs in background emission. Spitzer observations with high sensitivity and resolution allow us to separate PAHs associated with the SNRs and unrelated, Galactic PAHs. In the young SNR N132D, PAH features are detected with a higher PAH ratio of 15–20/7.7 μ m than those of other astronomical objects, and we suggest large PAHs have survived behind the shock. We present the spectra of additional 14 SNRs observed with Spitzer IRS and MIPS SED covering the range of 5–90 μ m. Bright PAH features from 6.2 to 15–20 μ m are detected from many of SNRs which emit molecular hydrogen lines, indicating that both large and small PAHs survive in low velocity shocks. We observe a strong correlation between PAH detection and carbonaceous small grains, while a few SNRs with dominant silicate dust lack PAH features. We characterize PAHs depending on the shock velocity, preshock density and temperature of hot gas, and discuss PAH and dust processing in shocks and implication of PAH and dust cycles in ISM.
Published: 2011

38. The SAGE-Spec Spitzer Legacy programme: the life-cycle of dust and gas in the Large Magellanic Cloud - Point source classification I

Author: B. O'Halloran, E. van Aarle, Olivia Jones, C. Dijkstra, Igor Soszyński, Robert Blum, Angela Speck, Mikako Matsuura, Sundar Srinivasan, Alexander G. G. M. Tielens, Brandon Lawton, Eric Lagadec, A. J. Mulia, Martin Cohen, S. Hony, Clio Gielen, A. N. Wilkins, Karl D. Gordon, Maud Galametz, Bernie Shiao, D. Rubin, Kathleen E. Kraemer, B. A. Sargent, Karin Sandstrom, J. Th. van Loon, Joseph L. Hora, Joana M. Oliveira, Iain McDonald, Varoujan Gorjian, Jarron Leisenring, Massimo Marengo, Greg Sloan, Paul M. Woods, R. Paladini, Kevin Volk, S. D. Van Dyk, K. A. G. Olsen, J. Harris, D. Riebel, Martha L. Boyer, Frédéric Galliano, B. A. Whitney, William T. Reach, Remy Indebetouw, H. Van Winckel, Marta Sewilo, Margaret Meixner, Albert A. Zijlstra, D. Paradis, S. C. Madden, Vallia Antoniou, Uma P. Vijh, J.-P. Bernard, Francisca Kemper, Ryszard Szczerba, Akiko Kawamura, C. McGuire, and C.-H. R. Chen
Subjects: Physics, Space and Planetary Science, Point source, SAGE, Astronomy, Spec#, Astronomy and Astrophysics, Large Magellanic Cloud, computer, computer.programming_language
Published: 2010

39. Épaisseur de la clarté nucale A 11–14 SA : courbes et équations françaises

Author: L.J. Salomon, G.E. Chalouhi, J.-P. Bernard, and Y. Ville
Subjects: Maternity and Midwifery
Published: 2010

40. Prevention of Early Familial Maladjustment by Parent-Staff Group Meetings: Influence of Familial Background

Author: Y Laurian, J P Bernard, J P Allain, J P Proust, and D Frommel
Subjects: Male, medicine.medical_specialty, Discussion group, business.industry, Hematology, Hemophilia A, Haemophilia, medicine.disease, Chronic disease, Patient Education as Topic, Professional-Family Relations, Child, Preschool, hemic and lymphatic diseases, Adaptation, Psychological, Familial history, Humans, Medicine, Family, business, Psychiatry, Psychosocial, FAMILIAL MALADJUSTMENT
Abstract: The possibility of preventing some major familial maladjustment following the diagnosis of severe haemophilia in the frame of free discussion group was explored. Five couples, 3 with a familial history of haemophilia and 2 without met 5 times over a 2 year period with 3 staff members for a full day. Transcripts of tape recorded sessions were analyzed. Parents with no familial history were apparently more affected but had a more dynamic approach towards hemophilia than the others. They benefited more from the program. Four of the five families were able to treat their child at home before 4 years of age. This new approach seems to help parents to adjust to this severe chronic disease and staff members to reconsider their interaction with parents.
Published: 2009

41. THE DUST-TO-GAS RATIO IN THE SMALL MAGELLANIC CLOUD TAIL

Author: William T. Reach, S. C. Madden, Geoffrey C. Clayton, Karl D. Gordon, Aigen Li, Linda J. Smith, Joseph L. Hora, Caroline Bot, Barbara A. Whitney, J.-P. Bernard, Remy Indebetouw, Frank P. Israel, Marilyn R. Meade, Erik Muller, Charles W. Engelbracht, J. Th. van Loon, S. Bracker, Alberto D. Bolatto, Marta Sewilo, Bernie Shiao, Margaret Meixner, Karl Misselt, Brian Babler, and M. Block
Subjects: Physics, Infrared, Metallicity, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Plasma, complex mixtures, respiratory tract diseases, Stars, Spitzer Space Telescope, Space and Planetary Science, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Small Magellanic Cloud, Tidal tail, Caltech Library Services, Astrophysics::Galaxy Astrophysics
Abstract: The Tail region of the Small Magellanic Cloud (SMC) was imaged using the MIPS instrument on the Spitzer Space Telescope as part of the SAGE-SMC Spitzer Legacy. Diffuse infrared emission from dust was detected in all the MIPS bands. The Tail gas-to-dust ratio was measured to be 1200 +/- 350 using the MIPS observations combined with existing IRAS and HI observations. This gas-to-dust ratio is higher than the expected 500-800 from the known Tail metallicity indicating possible destruction of dust grains. Two cluster regions in the Tail were resolved into multiple sources in the MIPS observations and local gas-to-dust ratios were measured to be ~440 and ~250 suggests dust formation and/or significant amounts of ionized gas in these regions. These results support the interpretation that the SMC Tail is a tidal tail recently stripped from the SMC that includes gas, dust, and young stars., 6 pages, 3 figures, ApJ Letters, in press, (version with full resolution figures at http://www.stsci.edu/~kgordon/papers/PS_files/sage-smc_taildust_v1.62.pdf)
Published: 2008

42. Early results from the SAGE-SMC Spitzer legacy

Author: E. Muller, A. Li, A. Kawamura, Karl D. Gordon, Maureen O. Meade, K. M. Sandstrom, Linda J. Smith, U. Vijh, J. Th. van Loon, Alberto D. Bolatto, S. Hony, F. Markwick-Kemper, K. Olsen, Jason Harris, J. D. Simon, R. D. Blum, R. Paladini, Dennis Zaritsky, Margaret Meixner, Y. Fukui, K. A. Misselt, A. K. Leroy, D. Paradis, E. Churchwell, R. Indebetouw, C. Bot, B. A. Whitney, H. Shibai, S. Madden, Geoffrey C. Clayton, N. Mizuno, Alexander G. G. M. Tielens, J.-P. Bernard, B. L. Babler, T. Robitaille, D. Rubin, J. L. Hora, S. Points, S. Srinivasan, S. D. Van Dyk, M. Block, F. Israel, Marta Sewilo, Kevin Volk, William T. Reach, L. Carlson, V. Gorjian, M. Cohen, S. Sato, Toshikazu Onishi, C. W. Engelbracht, S. Bracker, A. R. Marble, A. Mizuno, and J. M. Oliveira
Subjects: Physics, Luminous infrared galaxy, Infrared, Astronomy, Astronomy and Astrophysics, Astrophysics, Tail region, Hubble sequence, symbols.namesake, Early results, Space and Planetary Science, Galaxy formation and evolution, symbols, Small Magellanic Cloud, Dust emission
Abstract: Early results from the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the tidally-disrupted, low-metallicity Small Magellanic Cloud) Spitzer legacy program are presented. These early results concentrate on the SAGE-SMC MIPS observations of the SMC Tail region. This region is the high H i column density portion of the Magellanic Bridge adjacent to the SMC Wing. We detect infrared dust emission and measure the gas-to-dust ratio in the SMC Tail and find it similar to that of the SMC Body. In addition, we find two embedded cluster regions that are resolved into multiple sources at all MIPS wavelengths.
Published: 2008

43. SPITZERSAGE SURVEY OF THE LARGE MAGELLANIC CLOUD. III. STAR FORMATION AND ∼1000 NEW CANDIDATE YOUNG STELLAR OBJECTS

Author: Michael W. Werner, Jay A. Frogel, William T. Reach, Linda J. Smith, Alexander G. G. M. Tielens, Kevin Volk, S. D. Van Dyk, Brian Babler, Ed Churchwell, Karl D. Gordon, Hiroshi Shibai, Francisca Kemper, Nino Panagia, Dennis Zaritsky, Joseph L. Hora, Karl Misselt, J. R. Mould, Lister Staveley-Smith, Miwa Block, Akira Mizuno, Francois Boulanger, B. A. Whitney, Roberta Paladini, U. Vijh, J.-P. Bernard, Varoujan Gorjian, Akiko Kawamura, S. C. Madden, Remy Indebetouw, Thomas P. Robitaille, J. C. Gallagher, Pablo G. Pérez-González, Matthew S. Povich, S. Bracker, Sundar Srinivasan, Yasuo Fukui, Toshikazu Onishi, M. J. Wolff, Claus Leitherer, William B. Latter, Bi-Qing For, K. A. G. Olsen, Jason Harris, Toshiya Ueta, Marvin L. Cohen, Susumu Sato, Norikazu Mizuno, Marta Sewilo, Antonella Nota, Margaret Meixner, D. M. Kelly, M. S. Oey, Robert Blum, Marilyn R. Meade, and Charles W. Engelbracht
Subjects: Physics, Initial mass function, Star formation, Young stellar object, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Luminosity, Stars, Spitzer Space Telescope, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics
Abstract: We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations. The YSOs are biased toward intermediate- to high-mass and young evolutionary stages, because these overlap less with galaxies and evolved stars in color-magnitude space. The YSOs are highly correlated spatially with atomic and molecular gas, and are preferentially located in the shells and bubbles created by massive stars inside. They are more clustered than generic point sources, as expected if star formation occurs in filamentary clouds or shells. We applied a more stringent color-magnitude selection to produce a subset of "high-probability" YSO candidates. We fitted the spectral-energy distributions (SEDs) of this subset and derived physical properties for those that were well fitted. The total mass of these well-fitted YSOs is ~2900 M_☉ and the total luminosity is ~2.1 × 10^6 L_☉ . By extrapolating the mass function with a standard initial mass function and integrating, we calculate a current star-formation rate of ~0.06 M_☉ yr^(–1), which is at the low end of estimates based on total ultraviolet and IR flux from the galaxy (~0.05 – 0.25 M_☉ yr^(–1)), consistent with the expectation that our current YSO list is incomplete. Follow-up spectroscopy and further data mining will better separate the different IR-bright populations and likely increase the estimated number of YSOs. The full YSO list is available as electronic tables, and the SEDs are available as an electronic figure for further use by the scientific community.
Published: 2008

44. Extinction and dust/gas ratio in LMC molecular clouds

Author: William T. Reach, Annie Hughes, D. Paradis, J.-P. Bernard, Kazuhito Dobashi, and Akiko Kawamura
Subjects: Physics, Molecular cloud, Extinction (astronomy), Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spatial distribution, Galaxy, Virial theorem, Wavelength, Stars, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics
Abstract: Aims. The goal of this paper is to measure the dust content and distribution in the Large Magellanic Cloud (LMC) by comparing extinction maps produced in the near-infrared wavelengths and the spatial distribution of the neutral and molecular gas, as traced by Hi and CO observations. Methods. In order to derive an extinction map of the LMC, we have developed a new method to measure the color excess of dark clouds, using the 2MASS all-sky survey. Classical methods to measure the color excess (including the NICE method) tend to underestimate the true color excess if the clouds are significantly contaminated by unreddened foreground stars, as is the case in the LMC. We propose a new method that uses the color of the X percentile reddest stars and which is robust against such contamination. Using this method, it is possible to infer the positions of dark clouds with respect to the star distribution by comparing the observed color excess as a function of the percentile used and that predicted by a model. Results. On the basis of the resulting extinction map, we perform a correlation analysis for a set of dark molecular clouds. Assuming similar infrared absorption properties for the dust in the neutral and molecular phases, we derive the absorption-to-column density ratio AV/NH and the CO-to-H2 conversion factor X_(CO). We show that AV/NH increases from the outskirts of the LMC towards the 30 Dor star-forming region. This can be explained either by a systematic increase of the dust abundance, or by the presence of an additional gas component not traced by Hi or CO, but strongly correlated to the Hi distribution. If dust abundance is allowed to vary, the derived X_(CO) factors for the selected regions are several times lower than those derived from a virial analysis of the CO data. This could indicate that molecular clouds in the LMC are not gravitationally bound, or that they are bounded by substantial external pressure. However, the X_(CO) values derived from absorption can be reconciled with the virial results assuming a constant value for the dust abundance and the existence of an additional, unseen gas component. These results are in agreement with those derived for the LMC from diffuse far-infrared emission.
Published: 2008

45. First-trimester ultrasound examination and the outcome of monochorionic twin pregnancies

Author: M. Nassar, J. P. Bernard, Yves Ville, B. Nasr, and A. Y. El Kateb
Subjects: medicine.medical_specialty, Twins, Crown-Rump Length, Ultrasonography, Prenatal, Pregnancy, Nuchal Translucency Measurement, medicine, Humans, Neonatology, Genetics (clinical), Twin Pregnancy, Retrospective Studies, Gynecology, Crown-rump length, Obstetrics, business.industry, Incidence, Obstetrics and Gynecology, Gestational age, Chorion, Fetofetal Transfusion, medicine.disease, Pregnancy Trimester, First, Gestation, Female, France, Monochorionic twins, business
Abstract: Objective To refine the incidence of abnormal first-trimester ultrasound measurements and their correlation with the outcome of monochorionic diamniotic pregnancies. Methods First-trimester crown–rump length (CRL) and nuchal translucency thickness (NT) measurements were studied in three subgroups of a total of 200 monochorionic twin gestations referred to our center between June 2002 and February 2006. Intertwin CRL discordance was defined as > 10% and the 95th percentile of NT thickness for gestational age was used. The first group of 103 consecutive unselected monochorionic diamniotic twin pregnancies was prospectively followed up from 11–14 weeks onwards, throughout the pregnancy. The second group of 136 nonconsecutive monochorionic diamniotic twin pregnancies including 64 that developed TTTS was studied retrospectively. The third group of 100 consecutive cases of TTTS studied retrospectively for the correlation between first trimester measurements and staging and timing of occurrence of TTTS. Results In group 1, the incidence of TTTS was 5 in 103 (5%, 95CI [0.7–9]). Large intertwin CRL discordance and increased NT were correlated with perinatal death. In group 2, no significant association was found between first-trimester parameters and the development of TTTS but discordance in early second trimester biometry and Doppler were. In group three, a positive correlation was found between the intertwin discordance in CRL and early occurrence of TTTS before 20 weeks of gestation (p = 0.02). Conclusion Monochorionic twin gestations who ultimately develop TTTS may exhibit intertwin difference in growth as early as 11–14 weeks of gestation. The earlier the discordance the earlier the development of the disease. Copyright © 2007 John Wiley & Sons, Ltd.
Published: 2007

46. Pancréatite médicamenteuse

Author: L. Heyries, J.-P. Bernard, A. Guillin-Poujol, and J. Sahel
Published: 2007

47. Planck intermediate results X. Physics of the hot gas in the Coma cluster

Author: Nabila Aghanim, Jacques Delabrouille, Peter A. R. Ade, Amedeo Balbi, Fabio Finelli, James G. Bartlett, A. de Rosa, Ricardo Genova-Santos, W. C. Jones, Allan Hornstrup, Etienne Pointecouteau, R. Leonardi, T. Riller, Monique Arnaud, S. R. Hildebrandt, Pasquale Mazzotta, C. Renault, R. B. Barreiro, J. Knoche, Simon Prunet, F. Cuttaia, Gayoung Chon, Mika Juvela, Rashmikant V. Sudiwala, J. González-Nuevo, O. Perdereau, Anna Bonaldi, Lloyd Knox, Carlo Burigana, Davide Maino, X. Dupac, C. Hernández-Monteagudo, I. F. Bikmaev, Niraj Welikala, Marc-Antoine Miville-Deschênes, T. R. Jaffe, L. P. L. Colombo, Dmitry Novikov, Hans Ulrik Nørgaard-Nielsen, Marc Türler, Pavel Naselsky, R. J. Davis, L. Popa, Jean-Baptiste Melin, J. A. Murphy, M. Reinecke, George F. Smoot, F. Noviello, K. Ganga, J. Tuovinen, B. Van Tent, Simona Mei, L. A. Wade, Daniela Paoletti, Jussi Varis, Andrea Zonca, A. J. Banday, Klaus Dolag, L. Montier, A. Gregorio, Krzysztof M. Gorski, Jose M. Diego, M. Giard, K. Benabed, J.-L. Puget, Michael L. Brown, P. R. Christensen, Luca Terenzi, B. P. Crill, Lung-Yih Chiang, Dipak Munshi, J. R. Bond, Francesca Perrotta, G. de Gasperis, T. Jagemann, D. Yvon, Olivier Doré, E. Franceschi, Martin Kunz, H. K. Eriksen, M. Sandri, Mathieu Remazeilles, Torsten A. Enßlin, L. Toffolatti, Shea Brown, W. Hovest, U. Dörl, Håkon Dahle, E. Battaner, Rafael Rebolo, J.-P. Bernard, Anthony Lasenby, Charles R. Lawrence, E. Martínez-González, E. Keihänen, Matthieu Roman, R. Kneissl, Bruno Maffei, Saleem Zaroubi, Benjamin D. Wandelt, Julian Borrill, F. Piacentini, Nicola Vittorio, M. Frommert, G. W. Pratt, M. Piat, Gianluca Morgante, R. Piffaretti, Clive Dickinson, M. Le Jeune, I. Flores-Cacho, Alain Benoit, Simon D. M. White, L. Mendes, Sabino Matarrese, F.-X. Désert, Anne Lähteenmäki, G. Umana, A. Da Silva, F. Atrio-Barandela, Mariachiara Rossetti, S. Ricciardi, R. A. Burenin, J. Démoclès, Andrea Zacchei, S. Galeotta, Sophie Henrot-Versille, P. B. Lilje, Rashid Sunyaev, E. M. Churazov, B. M. Schaefer, Jörg P. Rachen, A. Coulais, Paolo Natoli, Olivier Forni, F. Matthai, Jose Alberto Rubino-Martin, F. K. Hansen, G. de Zotti, M. Ashdown, Paolo Cabella, E. Pierpaoli, Douglas Scott, W. Holmes, M. Tristram, G. Polenta, M. Linden-Vørnle, P. Carvalho, D. L. Harrison, T. Poutanen, M. Maris, Alessandro Melchiorri, Ben Rusholme, Hervé Bourdin, A. Moneti, N. Mandolesi, François R. Bouchet, Philip Lubin, L. Cayón, J. F. Macías-Pérez, Irek Khamitov, Graca Rocha, Marian Douspis, G. Hurier, Hans Böhringer, Kevin M. Huffenberger, Francine R. Marleau, Fabrizio Villa, Silvia Masi, M. Frailis, Carlo Baccigalupi, E. Hivon, J.-F. Sygnet, Lawrence Rudnick, Luca Valenziano, A. Mennella, D. Sutton, F. Stivoli, Nicolas Ponthieu, S. Donzelli, Luigi Danese, Marat Gilfanov, Alessandro Gruppuso, Giorgio Savini, A. Catalano, J.-M. Lamarre, S. Osborne, Michael P. Hobson, Hannu Kurki-Suonio, F. Pajot, David L. Clements, I. Ristorcelli, H. Dole, Subhabrata Mitra, J. A. Tauber, M. Tomasi, Marco Bersanelli, J.-F. Cardoso, Stéphane Plaszczynski, Guilaine Lagache, M. López-Caniego, P. de Bernardis, C. Rosset, J. Aumont, P. Vielva, Marcella Massardi, I. D. Novikov, A.-S. Suur-Uski, Sergio Colafrancesco, 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 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-Saclay-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), 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), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), 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 Traitement et Communication de l'Information (LTCI), Institut Mines-Télécom [Paris] (IMT)-Télécom Paris, 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, 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), 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 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Paris Diderot, Sorbonne Paris Cité, Paris, France, Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-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 Joseph Fourier - Grenoble 1 (UJF)-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), 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), Université Paris-Sud - Paris 11 (UP11), Planck Collaboration, Department of Physics, Helsinki Institute of Physics, University of Minnesota, 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7), Hélium : du fondamental aux applications [2007-2015] (HELFA [2007-2015]), Institut Néel [2007-2015] (NEEL [2007-2015]), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), 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), 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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PLANCK, Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, Astronomy, APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, P. A. R., Ade, N., Aghanim, M., Arnaud, M., Ashdown, F., Atrio Barandela, J., Aumont, C., Baccigalupi, A., Balbi, A. J., Banday, R. B., Barreiro, J. G., Bartlett, E., Battaner, K., Benabed, A., Benoît, J. P., Bernard, M., Bersanelli, I., Bikmaev, H., Böhringer, A., Bonaldi, J. R., Bond, J., Borrill, F. R., Bouchet, H., Bourdin, M. L., Brown, S. D., Brown, R., Burenin, C., Burigana, P., Cabella, J. F., Cardoso, P., Carvalho, A., Catalano, L., Cayón, L. Y., Chiang, G., Chon, P. R., Christensen, E., Churazov, D. L., Clement, S., Colafrancesco, L. P. L., Colombo, A., Coulai, B. P., Crill, F., Cuttaia, A., Da Silva, H., Dahle, L., Danese, R. J., Davi, P., de Bernardi, G., de Gasperi, A., de Rosa, G., de Zotti, J., Delabrouille, J., Démoclè, F. X., Désert, C., Dickinson, J. M., Diego, K., Dolag, H., Dole, S., Donzelli, O., Doré, U., Dörl, M., Douspi, X., Dupac, T. A., Enßlin, H. K., Eriksen, F., Finelli, I., Flores Cacho, O., Forni, M., Fraili, E., Franceschi, M., Frommert, S., Galeotta, K., Ganga, R. T., Génova Santo, M., Giard, M., Gilfanov, J., González Nuevo, K. M., Górski, Gregorio, Anna, A., Gruppuso, F. K., Hansen, D., Harrison, S., Henrot Versillé, C., Hernández Monteagudo, S. R., Hildebrandt, E., Hivon, M., Hobson, W. A., Holme, A., Hornstrup, W., Hovest, K. M., Huffenberger, G., Hurier, T. R., Jaffe, T., Jagemann, W. C., Jone, M., Juvela, E., Keihänen, I., Khamitov, R., Kneissl, J., Knoche, L., Knox, M., Kunz, H., Kurki Suonio, G., Lagache, A., Lähteenmäki, J. M., Lamarre, A., Lasenby, C. R., Lawrence, M., Le Jeune, R., Leonardi, P. B., Lilje, M., Linden Vørnle, M., López Caniego, P. M., Lubin, J. F., Macías Pérez, B., Maffei, D., Maino, N., Mandolesi, M., Mari, F., Marleau, E., Martínez González, S., Masi, M., Massardi, S., Matarrese, F., Matthai, P., Mazzotta, S., Mei, A., Melchiorri, J. B., Melin, L., Mende, A., Mennella, S., Mitra, M. A., Miville Deschêne, A., Moneti, L., Montier, G., Morgante, D., Munshi, J. A., Murphy, P., Naselsky, P., Natoli, H. U., Nørgaard Nielsen, F., Noviello, D., Novikov, I., Novikov, S., Osborne, F., Pajot, D., Paoletti, O., Perdereau, F., Perrotta, F., Piacentini, M., Piat, E., Pierpaoli, R., Piffaretti, S., Plaszczynski, E., Pointecouteau, G., Polenta, N., Ponthieu, L., Popa, T., Poutanen, G. W., Pratt, S., Prunet, J. L., Puget, J. P., Rachen, R., Rebolo, M., Reinecke, M., Remazeille, C., Renault, S., Ricciardi, T., Riller, I., Ristorcelli, G., Rocha, M., Roman, C., Rosset, M., Rossetti, J. A., Rubiño Martín, L., Rudnick, B., Rusholme, M., Sandri, G., Savini, B. M., Schaefer, D., Scott, G. F., Smoot, F., Stivoli, R., Sudiwala, R., Sunyaev, D., Sutton, A. S., Suur Uski, J. F., Sygnet, J. A., Tauber, L., Terenzi, L., Toffolatti, M., Tomasi, M., Tristram, J., Tuovinen, M., Türler, G., Umana, L., Valenziano, B., Van Tent, J., Vari, P., Vielva, F., Villa, N., Vittorio, L. A., Wade, B. D., Wandelt, N., Welikala, S. D. M., White, D., Yvon, A., Zacchei, S., Zaroubi, A., Zonca, 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), 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Hélium : du fondamental aux applications (NEEL - HELFA), 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), École normale supérieure - Paris (ENS-PSL), 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), 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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-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 Joseph Fourier - Grenoble 1 (UJF)-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)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Shock wave, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Coma (optics), galaxies: clusters: individual: Coma cluster, Astrophysics, cosmic background radiation, 01 natural sciences, ROSAT, clusters: general [galaxies], 010303 astronomy & astrophysics, Physics, Shock (fluid dynamics), TEMPERATURE STRUCTURE, MAGNETIC-FIELD, Radius, observations [cosmology], galaxies: cluster [X-rays], SHOCK-WAVES, Cosmic background radiation, Cosmology: observations, Galaxies: clusters: general, Galaxies: clusters: individual: Coma cluster, Galaxies: clusters: intracluster medium, X-rays: galaxies: clusters, clusters: intracluster medium [galaxies], galaxies: clusters: general, ALL-SKY SURVEY, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, astro-ph.CO, galaxies: clusters: intracluster medium, cosmology: observations, LAL 13-71, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, clusters: individual: Coma cluster [galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], SIMULATED GALAXY CLUSTERS, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, RADIO HALOS, 0103 physical sciences, LARGE-SCALE STRUCTURE, Coma Cluster, Cluster (physics), PRE-LAUNCH STATUS, Planck, Astrophysics::Galaxy Astrophysics, XMM-NEWTON, 010308 nuclear & particles physics, Astronomy and Astrophysics, 115 Astronomy, Space science, Space and Planetary Science, galaxies: clusters: individual: coma cluster, x-rays: galaxies: clusters, galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SUNYAEV-ZELDOVICH
Abstract: We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r ≈ 3 × R500. We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) “universal” pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R500; by r = 2 × R500 it underestimates the observed y profile by a factor of ≃2. This may indicate that at these larger radii either: i) the cluster SZ emission is contaminated by unresolved SZ sources along the line of sight; or ii) the pressure profile of Coma is higher at r > R500 than the mean pressure profile predicted by the simulations used to constrain the models. The Planck image shows significant local steepening of the y profile in two regions about half a degree to the west and to the south-east of the cluster centre. These features are consistent with the presence of shock fronts at these radii, and indeed the western feature was previously noticed in the ROSAT PSPC mosaic as well as in the radio. Using Plancky profiles extracted from corresponding sectors we find pressure jumps of 4.9-0.2+0.4 and 5.0-0.1+1.3 in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number Mw = 2.03-0.04+0.09 and Mse = 2.05-0.02+0.25 in the west and south-east, respectively. Finally, we find that the y and radio-synchrotron signals are quasi-linearly correlated on Mpc scales, with small intrinsic scatter. This implies either that the energy density of cosmic-ray electrons is relatively constant throughout the cluster, or that the magnetic fields fall off much more slowly with radius than previously thought., 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, MICINN and JA (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 DEISA (EU). Partial support for this work for L. Rudnick comes from U.S. NSF Grant 09-08668 to the University of Minnesota.
Published: 2013

48. [First trimester screening for Down syndrome at Prima facie. A 6-year survey]

Author: P, Roth, J-P, Bernard, V, Meyer, M-P, Beaujard, L-J, Salomon, and Y, Ville
Subjects: Adult, Karyotype, Prenatal Care, Sensitivity and Specificity, Ultrasonography, Prenatal, Pregnancy Trimester, First, Pregnancy, Risk Factors, Prenatal Diagnosis, Humans, Pregnancy-Associated Plasma Protein-A, Chorionic Gonadotropin, beta Subunit, Human, False Positive Reactions, Female, Down Syndrome, Nuchal Translucency Measurement, Biomarkers, Maternal Age
Abstract: To evaluate the results of screening for trisomy 21 by the combined risk of first trimester (as defined by the decree of June 23, 2009) in the Prima facie structure.Single center study involving all patients that were seen for first trimester screening at Prima facie with singleton living pregnancy, not obtained by embryo donation, between 1 January 2009 and 31 December 2014.Eighteen thousand two hundred and fifty-one patients were included, of which underwent screening for trisomy 21 by the combined risk. One thousand and forty-six (6.1%) had a calculated risk higher than 1/250. Seventy-five were affected by trisomy 21, of whom 65 in the high risk group. The sensitivity and specificity of screening are 86.7% and 94.4%. The median nuchal translucency was 0.98 MoM.Screening for trisomy 21 by calculating the combined risk of first trimester enabled to detect 86.7% of trisomy 21 with a false positive rate of 5.6%.
Published: 2015

49. Planck Intermediate Results. IV. The XMM-Newton validation programme for new Planck clusters

Author: P. A. R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, J. Aumont, C. Baccigalupi, A. Balbi, A. J. Banday, R. B. Barreiro, J. G. Bartlett, E. Battaner, K. Benabed, A. Benoît, J. P. Bernard, M. Bersanelli, I. Bikmaev, H. Böhringer, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, M. L. Brown, C. Burigana, R. C. Butler, P. Cabella, P. Carvalho, A. Catalano, L. Cayón, A. Chamballu, R. R. Chary, L. Y. Chiang, G. Chon, P. R. Christensen, D. L. Clements, S. Colafrancesco, S. Colombi, A. Coulais, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, R. J. Davis, P. de Bernardis, G. de Gasperis, G. de Zotti, J. Delabrouille, J. Démoclès, F. X. Désert, J. M. Diego, K. Dolag, H. Dole, S. Donzelli, O. Doré, M. Douspis, X. Dupac, T. A. Enßlin, H. K. Eriksen, F. Finelli, I. Flores Cacho, O. Forni, M. Frailis, E. Franceschi, M. Frommert, S. Galeotta, K. Ganga, R. T. Génova Santos, Y. Giraud Héraud, J. González Nuevo, R. González Riestra, K. M. Górski, A. Gruppuso, F. K. Hansen, D. Harrison, A. Hempel, S. Henrot Versillé, C. Hernández Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, A. Hornstrup, W. Hovest, K. M. Huffenberger, G. Hurier, A. H. Jaffe, T. Jagemann, W. C. Jones, M. Juvela, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki Suonio, G. Lagache, J. M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune, S. Leach, R. Leonardi, A. Liddle, P. B. Lilje, M. Linden Vørnle, M. López Caniego, G. Luzzi, J. F. Macías Pérez, D. Maino, N. Mandolesi, R. Mann, M. Maris, F. Marleau, D. J. Marshall, E. Martínez González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, S. Mei, P. R. Meinhold, A. Melchiorri, J. B. Melin, L. Mendes, A. Mennella, S. Mitra, M. A. Miville Deschênes, A. Moneti, G. Morgante, D. Mortlock, D. Munshi, P. Naselsky, F. Nati, P. Natoli, H. U. Nørgaard Nielsen, F. Noviello, S. Osborne, F. Pajot, D. Paoletti, O. Perdereau, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, R. Piffaretti, S. Plaszczynski, P. Platania, E. Pointecouteau, G. Polenta, L. Popa, T. Poutanen, G. W. Pratt, S. Prunet, J. L. Puget, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, G. Rocha, C. Rosset, M. Rossetti, J. A. Rubiño Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, G. F. Smoot, A. Stanford, F. Stivoli, R. Sudiwala, R. Sunyaev, D. Sutton, A. S. Suur Uski, J. F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, N. Welikala, J. Weller, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca, BORGANI, STEFANO, GREGORIO, ANNA, P. A. R., Ade, N., Aghanim, M., Arnaud, M., Ashdown, J., Aumont, C., Baccigalupi, A., Balbi, A. J., Banday, R. B., Barreiro, J. G., Bartlett, E., Battaner, K., Benabed, A., Benoît, J. P., Bernard, M., Bersanelli, I., Bikmaev, H., Böhringer, A., Bonaldi, J. R., Bond, Borgani, Stefano, J., Borrill, F. R., Bouchet, M. L., Brown, C., Burigana, R. C., Butler, P., Cabella, P., Carvalho, A., Catalano, L., Cayón, A., Chamballu, R. R., Chary, L. Y., Chiang, G., Chon, P. R., Christensen, D. L., Clement, S., Colafrancesco, S., Colombi, A., Coulai, B. P., Crill, F., Cuttaia, A., Da Silva, H., Dahle, R. J., Davi, P., de Bernardi, G., de Gasperi, G., de Zotti, J., Delabrouille, J., Démoclè, F. X., Désert, J. M., Diego, K., Dolag, H., Dole, S., Donzelli, O., Doré, M., Douspi, X., Dupac, T. A., Enßlin, H. K., Eriksen, F., Finelli, I., Flores Cacho, O., Forni, M., Fraili, E., Franceschi, M., Frommert, S., Galeotta, K., Ganga, R. T., Génova Santo, Y., Giraud Héraud, J., González Nuevo, R., González Riestra, K. M., Górski, Gregorio, Anna, A., Gruppuso, F. K., Hansen, D., Harrison, A., Hempel, S., Henrot Versillé, C., Hernández Monteagudo, D., Herranz, S. R., Hildebrandt, E., Hivon, M., Hobson, W. A., Holme, A., Hornstrup, W., Hovest, K. M., Huffenberger, G., Hurier, A. H., Jaffe, T., Jagemann, W. C., Jone, M., Juvela, R., Kneissl, J., Knoche, L., Knox, M., Kunz, H., Kurki Suonio, G., Lagache, J. M., Lamarre, A., Lasenby, C. R., Lawrence, M., Le Jeune, S., Leach, R., Leonardi, A., Liddle, P. B., Lilje, M., Linden Vørnle, M., López Caniego, G., Luzzi, J. F., Macías Pérez, D., Maino, N., Mandolesi, R., Mann, M., Mari, F., Marleau, D. J., Marshall, E., Martínez González, S., Masi, M., Massardi, S., Matarrese, P., Mazzotta, S., Mei, P. R., Meinhold, A., Melchiorri, J. B., Melin, L., Mende, A., Mennella, S., Mitra, M. A., Miville Deschêne, A., Moneti, G., Morgante, D., Mortlock, D., Munshi, P., Naselsky, F., Nati, P., Natoli, H. U., Nørgaard Nielsen, F., Noviello, S., Osborne, F., Pajot, D., Paoletti, O., Perdereau, F., Perrotta, F., Piacentini, M., Piat, E., Pierpaoli, R., Piffaretti, S., Plaszczynski, P., Platania, E., Pointecouteau, G., Polenta, L., Popa, T., Poutanen, G. W., Pratt, S., Prunet, J. L., Puget, M., Reinecke, M., Remazeille, C., Renault, S., Ricciardi, G., Rocha, C., Rosset, M., Rossetti, J. A., Rubiño Martín, B., Rusholme, M., Sandri, G., Savini, D., Scott, G. F., Smoot, A., Stanford, F., Stivoli, R., Sudiwala, R., Sunyaev, D., Sutton, A. S., Suur Uski, J. F., Sygnet, J. A., Tauber, L., Terenzi, L., Toffolatti, M., Tomasi, M., Tristram, L., Valenziano, B., Van Tent, P., Vielva, F., Villa, N., Vittorio, L. A., Wade, B. D., Wandelt, N., Welikala, J., Weller, S. D. M., White, D., Yvon, A., Zacchei, and A., Zonca
Subjects: galaxies: clusters: intracluster medium, clusters: intracluster medium [galaxies], galaxies: clusters: general, cosmology: observations, X-rays: galaxies: clusters, clusters: general [galaxies], galaxies: clusters [X-rays], cosmic background radiation, observation [cosmology]
Abstract: We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. Fourteen new clusters were detected by XMM-Newton, ten single clusters and two double systems. Redshifts from X-ray spectroscopy lie in the range 0.2 to 0.9, with six clusters at z > 0.5. Estimated masses (M500) range from 2.5 × 1014 to 8 × 1014 M⊙. We discuss our results in the context of the full XMM-Newton validation programme, in which 51 new clusters have been detected. This includes four double and two triple systems, some of which are chance projections on the sky of clusters at different redshifts. We find thatassociation with a source from the RASS-Bright Source Catalogue is a robust indicator of the reliability of a candidate, whereas association with a source from the RASS-Faint Source Catalogue does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2σ being a good indication that the candidate is a real cluster. Candidate validation from association with SDSS galaxy overdensity at z > 0.5 is also discussed. The full sample gives a Planck sensitivity threshold of Y500 ~ 4 × 10-4 arcmin2, with indication for Malmquist bias in the YX-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 M⊙ at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. In particular, there is no significant evolution of the YX / Y500 ratio.
Published: 2013

50. Planckintermediate results(Corrigendum)

Author: P. A. R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, F. Atrio Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A. J. Banday, R. B. Barreiro, J. G. Bartlett, E. Battaner, K. Benabed, A. Benoît, J. P. Bernard, M. Bersanelli, R. Bhatia, I. Bikmaev, J. Bobin, H. Böhringer, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, H. Bourdin, M. L. Brown, R. Burenin, C. Burigana, P. Cabella, J. F. Cardoso, P. Carvalho, G. Castex, A. Catalano, L. Cayón, A. Chamballu, L. Y. Chiang, G. Chon, P. R. Christensen, E. Churazov, D. L. Clements, S. Colafrancesco, S. Colombi, L. P. L. Colombo, B. Comis, A. Coulais, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, L. Danese, R. J. Davis, P. de Bernardis, G. de Gasperis, G. de Zotti, J. Delabrouille, J. Démoclès, F. X. Désert, J. M. Diego, K. Dolag, H. Dole, S. Donzelli, O. Doré, U. Dörl, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, I. Flores Cacho, O. Forni, P. Fosalba, M. Frailis, E. Franceschi, M. Frommert, S. Galeotta, K. Ganga, R. T. Génova Santos, M. Giard, Y. Giraud Héraud, J. González Nuevo, K. M. Górski, GREGORIO, ANNA, A. Gruppuso, F. K. Hansen, D. Harrison, A. Hempel, S. Henrot Versillé, C. Hernández Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, G. Hurier, T. R. Jaffe, A. H. Jaffe, T. Jagemann, W. C. Jones, M. Juvela, E. Keihänen, I. Khamitov, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki Suonio, G. Lagache, A. Lähteenmäki, J. M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune, R. Leonardi, A. Liddle, P. B. Lilje, M. López Caniego, G. Luzzi, J. F. Macías Pérez, D. Maino, N. Mandolesi, M. Maris, F. Marleau, D. J. Marshall, E. Martínez González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, S. Mei, A. Melchiorri, J. B. Melin, L. Mendes, A. Mennella, S. Mitra, M. A. Miville Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, H. U. Nørgaard Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, F. Pajot, D. Paoletti, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, R. Piffaretti, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, S. Prunet, J. L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, M. Roman, C. Rosset, M. Rossetti, J. A. Rubiño Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, G. F. Smoot, J. L. Starck, R. Sudiwala, R. Sunyaev, D. Sutton, A. S. Suur Uski, J. F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, J. Tuovinen, L. Valenziano, B. Van Tent, J. Varis, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, N. Welikala, S. D. M. White, M. White, D. Yvon, A. Zacchei, A. Zonca, BORGANI, STEFANO, P. A. R., Ade, N., Aghanim, M., Arnaud, M., Ashdown, F., Atrio Barandela, J., Aumont, C., Baccigalupi, A., Balbi, A. J., Banday, R. B., Barreiro, J. G., Bartlett, E., Battaner, K., Benabed, A., Benoît, J. P., Bernard, M., Bersanelli, R., Bhatia, I., Bikmaev, J., Bobin, H., Böhringer, A., Bonaldi, J. R., Bond, Borgani, Stefano, J., Borrill, F. R., Bouchet, H., Bourdin, M. L., Brown, R., Burenin, C., Burigana, P., Cabella, J. F., Cardoso, P., Carvalho, G., Castex, A., Catalano, L., Cayón, A., Chamballu, L. Y., Chiang, G., Chon, P. R., Christensen, E., Churazov, D. L., Clement, S., Colafrancesco, S., Colombi, L. P. L., Colombo, B., Comi, A., Coulai, B. P., Crill, F., Cuttaia, A., Da Silva, H., Dahle, L., Danese, R. J., Davi, P., de Bernardi, G., de Gasperi, G., de Zotti, J., Delabrouille, J., Démoclè, F. X., Désert, J. M., Diego, K., Dolag, H., Dole, S., Donzelli, O., Doré, U., Dörl, M., Douspi, X., Dupac, G., Efstathiou, T. A., Enßlin, H. K., Eriksen, F., Finelli, I., Flores Cacho, O., Forni, P., Fosalba, M., Fraili, E., Franceschi, M., Frommert, S., Galeotta, K., Ganga, R. T., Génova Santo, M., Giard, Y., Giraud Héraud, J., González Nuevo, K. M., Górski, Gregorio, Anna, A., Gruppuso, F. K., Hansen, D., Harrison, A., Hempel, S., Henrot Versillé, C., Hernández Monteagudo, D., Herranz, S. R., Hildebrandt, E., Hivon, M., Hobson, W. A., Holme, G., Hurier, T. R., Jaffe, A. H., Jaffe, T., Jagemann, W. C., Jone, M., Juvela, E., Keihänen, I., Khamitov, T. S., Kisner, R., Kneissl, J., Knoche, L., Knox, M., Kunz, H., Kurki Suonio, G., Lagache, A., Lähteenmäki, J. M., Lamarre, A., Lasenby, C. R., Lawrence, M., Le Jeune, R., Leonardi, A., Liddle, P. B., Lilje, M., López Caniego, G., Luzzi, J. F., Macías Pérez, D., Maino, N., Mandolesi, M., Mari, F., Marleau, D. J., Marshall, E., Martínez González, S., Masi, M., Massardi, S., Matarrese, P., Mazzotta, S., Mei, A., Melchiorri, J. B., Melin, L., Mende, A., Mennella, S., Mitra, M. A., Miville Deschêne, A., Moneti, L., Montier, G., Morgante, D., Mortlock, D., Munshi, J. A., Murphy, P., Naselsky, F., Nati, P., Natoli, H. U., Nørgaard Nielsen, F., Noviello, D., Novikov, I., Novikov, S., Osborne, F., Pajot, D., Paoletti, F., Pasian, G., Patanchon, O., Perdereau, L., Perotto, F., Perrotta, F., Piacentini, M., Piat, E., Pierpaoli, R., Piffaretti, S., Plaszczynski, E., Pointecouteau, G., Polenta, N., Ponthieu, L., Popa, T., Poutanen, G. W., Pratt, S., Prunet, J. L., Puget, J. P., Rachen, W. T., Reach, R., Rebolo, M., Reinecke, M., Remazeille, C., Renault, S., Ricciardi, T., Riller, I., Ristorcelli, G., Rocha, M., Roman, C., Rosset, M., Rossetti, J. A., Rubiño Martín, B., Rusholme, M., Sandri, G., Savini, D., Scott, G. F., Smoot, J. L., Starck, R., Sudiwala, R., Sunyaev, D., Sutton, A. S., Suur Uski, J. F., Sygnet, J. A., Tauber, L., Terenzi, L., Toffolatti, M., Tomasi, M., Tristram, J., Tuovinen, L., Valenziano, B., Van Tent, J., Vari, P., Vielva, F., Villa, N., Vittorio, L. A., Wade, B. D., Wandelt, N., Welikala, S. D. M., White, M., White, D., Yvon, A., Zacchei, and A., Zonca
Subjects: galaxies: clusters: intracluster medium, clusters: intracluster medium [galaxies], galaxies: clusters: general, general [X-rays], cosmology: observations, clusters: general [galaxies], submillimeter: general, general [submillimeter], X-rays: general, errata, addenda, observation [cosmology]
Published: 2013

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Region

Database

Publisher

451 results on '"J.-P. Bernard"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources