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1. Accurate CMB covariance matrices: exact calculation and approximations

Author: Étienne Camphuis, Karim Benabed, Silvia Galli, Eric Hivon, and Marc Lilley
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Accurate covariance matrices are required for a reliable estimation of cosmological parameters from pseudo-power spectrum estimators. In this work, we focus on the analytical calculation of covariance matrices. We consider the case of observations of the Cosmic Microwave Background in temperature and polarization on a small footprint such as in the SPT-3G experiment, which observes 4% of the sky. Power spectra evaluated on small footprints are expected to have large correlations between modes, and these need to be accurately modelled. We present, for the first time, an algorithm that allows an efficient (but computationally expensive) exact calculation of analytic covariance matrices. Using it as our reference, we test the accuracy of existing fast approximations of the covariance matrix. We find that, when the power spectrum is binned in wide bandpowers, current approaches are correct up to the 5% level on the SPT-3G small sky footprint. Furthermore, we propose a new approximation which improves over the previous ones reaching a precision of 1% in the wide bandpowers case and generally more than 4 times more accurate than current approaches. Finally, we derive the covariance matrices for mask-corrected power spectra estimated by the PolSpice code. In particular, we include, in the case of a small sky fraction, the effect of the apodization of the large scale modes. While we considered the specific case of the CMB, our results are applicable to any other cosmological probe which requires the calculation of pseudo-power spectrum covariance matrices., Comment: 20 pages, 14 figures, 1 table
Published: 2022
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2. Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data

Author: Faustin Carter, S. E. Kuhlmann, Junjia Ding, Gene C. Hilton, J. C. Hood, A. T. Lee, M. Millea, Erik Shirokoff, Oliver Jeong, N. W. Halverson, Thomas Cecil, John E. Pearson, G. I. Noble, John E. Carlstrom, E. V. Denison, B. Thorne, K. Prabhu, C. L. Kuo, François R. Bouchet, M. Korman, Federico Bianchini, K. Dibert, S. Padin, Ethan Anderes, Neil Goeckner-Wald, D. Riebel, J. E. Ruhl, Jason W. Henning, Nikhel Gupta, N. Huang, M. Rouble, M. Jonas, RB Thakur, K. L. Thompson, J. T. Sayre, C. Tucker, A. A. Stark, A. Lowitz, M. A. Dobbs, N. L. Harrington, Z. Pan, Karen Byrum, A. H. Harke-Hosemann, C. Lu, Srinivasan Raghunathan, B. Riedel, C. L. Chang, A. Cukierman, Andreas Bender, Z. Ahmed, K. Aylor, E. M. Leitch, Alexandra S. Rahlin, S. Guns, J. A. Sobrin, K. W. Yoon, D. Howe, P. Chaubal, Young, Graeme Smecher, C. Umilta, J. F. Cliche, T. de Haan, Silvia Galli, H. Nguyen, Lloyd Knox, T. Natoli, K. Vanderlinde, T. M. Crawford, J. Fu, P. Paschos, S. S. Meyer, Christian L. Reichardt, H-M. Cho, L. R. Vale, A. Foster, K. T. Story, Karim Benabed, E. Hivon, E. Schiappucci, Anthony P. Jones, Andrew Nadolski, Lindsey Bleem, Jessica Avva, Peter S. Barry, L. Balkenhol, Bradford Benson, Yefremenko, R. Guyser, R. Gualtieri, C. M. Posada, Chang Feng, G. P. Holder, A. M. Kofman, Daniel Michalik, Novosad, J. D. Vieira, C. Daley, Gensheng Wang, W. L. Holzapfel, W. Quan, K. R. Ferguson, Adam Anderson, Gang Chen, Nathan Whitehorn, Robert Gardner, M. Archipley, Y. Omori, A. Suzuki, Lincoln Bryant, D. Dutcher, T.-L. Chou, Trupti Khaire, Joshua Montgomery, J. Stephen, A. E. Gambrel, Kent D. Irwin, W. L. K. Wu, Donna Kubik, P. A. R. Ade, and W. B. Everett
Subjects: Physics, 010308 nuclear & particles physics, Cosmic microwave background, Spectral density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Parameter space, 01 natural sciences, 7. Clean energy, symbols.namesake, Amplitude, Gravitational lens, South Pole Telescope, 0103 physical sciences, symbols, Planck, Multipole expansion, 010303 astronomy & astrophysics
Abstract: We present measurements of the $E$-mode ($EE$) polarization power spectrum and temperature-$E$-mode ($TE$) cross-power spectrum of the cosmic microwave background using data collected by SPT-3G, the latest instrument installed on the South Pole Telescope. This analysis uses observations of a 1500 deg$^2$ region at 95, 150, and 220 GHz taken over a four month period in 2018. We report binned values of the $EE$ and $TE$ power spectra over the angular multipole range $300 \le \ell < 3000$, using the multifrequency data to construct six semi-independent estimates of each power spectrum and their minimum-variance combination. These measurements improve upon the previous results of SPTpol across the multipole ranges $300 \le \ell \le 1400$ for $EE$ and $300 \le \ell \le 1700$ for $TE$, resulting in constraints on cosmological parameters comparable to those from other current leading ground-based experiments. We find that the SPT-3G dataset is well-fit by a $\Lambda$CDM cosmological model with parameter constraints consistent with those from Planck and SPTpol data. From SPT-3G data alone, we find $H_0 = 68.8 \pm 1.5 \mathrm{km\,s^{-1}\,Mpc^{-1}}$ and $\sigma_8 = 0.789 \pm 0.016$, with a gravitational lensing amplitude consistent with the $\Lambda$CDM prediction ($A_L = 0.98 \pm 0.12$). We combine the SPT-3G and the Planck datasets and obtain joint constraints on the $\Lambda$CDM model. The volume of the 68% confidence region in six-dimensional $\Lambda$CDM parameter space is reduced by a factor of 1.5 compared to Planck-only constraints, with only slight shifts in central values. We note that the results presented here are obtained from data collected during just half of a typical observing season with only part of the focal plane operable, and that the active detector count has since nearly doubled for observations made with SPT-3G after 2018.
Published: 2021

3. 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

4. Breaking the degeneracy between polarization efficiency and cosmological parameters in CMB experiments

Author: Silvia Galli, Karim Benabed, T. M. Crawford, W. L. Kimmy Wu, François R. Bouchet, E. Hivon, 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: Particle physics, data analysis method, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Cosmic microwave background, Scalar (mathematics), FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Computer Science::Digital Libraries, Spectral line, power spectrum: primordial, symbols.namesake, power spectrum: scalar, gravitation: lens, statistical analysis, 0103 physical sciences, neutrino: mass, Planck, cosmic background radiation: power spectrum, 010303 astronomy & astrophysics, Physics, polarization, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Polarization (waves), calibration, Amplitude, symbols, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Accurate cosmological parameter estimates using polarization data of the cosmic microwave background (CMB) put stringent requirements on map calibration, as highlighted in the recent results from the Planck satellite. In this paper, we point out that a model-dependent determination of polarization calibration can be achieved by the joint fit of the TE and EE CMB power spectra. This provides a valuable cross-check to band-averaged polarization efficiency measurements determined using other approaches. We demonstrate that, in $\Lambda$CDM, the combination of the TE and EE constrain polarization calibration with sub-percent uncertainty with Planck data and 2% uncertainty with SPTpol data. We arrive at similar conclusions when extending $\Lambda$CDM to include the amplitude of lensing $A_{\rm L}$, the number of relativistic species $N_{\rm eff}$, or the sum of the neutrino masses $\sum m_{\nu}$. The uncertainties on cosmological parameters are minimally impacted when marginalizing over polarization calibration, except, as can be expected, for the uncertainty on the amplitude of the primordial scalar power spectrum $\ln(10^{10} A_{\rm s})$, which increases by $20-50$%. However, this information can be fully recovered by adding TT data. For current and future ground-based experiments, SPT-3G and CMB-S4, we forecast the cosmological parameter uncertainties to be minimally degraded when marginalizing over polarization calibration parameters. In addition, CMB-S4 could constrain its polarization calibration at the level of $\sim$0.2% by combining TE and EE, and reach $\sim$0.06% by also including TT. We therefore conclude that relying on calibrating against Planck polarization maps, whose statistical uncertainty is limited to $\sim$0.5%, would be insufficient for upcoming experiments., Comment: 11 pages, 8 figures. Comments welcome
Published: 2021

5. 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

6. Tomographic weak lensing bispectrum: a thorough analysis towards the next generation of galaxy surveys

Author: F. Lacasa, Francis Bernardeau, Matteo Rizzato, Karim Benabed, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Covariance matrix, Gaussian, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), 01 natural sciences, symbols.namesake, Space and Planetary Science, 0103 physical sciences, Convergence (routing), Principal component analysis, symbols, Statistical physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Bispectrum, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We address key points for an efficient implementation of likelihood codes for modern weak lensing large-scale structure surveys. Specifically, we focus on the joint weak lensing convergence power spectrum-bispectrum probe and we tackle the numerical challenges required by a realistic analysis. Under the assumption of (multivariate) Gaussian likelihoods, we have developed a high performance code that allows highly parallelised prediction of the binned tomographic observables and of their joint non-Gaussian covariance matrix accounting for terms up to the 6-point correlation function and super-sample effects. This performance allows us to qualitatively address several interesting scientific questions. We find that the bispectrum provides an improvement in terms of signal-to-noise ratio (S/N) of about 10% on top of the power spectrum, making it a non-negligible source of information for future surveys. Furthermore, we are capable to test the impact of theoretical uncertainties in the halo model used to build our observables; with presently allowed variations we conclude that the impact is negligible on the S/N. Finally, we consider data compression possibilities to optimise future analyses of the weak lensing bispectrum. We find that, ignoring systematics, 5 equipopulated redshift bins are enough to recover the information content of a Euclid-like survey, with negligible improvement when increasing to 10 bins. We also explore principal component analysis and dependence on the triangle shapes as ways to reduce the numerical complexity of the problem., 29 pages, 14 figures. Latest version as accepted by MNRAS
Published: 2019

7. Redshift and luminosity evolution of the intrinsic alignments of galaxies in Horizon-AGN

Author: Lance Miller, Julien Devriendt, Adrianne Slyz, Sandrine Codis, Yohan Dubois, C. Pichon, Karim Benabed, Clotilde Laigle, Nora Elisa Chisari, and Raphael Gavazzi
Subjects: Physics, Absolute magnitude, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Population, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Redshift, Luminosity, Space and Planetary Science, 0103 physical sciences, astro-ph.CO, Galaxy formation and evolution, Interacting galaxy, education, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Intrinsic galaxy shape and angular momentum alignments can arise in cosmological large-scale structure due to tidal interactions or galaxy formation processes. Cosmological hydrodynamical simulations have recently come of age as a tool to study these alignments and their contamination to weak gravitational lensing. We probe the redshift and luminosity evolution of intrinsic alignments in Horizon-AGN between z=0 and z=3 for galaxies with an r-band absolute magnitude of 1 Mpc. Alignments of discs are null in projection and consistent with current low redshift observations. The combination of the two populations yields an overall amplitude a factor of ~4 lower than observed alignments of luminous red galaxies with a steeper luminosity dependence. The restriction on accurate galaxy shapes implies that the galaxy population in the simulation is complete only to an r-band absolute magnitude of, Comment: 23 pages, 17 figures, changes matching version accepted by MNRAS
Published: 2016

8. Semi-blind Bayesian inference of CMB map and power spectrum

Author: Jean-François Cardoso, Karim Benabed, Flavien Vansyngel, Benjamin D. Wandelt, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, Bayesian probability, Inference, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, Bayesian inference, 01 natural sciences, 0103 physical sciences, Phenomenological model, 010303 astronomy & astrophysics, media_common, Physics, methods: statistical, Physical model, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, methods: data analysis, Space and Planetary Science, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a new blind formulation of the Cosmic Microwave Background (CMB) inference problem. The approach relies on a phenomenological model of the multi-frequency microwave sky without the need for physical models of the individual components. For all-sky and high resolution data, it unifies parts of the analysis that have previously been treated separately, such as component separation and power spectrum inference. We describe an efficient sampling scheme that fully explores the component separation uncertainties on the inferred CMB products such as maps and/or power spectra. External information about individual components can be incorporated as a prior giving a flexible way to progressively and continuously introduce physical component separation from a maximally blind approach. We connect our Bayesian formalism to existing approaches such as Commander, SMICA and ILC, and discuss possible future extensions., Comment: 11 pages, 9 figures
Published: 2016

9. TEASING: a fast and accurate approximation for the low multipole likelihood of the cosmic microwave background temperature

Author: Simon Prunet, J.-F. Cardoso, Eric Hivon, and Karim Benabed
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Posterior probability, Cosmic microwave background, FOS: Physical sciences, Inverse, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Measure (mathematics), Data set, Angular spectrum method, Space and Planetary Science, 0103 physical sciences, Statistical physics, Multipole expansion, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Inverse-gamma distribution
Abstract: We explore the low-l likelihood of the angular spectrum C(l) of masked CMB temperature maps using an adaptive importance sampler. We find that, in spite of a partial sky coverage, the likelihood distribution of each C(l) closely follows an inverse gamma distribution. Our exploration is accurate enough to measure the inverse gamma parameters along with the correlation between multipoles. Those quantities are used to build an approximation of the joint posterior distribution of the low-l likelihood. The accuracy of the proposed approximation is established using both statistical criteria and a mock cosmological parameter fit. When applied to the WMAP5 data set, this approximation yields cosmological parameter estimates at the same level of accuracy as the best current techniques but with very significant speed gains., Comment: 10 pages, 10 figures, submitted to MNRAS
Published: 2009

10. Simulating weak lensing of CMB maps

Author: S. Basak, Karim Benabed, and Simon Prunet
Subjects: Physics, Cosmic microwave background, Fast Fourier transform, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic background radiation, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), symbols.namesake, Gravitational lens, Space and Planetary Science, symbols, Planck, Weak gravitational lensing
Abstract: Aims. Accurate predictions of cosmic microwave background (CMB) anisotropies and polarization are required for analyzing future CMB data sets, which ultimately require accurately simulated lensed maps. Methods. We present a fast, arbitrarily accurate method to simulate the effect of gravitational lensing of the CMB anisotropies and polarization fields by large-scale structures on arbitrarily spaced grid points over a unit sphere using a non-equispaced fast Fourier transform (NFFT). Results. The angular power spectrum of the simulated lensed CMB map, particularly the B-mode of polarization, agrees extremely well with analytical predictions. The analytical derivation of CMB-lensed spectra is based on non-trivial, partially resummed perturbative expansions of the correlation functions, for which our simulations therefore provide an accurate numerical validation. We demonstrate the efficiency and accuracy of the method and exhibit their dependence on the algorithm parameters. Lensed CMB maps simulated in this method are a useful tool for the analysis and interpretation of upcoming CMB experiments, such as PLANCK and ACT. Our code is available on request.
Published: 2009

11. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Author: A. Coulais, G. de Zotti, A. Benoit-Lévy, B. P. Crill, B. Van Tent, Francesca Perrotta, F. Atrio-Barandela, S. Ricciardi, T. Riller, Federico Nati, Anna Gregorio, R. B. Barreiro, A. Mennella, Y. Giraud-Héraud, Torsten A. Enßlin, Radek Stompor, Jörg P. Rachen, Allan Hornstrup, D. Sutton, X. Dupac, M. Tomasi, Ben Rusholme, Mika Juvela, D. Alina, Jacques Delabrouille, Rashmikant V. Sudiwala, Marc-Antoine Miville-Deschênes, Luca Terenzi, C. Combet, Doris Arzoumanian, Etienne Pointecouteau, Marco Bersanelli, A. De Rosa, L. Fanciullo, L. Popa, J.-F. Cardoso, Jose M. Diego, A. Moneti, Benjamin D. Wandelt, Julian Borrill, Eric Hivon, Stéphane Plaszczynski, Kevin M. Huffenberger, Katia Ferrière, H. K. Eriksen, Ken Ganga, F. Noviello, O. Doré, Gianluca Morgante, Carlo Burigana, Paolo Natoli, Fabio Finelli, M. Piat, Michael P. Hobson, L. A. Montier, C. A. Oxborrow, F. Boulanger, Fabrizio Villa, J.-P. Bernard, M. I. R. Alves, Alessandro Gruppuso, Pavel Naselsky, C. Armitage-Caplan, L. Mendes, Sabino Matarrese, W. Holmes, John Bond, Peter G. Martin, F. Piacentini, Douglas J. Marshall, Igor D. Novikov, A. Curto, E. Battaner, J.-M. Lamarre, Andrea Zonca, François R. Bouchet, Juan D. Soler, R. J. Davis, J. A. Tauber, D. L. Harrison, H. C. Chiang, George Helou, Luigi Danese, V. Stolyarov, Monique Arnaud, Hannu Kurki-Suonio, M. Migliaccio, R. Kneissl, A. Catalano, L. Pagano, Karim Benabed, Tuhin Ghosh, Charles R. Lawrence, M. Tucci, Enrique Martínez-González, F. Pajot, F. Couchot, T. R. Jaffe, Nabila Aghanim, F. Pasian, Alessandro Melchiorri, Andrea Bracco, R. D. Davies, P. B. Lilje, Peter A. R. Ade, G. Polenta, Clive Dickinson, V.-M. Pelkonen, I. Ristorcelli, G. Umana, Davide Pietrobon, Ted Kisner, M. Ashdown, Edith Falgarone, S. Donzelli, Marian Douspis, Davide Maino, A. A. Fraisse, G. Aniano, L. Toffolatti, Sergi R. Hildebrandt, L. P. L. Colombo, Anthony Lasenby, E. Keihänen, G. W. Pratt, Krzysztof M. Gorski, Calvin B. Netterfield, Stephane Colombi, Martin Kunz, P. R. Christensen, A. J. Banday, Dmitry Novikov, L. A. Wade, Daniela Paoletti, A. Chamballu, R. Leonardi, C. Rosset, G. Roudier, Dipak Munshi, Mathieu Remazeilles, George Efstathiou, Michele Liguori, M. Linden-Vørnle, Jussi Valiviita, Vincent Guillet, J. González-Nuevo, Silvia Masi, Locke D. Spencer, J. Knoche, Simon Prunet, P. Bielewicz, Olivier Forni, M. Frailis, M. Reinecke, Carlo Baccigalupi, François Levrier, C. Hernández-Monteagudo, F. K. Hansen, J.-F. Sygnet, Luca Valenziano, E. Franceschi, S. Galeotta, J. Aumont, J. F. Macías-Pérez, Graca Rocha, Douglas Scott, N. Mandolesi, Andrew H. Jaffe, Philip Lubin, P. de Bernardis, L. Perotto, O. Perdereau, A.-S. Suur-Uski, M. Giard, M. Maris, Reijo Keskitalo, Guilaine Lagache, M. López-Caniego, Daniel J. Mortlock, M. Sandri, P. Vielva, J. A. Murphy, Matthieu Tristram, Pasquale Mazzotta, C. Renault, F. Cuttaia, Jean-Loup Puget, W. C. Jones, Consejo Superior de Investigaciones Científicas (España), European Research Council, Junta de Andalucía, European Commission, Ministerio de Ciencia e Innovación (España), 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), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Planck, Department of Physics, Helsinki Institute of Physics, Ade, P, Aghanim, N, Alina, D, Alves, M, Aniano, G, Armitage-Caplan, C, Arnaud, M, Arzoumanian, D, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Battaner, E, Benabed, K, Benoit-Levy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bracco, A, Burigana, C, Cardoso, J, Catalano, A, Chamballu, A, Chiang, H, Christensen, P, Colombi, S, Colombo, L, Combet, C, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Donzelli, S, Dore, O, Douspis, M, Dupac, X, Efstathiou, G, Ensslin, T, Eriksen, H, Falgarone, E, Fanciullo, L, Ferriere, K, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, F, Harrison, D, Helou, G, Hernandez-Monteagudo, C, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Huffenberger, K, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihanen, E, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden-Vornle, M, Lopez-Caniego, M, Lubin, P, Macias-Perez, J, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martinez-Gonzalez, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Noviello, F, Novikov, D, Novikov, I, Oxborrow, C, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Pelkonen, V, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Popa, L, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rusholme, B, Sandri, M, Scott, D, Soler, J, Spencer, L, Stolyarov, V, Stompor, R, Sudiwala, R, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, L, Wandelt, B, Zonca, A, Ade, P. A. R., Aghanim, N., Alina, D., Alves, M. I. R., Aniano, G., Armitage Caplan, C., Arnaud, M., Arzoumanian, D., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, C., Cardoso, J. F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pelkonen, V. M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Scott, D., Soler, J. D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Zonca, A., Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)
Subjects: statistical [Methods], magnetic field [ISM], Astronomy, cloud [ISM], Astrophysics, 7. Clean energy, ISM: clouds, TAURUS, Anisotropy, ComputingMilieux_MISCELLANEOUS, QB, ASSOCIATIONS, Physics, infrared: ISM, Dust , extinction, Line-of-sight, general [ISM], extinction, ADAPTIVE MESH REFINEMENT, ISM [Submillimeter], Dust, SUBMILLIMETER EMISSION, Polarization (waves), Magnetic field, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, submillimeter: ISM, INTERSTELLAR POLARIZATION, dust, extinction, ISM: magnetic fields, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Atomic physics, clouds [ISM], EFFICIENCY, Opacity, GRAIN ALIGNMENT, ISM [Infrared], FOS: Physical sciences, MAGNETIC-FIELDS, NO, Dust, extinction, Infrared: ISM, ISM: general, Submillimeter: ISM, Astronomy and Astrophysics, Space and Planetary Science, symbols.namesake, ISM: magnetic field, Settore FIS/05 - Astronomia e Astrofisica, ISM: cloud, RADIATIVE TORQUE ALIGNMENT, Planck, Astrophysics::Galaxy Astrophysics, Brewster's angle, numerical [Methods], magnetic fields [ISM], Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Observational [Methods], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR CLOUDS, Magnetohydrodynamics
Abstract: et al., Polarized emission observed by Planck HFI at 353 GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction pmax decreases with column density NH in the more opaque fields with NH> 1021 cm-2; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction pmax in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function . However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties., The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement No. 267934.
Published: 2015

12. Cosmic shear analysis with CFHTLS deep data

Author: Elisabetta Semboloni, Laura C. Parker, Michael J. Hudson, Liping Fu, Karim Benabed, Ismael Tereno, Yannick Mellier, Henk Hoekstra, Stephen D. J. Gwyn, L. van Waerbeke, R. Maoli, 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), 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), Department of Physics and Astronomy, University of British Columbia, Department of Physics and Astronomy, University of Victoria, Departamento de Fisica, Universidade de Lisboa, Department of Physics, University of Waterloo, and Dipartimento di Fisica, Università di Roma 1 La Sapienza
Subjects: Cold dark matter, cosmology : dark matter, gravitational lensing, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, scale structure of universe, symbols.namesake, cosmology : large, cosmology: theory, 0103 physical sciences, 010303 astronomy & astrophysics, Weak gravitational lensing, Photometric redshift, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), cosmology: large-scale structure of universe, Astronomy and Astrophysics, cosmology: dark matter, Redshift, Galaxy, cosmology : theory, Space and Planetary Science, symbols, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract: We present the first cosmic shear measurements obtained from the T0001 release of the Canada-France-Hawaii Telescope Legacy Survey. The data set covers three uncorrelated patches (D1, D3 and D4) of one square degree each observed in u*, g', r', i' and z' bands, out to i'=25.5. The depth and the multicolored observations done in deep fields enable several data quality controls. The lensing signal is detected in both r' and i' bands and shows similar amplitude and slope in both filters. B-modes are found to be statistically zero at all scales. Using multi-color information, we derived a photometric redshift for each galaxy and separate the sample into medium and high-z galaxies. A stronger shear signal is detected from the high-z subsample than from the low-z subsample, as expected from weak lensing tomography. While further work is needed to model the effects of errors in the photometric redshifts, this results suggests that it will be possible to obtain constraints on the growth of dark matter fluctuations with lensing wide field surveys. The various quality tests and analysis discussed in this work demonstrate that MegaPrime/Megacam instrument produces excellent quality data. The combined Deep and Wide surveys give sigma_8= 0.89 pm 0.06 assuming the Peacock & Dodds non-linear scheme and sigma_8=0.86 pm 0.05 for the halo fitting model and Omega_m=0.3. We assumed a Cold Dark Matter model with flat geometry. Systematics, Hubble constant and redshift uncertainties have been marginalized over. Using only data from the Deep survey, the 1 sigma upper bound for w_0, the constant equation of state parameter is w_0 < -0.8., 14 pages, 16 figures, accepted A&A
Published: 2006

13. Dancing in the dark: galactic properties trace spin swings along the cosmic web

Author: Joseph Silk, Julien Devriendt, V. de Lapparent, Dmitry Pogosyan, Sandrine Codis, Vincent Desjacques, Karim Benabed, François R. Bouchet, Susan A. Kassin, Stéphane Arnouts, Y. Dubois, M. Volonteri, Simon Prunet, Jean-François Cardoso, Thierry Sousbie, D. Le Borgne, Clotilde Laigle, Stéphane Colombi, C. Pichon, C. Welker, Sébastien Peirani, Romain Teyssier, B. Milliard, E. Bertin, D. Vibert, Raphael Gavazzi, H. J. McCracken, Laurence Tresse, Adrianne Slyz, Marie Treyer, Taysun Kimm, S. Rouberol, J. Blaizot, University of Zurich, Dubois, Y, 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), and 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)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 530 Physics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, methods: numerical, Peculiar galaxy, 1912 Space and Planetary Science, cosmology: theory, Galaxy group, galaxies: formation, [INFO]Computer Science [cs], Disc, Lenticular galaxy, ComputingMilieux_MISCELLANEOUS, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, Astronomy, Astronomy and Astrophysics, Void galaxy, Space and Planetary Science, 10231 Institute for Computational Science, Elliptical galaxy, 3103 Astronomy and Astrophysics, large-scale structure of Universe, Dark galaxy, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A large-scale hydrodynamical cosmological simulation, Horizon-AGN, is used to investigate the alignment between the spin of galaxies and the cosmic filaments above redshift 1.2. The analysis of more than 150 000 galaxies per time step in the redshift range 1.2, Comment: 18 pages, 19 figures, accepted for publication in MNRAS, movies and pictures of the simulation can be found at this address http://horizon-AGN.projet-horizon.fr
Published: 2014

14. Intrinsic alignment of simulated galaxies in the cosmic web: implications for weak lensing surveys

Author: Vincent Desjacques, Raphael Gavazzi, C. Pichon, Adrianne Slyz, Karim Benabed, Julien Devriendt, Sandrine Codis, Dmitry Pogosyan, and Yohan Dubois
Subjects: Physics, Luminous infrared galaxy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Radio galaxy, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Peculiar galaxy, Space and Planetary Science, Galaxy group, 0103 physical sciences, Elliptical galaxy, Dark galaxy, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The intrinsic alignment of galaxy shapes (by means of their angular momentum) and their cross-correlation with the surrounding dark matter tidal field are investigated using the 160 000, z=1.2 synthetic galaxies extracted from the high-resolution cosmological hydrodynamical simulation Horizon-AGN. One- and two-point statistics of the spin of the stellar component are measured as a function of mass and colour. For the low-mass galaxies, this spin is locally aligned with the tidal field `filamentary' direction while, for the high-mass galaxies, it is perpendicular to both filaments and walls. The bluest galaxies of our synthetic catalog are more strongly correlated with the surrounding tidal field than the reddest galaxies, and this correlation extends up to 10 Mpc/h comoving distance. We also report a correlation of the projected ellipticities of blue, intermediate mass galaxies on a similar scale at a level of 10^(-4) which could be a concern for cosmic shear measurements. We do not report any measurable intrinsic alignments of the reddest galaxies of our sample. This work is a first step toward the use of very realistic catalog of synthetic galaxies to evaluate the contamination of weak lensing measurement by the intrinsic galactic alignments., Comment: 15 pages, accepted for publication in MNRAS
Published: 2014
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15. Full-sky CMB lensing reconstruction in presence of sky-cuts

Author: Simon Prunet, Jean-François Cardoso, T. Déchelette, A. Benoit-Lévy, Duncan Hanson, Karim Benabed, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Traitement et Communication de l'Information (LTCI), Télécom ParisTech-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), University College of London [London] (UCL), 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), Laboratoire de Traitement et Transport de l'Information (L2TI), Université Sorbonne Paris Nord, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), McGill University = Université McGill [Montréal, Canada], and Planck Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gaussian, media_common.quotation_subject, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, gravitational lensing: weak, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy and Astrophysics, Galactic plane, methods: data analysis, Galaxy, Space and Planetary Science, Sky, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We consider the reconstruction of the CMB lensing potential and its power spectrum of the full sphere in presence of sky-cuts due to point sources and Galactic contaminations. Those two effects are treated separately. Small regions contaminated by point sources are filled in using Gaussian constrained realizations. The Galactic plane is simply masked using an apodized mask before lensing reconstruction. This algorithm recovers the power spectrum of the lensing potential with no significant bias., Comment: Submitted to A&A
Published: 2013

16. CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing

Author: Lance Miller, Christopher Bonnett, Hendrik Hildebrandt, Henk Hoekstra, Tim Schrabback, Michael J. Hudson, Thomas D. Kitching, Fergus Simpson, Liping Fu, Sanaz Vafaei, Konrad Kuijken, Malin Velander, Joachim Harnois-Déraps, Karim Benabed, Ludovic Van Waerbeke, Barnaby Rowe, Yannick Mellier, E. Semboloni, Catherine Heymans, Martin Kilbinger, Thomas Erben, J. Benjamin, and Jean Coupon
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, FOS: Physical sciences, Lambda-CDM model, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, media_common, Physics, 010308 nuclear & particles physics, Matter power spectrum, Astronomy and Astrophysics, Universe, Redshift, 13. Climate action, Space and Planetary Science, symbols, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: We present cosmological constraints from 2D weak gravitational lensing by the large-scale structure in the Canada-France Hawaii Telescope Lensing Survey (CFHTLenS) which spans 154 square degrees in five optical bands. Using accurate photometric redshifts and measured shapes for 4.2 million galaxies between redshifts of 0.2 and 1.3, we compute the 2D cosmic shear correlation function over angular scales ranging between 0.8 and 350 arcmin. Using non-linear models of the dark-matter power spectrum, we constrain cosmological parameters by exploring the parameter space with Population Monte Carlo sampling. The best constraints from lensing alone are obtained for the small-scale density-fluctuations amplitude sigma_8 scaled with the total matter density Omega_m. For a flat LambdaCDM model we obtain sigma_8(Omega_m/0.27)^0.6 = 0.79+-0.03. We combine the CFHTLenS data with WMAP7, BOSS and an HST distance-ladder prior on the Hubble constant to get joint constraints. For a flat LambdaCDM model, we find Omega_m = 0.283+-0.010 and sigma_8 = 0.813+-0.014. In the case of a curved wCDM universe, we obtain Omega_m = 0.27+-0.03, sigma_8 = 0.83+-0.04, w_0 = -1.10+-0.15 and Omega_K = 0.006+0.006-0.004. We calculate the Bayesian evidence to compare flat and curved LambdaCDM and dark-energy CDM models. From the combination of all four probes, we find models with curvature to be at moderately disfavoured with respect to the flat case. A simple dark-energy model is indistinguishable from LambdaCDM. Our results therefore do not necessitate any deviations from the standard cosmological model., Comment: 21 pages, 13 figures, 10 tables. Accepted for publication in MNRAS
Published: 2013

17. Planck intermediate results (Corrigendum). V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect

Author: T. Riller, A. Hempel, Elena Pierpaoli, M. Ashdown, H. K. Eriksen, N. Ponthieu, Jean-François Cardoso, Barbara Comis, X. Dupac, E. Churazov, G. Chon, L. Montier, Guilaine Lagache, M. Giard, F. Noviello, M. Arnaud, G. Polenta, L. Cayón, L. Toffolatti, A. Moneti, Federico Nati, Alessandro Gruppuso, Luca Terenzi, Ricardo Génova-Santos, B. P. Crill, Lung-Yih Chiang, M. López-Caniego, G. Castex, Paolo Cabella, C. Renault, U. Dörl, Anthony Lasenby, Stefano Borgani, M. Sandri, Francine R. Marleau, E. Keihänen, C. Hernández-Monteagudo, J. R. Bond, M. Frailis, Carlo Baccigalupi, Francesca Perrotta, J.-P. Bernard, L. Popa, Peter A. R. Ade, S. Osborne, E. Hivon, Nicola Vittorio, Julian Borrill, Daniel J. Mortlock, J. Aumont, Torsten A. Enßlin, Hannu Kurki-Suonio, Sophie Henrot-Versille, B. Van Tent, D. J. Marshall, J.-F. Sygnet, F. Cuttaia, A. J. Banday, Charles R. Lawrence, Matthieu Roman, Olivier Forni, W. C. Jones, Alain Benoit, Michael P. Hobson, I. Flores-Cacho, Lloyd Knox, David L. Clements, Jean-Loup Puget, T. Jagemann, W. A. Holmes, Karim Benabed, O. Perdereau, Klaus Dolag, Alessandro Melchiorri, Jose M. Diego, Michael L. Brown, Y. Giraud-Héraud, R. A. Burenin, Luca Valenziano, I. D. Novikov, Paolo Natoli, R. Leonardi, C. Rosset, F. K. Hansen, Marc-Antoine Miville-Deschênes, B. Rusholme, Herve Dole, D. L. Harrison, Andrew R. Liddle, S. Donzelli, Sabino Matarrese, F. Piacentini, I. Ristorcelli, Subhasish Mitra, M. Frommert, Pavel Naselsky, R. J. Davis, Giorgio Savini, Jean-Baptiste Melin, A. Coulais, A. Catalano, Marian Douspis, Anna Bonaldi, Mika Juvela, Andrea Zacchei, Martin Reinecke, I. F. Bikmaev, S. Ricciardi, Rashmikant V. Sudiwala, Michele Maris, Sergio Colafrancesco, J. A. Tauber, Niraj Welikala, Jose Alberto Rubino-Martin, Jussi Varis, William T. Reach, P. Carvalho, E. Franceschi, R. B. Barreiro, R. Piffaretti, J.-M. Lamarre, D. Sutton, T. Poutanen, P. de Bernardis, Hervé Bourdin, G. Hurier, G. W. Pratt, Jörg P. Rachen, Hans Böhringer, Gianluca Morgante, Simon D. M. White, Fernando Atrio-Barandela, A. Mennella, Nabila Aghanim, George F. Smoot, Luigi Danese, J. González-Nuevo, Matthieu Tristram, G. de Zotti, Theodore Kisner, G. Luzzi, Pasquale Mazzotta, Fabio Pasian, R. A. Sunyaev, Hans Ulrik Nørgaard-Nielsen, Silvia Masi, F. Pajot, Anne Lähteenmäki, F.-X. Désert, R. Bhatia, P. Vielva, J. Démoclès, S. R. Hildebrandt, D. Herranz, M. Le Jeune, R. Kneissl, G. Patanchon, Marcella Massardi, Jean-Luc Starck, A.-S. Suur-Uski, S. Galeotta, Martin White, Douglas Scott, Ken Ganga, Krzysztof M. Gorski, P. R. Christensen, B. D. Wandelt, J. F. Macías-Pérez, E. Martínez-González, N. Mandolesi, G. de Gasperis, Stéphane Colombi, Pablo Fosalba, Andrew H. Jaffe, Irek Khamitov, M. Piat, J. Knoche, Rafael Rebolo, E. Battaner, Etienne Pointecouteau, Graca Rocha, M. Tomasi, A. Da Silva, F. R. Bouchet, F. Villa, Carlo Burigana, Marco Bersanelli, L. Mendes, M. Rossetti, Stéphane Plaszczynski, L. Perotto, Jussi Tuovinen, Jérôme Bobin, Davide Maino, A. Chamballu, Simona Mei, Jacques Delabrouille, J. A. Murphy, Simon Prunet, Amedeo Balbi, Fabio Finelli, T. R. Jaffe, James G. Bartlett, Martin Kunz, Mathieu Remazeilles, Lawrence A. Wade, Håkon Dahle, O. Doré, Andrea Zonca, A. Gregorio, P. B. Lilje, D. Yvon, L. P. L. Colombo, Dmitry Novikov, Daniela Paoletti, Dipak Munshi, and George Efstathiou
Subjects: Surface (mathematics), cosmology: observations, galaxies: clusters: general, galaxies: clusters: intracluster medium, submillimeter: general, X-rays: general, errata, addenda, Astrophysics, System of linear equations, 01 natural sciences, Matrix (mathematics), Settore FIS/05 - Astronomia e Astrofisica, Position (vector), errata: addenda, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, submillimiter: general, cosmology: observations, galaxies: clusters: general, galaxies: clusters: intracluster medium, submillimeter: general, X-rays: general, errata, addenda, 010308 nuclear & particles physics, Scattering, Plane (geometry), Cosmology: observations, Galaxies: clusters: intracluster medium, X-Rays: General, Astronomy and Astrophysics, Transformation (function), Space and Planetary Science, addenda, errata, Gaussian optics
Abstract: We have developed an approximate technique, based on the principles of multi-mode Gaussian optics, for studying the behaviour of shaped off-axis mirrors. We describe a mirror as an inclined phase-transforming plane, where the phase transformation across the plane is determined by the depth of the mirror as a function of position. The scattering matrix is calculated in the usual way by evaluating the overlap integrals over some surface for which the amplitudes and phases of the incoming and outgoing fields are known; because, however, the modes are not orthogonal over the surface of interest, a system of linear equations has to be solved. We demonstrate the “thin-mirror” technique by studying the behaviour of paraboloidal and ellipsoidal mirros, and we show how the performance of measured and approximate surfaces can be assessed.
Published: 2013

18. Planck pre-launch status: The HFI instrument, from specification to actual performance

Author: Peter A. R. Ade, V. Yurchenko, F. Piacentini, R. Pons, M. Nexon, G. Recouvreur, Christopher G. Paine, C. Dumesnil, Philippe Camus, J. Pahn, O. Perdereau, M. Tristram, Sarah E. Church, M.-A. Miville-Deschênes, A. Coulais, J. J. Bock, F.-X. Désert, J. Lande, G. Serra, J. F. Macías-Pérez, F. Pajot, J.-L. Beney, F. Bouchet, Simon Prunet, J.-P. Torre, C. Leroy, N. Ponthieu, Bruno Maffei, E. Bréelle, M. Giard, B. P. Crill, J.-L. Puget, L. Vibert, W. A. Holmes, T. C. Koch, E. Hivon, J. Haissinski, R. V. Sudiwala, B. Mansoux, L. Montier, K. Dassas, C. Renault, C. Evesque, R. S. Bhatia, Alain Benoit, J. Charra, Sophie Henrot-Versille, W. C. Jones, Y. Blanc, P. de Bernardis, A. Arondel, F. Couchot, C. Rosset, Martin Crook, C. Marty, Stéphane Plaszczynski, B. Leriche, Etienne Pointecouteau, D. Rambaud, D. Santos, J.-F. Sygnet, M. Charra, Tom Bradshaw, J.-M. Delouis, I. Ristorcelli, P. Eng, Jan Tauber, Thierry Maciaszek, Karim Benabed, H. Lagardère, D. Yvon, A. Moneti, J. Narbonne, Giorgio Savini, Andrew E. Lange, X. Dupac, Y. Longval, A. Catalano, R. Gispert, P. de Marcillac, P. Lami, George Efstathiou, C. Mercier, Silvia Masi, Jacques Delabrouille, J. A. Murphy, Ken Ganga, J.-Ph. Bernard, M. Piat, Adam Woodcraft, J.-M. Lamarre, G. Guyot, L. Guglielmi, P. Stassi, J.-J. Fourmond, 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), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), 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), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, 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), Centre National d'Études Spatiales [Toulouse] (CNES), Département de Physique des Particules (ex SPP) (DPhP), 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, PLANCK, École normale supérieure - Paris (ENS Paris), 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), 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), Hélium : du fondamental aux applications (HELFA), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-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, 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), Cryogénie (Cryo), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), 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), Département de Physique des Particules (ex SPP) (DPP), 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), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université 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), 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), Cryo - Cryogénie, 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), 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, and 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)
Subjects: cosmic microwave background, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Point source, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Cosmic background radiation, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Radio spectrum, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, techniques: photometric, Optics, law, space vehicles: instruments, submillimeter: general, techniques: polarimetric, 0103 physical sciences, Calibration, Planck, 010303 astronomy & astrophysics, QB, Physics, 010308 nuclear & particles physics, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, symbols, business
Abstract: Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz–1 THz range.\ud \ud Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration.\ud \ud Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques.\ud \ud Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification.
Published: 2010

19. ASKI: full-sky lensing map-making algorithms

Author: Stephane Colombi, Christophe Pichon, E. Thiebaut, Romain Teyssier, T. Sousbie, Karim Benabed, Simon Prunet, University of Zurich, Pichon, C, 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Deblurring, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 530 Physics, media_common.quotation_subject, gravitational lensing, FOS: Physical sciences, techniques: image processing, 01 natural sciences, surveys, 1912 Space and Planetary Science, 0103 physical sciences, Maximum a posteriori estimation, Cluster (physics), methods: N-body simulations, 010303 astronomy & astrophysics, media_common, Physics, methods: statistical, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Inversion (meteorology), Space and Planetary Science, Sky, [SDU]Sciences of the Universe [physics], 10231 Institute for Computational Science, Kurtosis, 3103 Astronomy and Astrophysics, Deconvolution, large-scale structure of Universe, Algorithm, Smoothing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Within the context of upcoming full-sky lensing surveys, the edge-preserving non- linear algorithm Aski is presented. Using the framework of Maximum A Posteriori inversion, it aims at recovering the full-sky convergence map from surveys with masks. It proceeds in two steps: CCD images of crowded galactic fields are deblurred using automated edge-preserving deconvolution; once the reduced shear is estimated, the convergence map is also inverted via an edge- preserving method. For the deblurring, it is found that when the observed field is crowded, this gain can be quite significant for realistic ground-based surveys when both positivity and edge-preserving penalties are imposed during the iterative deconvolution. For the convergence inversion, the quality of the reconstruction is investigated on noisy maps derived from the horizon N-body simulation, with and without Galactic cuts, and quantified using one-point statistics, power spectra, cluster counts, peak patches and the skeleton. It is found that the reconstruction is able to interpolate and extrapolate within the Galactic cuts/non-uniform noise; its sharpness-preserving penalization avoids strong biasing near the clusters of the map; it reconstructs well the shape of the PDF as traced by its skewness and kurtosis; the geometry and topology of the reconstructed map is close to the initial map as traced by the peak patch distribution and the skeleton's differential length; the two-points statistics of the recovered map is consistent with the corresponding smoothed version of the initial map; the distribution of point sources is also consistent with the corresponding smoothing, with a significant improvement when edge preserving prior is applied. The contamination of B-modes when realistic Galactic cuts are present is also investigated. Leakage mainly occurs on large scales., Comment: 24 pages, 21 figures accepted for publication to MNRAS
Published: 2010

20. Evidence for the accelerated expansion of the Universe from weak lensing tomography with COSMOS

Author: Marusa Bradac, Martin Kilbinger, Henk Hoekstra, Tim Schrabback, Benjamin Joachimi, Patrick Simon, Peter Schneider, Konrad Kuijken, Hendrik Hildebrandt, Tim Eifler, Christopher D. Fassnacht, Yannick Mellier, Elisabetta Semboloni, Phil Marshall, Ludovic Van Waerbeke, Karim Benabed, Eric Morganson, Thomas Erben, Malin Velander, Jan Hartlap, F. William High, and Stefan Hilbert
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Deceleration parameter, 010308 nuclear & particles physics, General relativity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Cosmology, Metric expansion of space, Space and Planetary Science, 0103 physical sciences, Dark energy, Flatness (cosmology), 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a tomographic cosmological weak lensing analysis of the HST COSMOS Survey. Applying our lensing-optimized data reduction, principal component interpolation for the ACS PSF, and improved modelling of charge-transfer inefficiency, we measure a lensing signal which is consistent with pure gravitational modes and no significant shape systematics. We carefully estimate the statistical uncertainty from simulated COSMOS-like fields obtained from ray-tracing through the Millennium Simulation. We test our pipeline on simulated space-based data, recalibrate non-linear power spectrum corrections using the ray-tracing, employ photometric redshifts to reduce potential contamination by intrinsic galaxy alignments, and marginalize over systematic uncertainties. We find that the lensing signal scales with redshift as expected from General Relativity for a concordance LCDM cosmology, including the full cross-correlations between different redshift bins. For a flat LCDM cosmology, we measure sigma_8(Omega_m/0.3)^0.51=0.75+-0.08 from lensing, in perfect agreement with WMAP-5, yielding joint constraints Omega_m=0.266+0.025-0.023, sigma_8=0.802+0.028-0.029 (all 68% conf.). Dropping the assumption of flatness and using HST Key Project and BBN priors only, we find a negative deceleration parameter q_0 at 94.3% conf. from the tomographic lensing analysis, providing independent evidence for the accelerated expansion of the Universe. For a flat wCDM cosmology and prior w in [-2,0], we obtain w, Comment: 26 pages, 25 figures, matches version accepted for publication by Astronomy and Astrophysics
Published: 2009
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21. Simulating weak lensing on CMB maps

Author: Soumen Basak, Karim Benabed, and Simon Prunet
Subjects: Physics, Fast Fourier transform, Cosmic microwave background, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), Computational physics, symbols.namesake, Gravitational lens, symbols, Planck, Anisotropy, Weak gravitational lensing
Abstract: We present a fast, arbitrarily accurate method to simulate the effect of gravitational lensing of the Cosmic Microwave Background anisotropies and polarization fields by large scale structures. We demonstrate the efficiency and accuracy of the method and exhibit their dependence on the algorithm parameters., Comment: 10 pages, 6 figures, 5 tables
Published: 2008
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22. The cosmic shear three-point functions

Author: Karim Benabed and Roman Scoccimarro
Subjects: Physics, COSMIC cancer database, 010308 nuclear & particles physics, Analytic model, Astrophysics (astro-ph), Estimator, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Dark matter halo, Shear (geology), Space and Planetary Science, 0103 physical sciences, Statistical physics, 010303 astronomy & astrophysics, Weak gravitational lensing
Abstract: We investigate the three-point functions of the weak lensing cosmic shear, using both analytic methods and numerical results from N-body simulations. The analytic model, an isolated dark matter halo with a powerlaw profile chosen to fit the effective index at the scale probed, can be used to understand the basic properties of the eight three-point functions observed in simulations. We use this model to construct a single three-point function estimator that "optimally" combines the eight three-point functions. This new estimator is an alternative to Map statistics and provides up to a factor of two improvement in signal to noise compared to previously used combinations of cosmic shear three-point functions., Comment: 17 pages, 18 figures. Submitted to A&A
Published: 2005
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23. Constraining dark energy evolution with gravitational lensing by large scale structures

Author: Karim Benabed and Ludovic Van Waerbeke
Subjects: Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Order (ring theory), Spectral density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Cosmology, 0103 physical sciences, Dark energy, Sensitivity (control systems), 010303 astronomy & astrophysics, Weak gravitational lensing, Energy (signal processing), Quintessence
Abstract: We study the sensitivity of weak lensing by large scale structures to the evolution of dark energy. We explore a 2-parameters model of dark energy evolution, inspired by tracking quintessence models. To this end, we compute the likelihood of a few representative models with varying and non varying equation of states. Based on an earlier work, we show that the evolution of dark energy has a much stronger impact on the non-linear structure growth than on the angular diameter distance, which makes large scale structure measurements a very efficient probe of this evolution. For the different models, we investigate the dark energy parameters degeneracies with the mass power spectrum shape Gamma, normalisation sigma_8, and with the matter mean density Omega_M. This result is a strong motivation for performing large scale structure simulations beyond the simple constant dark energy models, in order to calibrate the non-linear regime accurately. Prospective for the Canada France Hawaii Telescope Legacy Survey (CFHTLS) and Super-Novae Acceleration Probe (SNAP) are given. These results complement nicely the cosmic microwave background and Super-Novae constraints. Weak lensing is shown to be more sensitive to a variation of the equation of state, whereas CMB and SNIa give information on its constant part., Comment: Submitted to Physical Review D
Published: 2004

24. Testing Quintessence models with large-scale structure growth

Author: Francis Bernardeau, Karim Benabed, Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), and arXiv, Import
Subjects: Physics, Nuclear and High Energy Physics, Field (physics), Equation of state (cosmology), Astrophysics (astro-ph), Spectral density, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, PACS: 98.80.Cq, 98.62.Sb, 98.65.Dx, Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Classical mechanics, Skewness, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Convergence (routing), Statistical physics, Constant (mathematics), Weak gravitational lensing, Quintessence
Abstract: We explore the possibility of putting constraints on quintessence models with large-scale structure observations. In particular we compute the linear and second order growth rate of the fluctuations in different flavors of quintessence scenarios. We show that effective models of quintessence (e.g. with a constant equation of state) do not account of the results found in more realistic scenarios. The impact of these results on observational quantities such as the shape of the non-linear power spectrum in weak lensing surveys or the skewness of the convergence field are investigated. It appears that the observational signature of quintessence models are specific and rather large. They clearly cannot be mistaken with a change of (\Omega_{0})., Comment: 11 pages, 7 figures, uses revtex
Published: 2001

25. CMB B-polarization to map the Large-scale Structures of the Universe

Author: L. van Waerbeke, Karim Benabed, Francis Bernardeau, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Canadian Institute for Theoretical Astrophysics (CITA), and arXiv, Import
Subjects: Physics, Nuclear and High Energy Physics, education.field_of_study, Population, Cosmic microwave background, Astrophysics (astro-ph), FOS: Physical sciences, Cosmological constant, Astrophysics, Cosmic variance, Astrophysics::Cosmology and Extragalactic Astrophysics, PACS: 98.80.Es, 98.35.Ce, 98.62.Sb, 98.70.Vc, Galaxy, Dark matter halo, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Observational cosmology, education, Weak gravitational lensing
Abstract: We explore the possibility of using the B-type polarization of the CMB to map the large-scale structures of the Universe taking advantage of the lens effects on the CMB polarization. The functional relation between the B component with the primordial CMB polarization and the line-of-sight mass distribution is explicited. Noting that a sizeable fraction (at least 40%) of the dark halo population which is responsible of this effect can also be detected in galaxy weak lensing survey, we present statistical quantities that should exhibit a strong sensitivity to this overlapping. We stress that it would be a sound test of the gravitational instability picture, independent on many systematic effects that may hamper lensing detection in CMB or galaxy survey alone. Moreover we estimate the intrinsic cosmic variance of the amplitude of this effect to be less than 8% for a 100, deg^2 survey with a 10' CMB beam. Its measurement would then provide us with an original mean for constraining the cosmological parameters, more particularly, as it turns out, the cosmological constant Lambda., Comment: Latex2e with REVTEX ; 14 pages, 8 figures
Published: 2000
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26. Conservative constraints on early cosmology with M<scp>ONTE</scp>P<scp>YTHON</scp>

Author: Simon Prunet, Benjamin Audren, Julien Lesgourgues, and Karim Benabed
Subjects: Physics, 010308 nuclear & particles physics, Cosmic microwave background, Degrees of freedom (statistics), Inference, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Decoupling (cosmology), Python (programming language), 01 natural sciences, Cosmology, Theoretical physics, 0103 physical sciences, Code (cryptography), Neutrino, 010303 astronomy & astrophysics, computer, computer.programming_language
Abstract: Models for the latest stages of the cosmological evolution rely on a less solid theoretical and observational ground than the description of earlier stages like BBN and recombination. As suggested in a previous work by Vonlanthen et al., it is possible to tweak the analysis of CMB data in such way to avoid making assumptions on the late evolution, and obtain robust constraints on "early cosmology parameters". We extend this method in order to marginalise the results over CMB lensing contamination, and present updated results based on recent CMB data. Our constraints on the minimal early cosmology model are weaker than in a standard LCDM analysis, but do not conflict with this model. Besides, we obtain conservative bounds on the effective neutrino number and neutrino mass, showing no hints for extra relativistic degrees of freedom, and proving in a robust way that neutrinos experienced their non-relativistic transition after the time of photon decoupling. This analysis is also an occasion to describe the main features of the new parameter inference code Monte Python, that we release together with this paper. Monte Python is a user-friendly alternative to other public codes like CosmoMC, interfaced with the Boltzmann code class.
Published: 2013

27. Probing inflation with cosmic microwave background polarization: the weak lensing effect on the covariance of cosmic microwave background spectra

Author: Karim Benabed, Jonathan Rocher, and François R. Bouchet
Subjects: Inflation (cosmology), Physics, Photon, 010308 nuclear & particles physics, Covariance matrix, 4. Education, Gaussian, Cosmic microwave background, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Covariance, Polarization (waves), 01 natural sciences, Computational physics, symbols.namesake, 0103 physical sciences, symbols, 010303 astronomy & astrophysics, Weak gravitational lensing
Abstract: CMB anisotropies are modified by the weak lensing effect of intervening large scale structures on the photon path from the last scattering surface to the observer. This has to be accounted for when observational data of sensitive experiments are used to constrain cosmological models. A common approximation to analyze the CMB angular power spectra is to include only the Gaussian part of the lensing correction and to ignore the non-gaussian terms in the error covariance matrix of the spectra. In order to investigate the validity of this approximation, we computed these non-Gaussian terms by using a perturbative expansion method. We present a graphical method to write down any N-point correlation functions at any order in lensing. We use a pedagogical approach to demonstrate that neglecting non-gaussian terms is an accurate approximation for all polarizations but B, and it will remain so even for the analysis of very sensitive post-Planck experiments. For the B polarization, non-gaussian contributions up to order 4 must be taken into account.
Published: 2007

28. Estimation of cosmological parameters using adaptive importance sampling

Author: J.-F. Cardoso, Martin Kilbinger, Gersende Fort, Christian P. Robert, Olivier Cappé, Karim Benabed, Simon Prunet, Darren Wraith, CEntre de REcherches en MAthématiques de la DEcision (CEREMADE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Dauphine-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Traitement et Communication de l'Information (LTCI), Télécom ParisTech-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche en Économie et Statistique (CREST), Ecole Nationale de la Statistique et de l'Analyse de l'Information [Bruz] (ENSAI)-École polytechnique (X)-École Nationale de la Statistique et de l'Administration Économique (ENSAE Paris)-Centre National de la Recherche Scientifique (CNRS), ANR-05-BLAN-0283,ECOSSTAT,Exploration du modèle cosmologique par fusion statistique de grands relevés hétérogènes(2005), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris Dauphine-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Benabed, Karim, and Programme non thématique - Appel à projets de recherche - Exploration du modèle cosmologique par fusion statistique de grands relevés hétérogènes - - ECOSSTAT2005 - ANR-05-BLAN-0283 - BLANC - VALID
Subjects: FOS: Computer and information sciences, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Monte Carlo method, Bayesian probability, FOS: Physical sciences, Markov process, Scale (descriptive set theory), Statistics - Computation, 01 natural sciences, Data type, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010104 statistics & probability, symbols.namesake, 0103 physical sciences, Statistical physics, 0101 mathematics, [STAT.CO]Statistics [stat]/Computation [stat.CO], 010303 astronomy & astrophysics, Computation (stat.CO), Physics, Sampling (statistics), Markov chain Monte Carlo, [INFO.INFO-MO]Computer Science [cs]/Modeling and Simulation, Statistics::Computation, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Algorithm, Importance sampling, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a Bayesian sampling algorithm called adaptive importance sampling or Population Monte Carlo (PMC), whose computational workload is easily parallelizable and thus has the potential to considerably reduce the wall-clock time required for sampling, along with providing other benefits. To assess the performance of the approach for cosmological problems, we use simulated and actual data consisting of CMB anisotropies, supernovae of type Ia, and weak cosmological lensing, and provide a comparison of results to those obtained using state-of-the-art Markov Chain Monte Carlo (MCMC). For both types of data sets, we find comparable parameter estimates for PMC and MCMC, with the advantage of a significantly lower computational time for PMC. In the case of WMAP5 data, for example, the wall-clock time reduces from several days for MCMC to a few hours using PMC on a cluster of processors. Other benefits of the PMC approach, along with potential difficulties in using the approach, are analysed and discussed., Comment: 17 pages, 11 figures

29. Performance and characterization of the SPT-3G digital frequency-domain multiplexed readout system using an improved noise and crosstalk model

Author: Joshua Montgomery, Peter A. R. Ade, Zeeshan Ahmed, Ethan Anderes, Adam J. Anderson, Melanie Archipley, Jessica S. Avva, Kevin Aylor, Lennart Balkenhol, Peter S. Barry, Ritoban B. Thakur, Karim Benabed, Amy N. Bender, Bradford A. Benson, Federico Bianchini, Lindsey E. Bleem, Francois R. Bouchet, Lincoln Bryant, Karen Byrum, John E. Carlstrom, Faustin W. Carter, Thomas W. Cecil, Clarence L. Chang, Prakrut Chaubal, Geoffrey Chen, Hsiaomei Cho, Ti-Lin Chou, Jean-Francois Cliche, Tom M. Crawford, Ari Cukierman, Cail Daley, Tijmen de Haan, Edward V. Denison, Karia Dibert, Junjia Ding, Matt A. Dobbs, Daniel Dutcher, Tucker Elleflot, Wendeline Everett, Cahng Feng, Kyle R. Ferguson, Allen Foster, Jianyang Fu, Silvia Galli, Anne E. Gambrel, Robert W. Gardner, Neil Goeckner-Wald, John C. Groh, Riccardo Gualtieri, Sam Guns, Nikhel Gupta, Robert Guyser, Nils W. Halverson, Angelina H. Harke-Hosemann, Nicholas L. Harrington, Jason W. Henning, Gene C. Hilton, Eric Hivon, William L. Holzapfel, John C. Hood, Doug Howe, Nicholas Huang, Kent D. Irwin, Oliver B. Jeong, Michelle Jonas, Adam Jones, Trupti S. Khaire, Lloyd Knox, Anna M. Kofman, Milo Korman, Donna L. Kubik, Stephen Kuhlmann, Chao-Lin Kuo, Adrian T. Lee, Erik M. Leitch, Amy E. Lowitz, Chunyu Lu, Stephan S. Meyer, Daniel Michalik, Marius Millea, Andrew Nadolski, Tyler Natoli, Hogan Nguyen, Gavin I. Noble, Valentine Novosad, Yuuki Omori, Steve Padin, Zhaodi Pan, Pascal Paschos, John Pearson, Chrystian M. Posada, Karthik Prabhu, Wei Quan, Alexandra Rahlin, Christian L. Reichardt, David Riebel, Benedikt Riedel, Maclean Rouble, John E. Ruhl, James T. Sayre, Eduardo Schiappucci, Erik Shirokoff, Graeme Smecher, Joshua A. Sobrin, Antony A. Stark, Judith Stephen, Kyle T. Story, Aritoki Suzuki, Keith L. Thompson, Ben Thorne, Carole Tucker, Caterina Umilta, Leila R. Vale, Keith Vanderlinde, Joaquin D. Vieira, Gensheng Wang, Nathan Whitehorn, Wai L. K. Wu, Volodymyr Yefremenko, Ki W. Yoon, Matt R. Young, 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), and SPT-3G
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, Mechanical Engineering, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Electronic, Optical and Magnetic Materials, 010309 optics, Space and Planetary Science, Control and Systems Engineering, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Instrumentation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The third generation South Pole Telescope camera (SPT-3G) improves upon its predecessor (SPTpol) by an order of magnitude increase in detectors on the focal plane. The technology used to read out and control these detectors, digital frequency-domain multiplexing (DfMUX), is conceptually the same as used for SPTpol, but extended to accommodate more detectors. A nearly 5x expansion in the readout operating bandwidth has enabled the use of this large focal plane, and SPT-3G performance meets the forecasting targets relevant to its science objectives. However, the electrical dynamics of the higher-bandwidth readout differ from predictions based on models of the SPTpol system due to the higher frequencies used, and parasitic impedances associated with new cryogenic electronic architecture. To address this, we present an updated derivation for electrical crosstalk in higher-bandwidth DfMUX systems, and identify two previously uncharacterized contributions to readout noise, which become dominant at high bias frequency. The updated crosstalk and noise models successfully describe the measured crosstalk and readout noise performance of SPT-3G. These results also suggest specific changes to warm electronics component values, wire-harness properties, and SQUID parameters, to improve the readout system for future experiments using DfMUX, such as the LiteBIRD space telescope., Comment: Accepted to the Journal of Astronomical Telescopes, Instruments, and Systems
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30. Non-Gaussian cosmology : theoretical and statistical challenges for modern galaxy surveys

Author: Rizzato, Matteo, 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), Sorbonne Université, Karim Benabed, and Francis Bernardeau
Subjects: [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Non-linear physics, Lentillage gravitationnel faible, Covariance matrix, Euclid, Matrice de covariance, Physique non linéaire, Large-scale structures, Weak gravitational lensing, Grandes structures, Cosmologie, Cosmology
Abstract: In this thesis, we address key points for an efficient implementation of likelihood codes for modern weak lensing large-scale structure surveys. Specifically, we will focus on the joint weak lensing convergence power spectrum-bispectrum probe and we will tackle the numerical challenges required by realistic analyses. In order to clearly convey the importance of our research, we first provide an in-depth review of the background material required for a comprehensive understanding of the final results. The cosmological context of the study is provided, followed by a description of the technical elements inherent to unbiased covariance matrix estimation for the probe considered. Under the assumption of multivariate Gaussian likelihood, we developed a high performance code that allows highly parallelised prediction of the binned tomographic observables and of their joint non-Gaussian covariance matrix accounting for terms up to the 6-point correlation function and super-sample effects. This performance allows us to qualitatively address several interesting scientific questions. We find that the bispectrum provides an improvement in terms of signal-to-noise ratio (S/N) of about 10% on top of the power spectrum alone, making it a non-negligible source of information for future surveys. Furthermore, we are capable to address the impact of theoretical uncertainties in the halo model used to build our observables; with presently allowed variations we conclude that the impact is negligible on the S/N. Finally, we consider data compression possibilities to optimise future analyses of the weak lensing bispectrum. We find that, ignoring systematics, 5 equipopulated redshift bins are enough to recover the information content of a Euclid-like survey, with negligible improvement when increasing to 10 bins. We also explore principal component analysis and dependence on the triangle shapes as ways to reduce the numerical complexity of the problem.; Nous détaillons dans cette thèse les différentes étapes nécessaires l’implémentation numérique optimale du calcul de la vraisemblance des paramètres cosmologiques appliqué aux relevés modernes de lentillage gravitationnel faible des grandes structures. En particulier, nous nous concentrons sur la détection conjointe du spectre de puissance et du bispectre du lentillage gravitationnel faible. Pour ce faire, nous avons relevé les défis numériques requis par une analyse complète. Dans un premier temps, nous dressons l'état de l'art nécessaire à la compréhension du formalisme de la sonde cosmologique susmentionnée et nous décrivons comment obtenir une estimation non biaisée de la matrice de covariance pour les observables considérées. En supposant une vraisemblance gaussienne multivariée, nous avons développé un algorithme de haute performance permettant de prédire les observables tomographiques rééchantillonnées avec leur matrice de covariance conjointe en tenant compte des fonctions de corrélations de 2 à 6 points et des corrélations avec les modes hors du relevé. La performance de notre code nous permet de répondre aux exigences scientifiques des relevés de galaxies des dix prochaines années. Nous montrons que le bispectre du lentillage gravitationnel faible améliore le signal sur bruit (S/N) de notre analyse conjointe du spectre et du bispectre d'environ 10% en comparaison avec une analyse du spectre seulement. Par conséquent, le bispectre est une source non négligeable d’information cosmologique pour les relevés futurs. En outre, nous sommes capables de quantifier l’impact des incertitudes théoriques liées à la description de la matière noire dans le “modèle des halos” qui est utilisé pour construire nos observables; cet impact se trouve être négligeable pour l’analyse du S/N. Finalement, nous étudions la possibilité de réduire les données pour optimiser les analyses futures du bispectre du lentillage. Nous trouvons qu’en ignorant les erreurs systématiques une analyse ne concernant que 5 échantillons en décalage vers le rouge permet d’obtenir la même quantité d’information que dans le cas d’un relevé semblable à celui d'Euclid, qui utilise 10 échantillons sans améliorer le S/N. Nous explorons également l’analyse en composantes principales et la dépendance de l’information cosmologique en fonction de la forme des triangles comme méthodes permettant de réduire la complexité du problème.
Published: 2019

31. Cosmologie non-Gaussienne : défis théoriques et statistiques pour les relevés de galaxie modernes

Author: Rizzato, Matteo, 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), Sorbonne Université, Karim Benabed, and Francis Bernardeau
Subjects: [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Non-linear physics, Lentillage gravitationnel faible, Covariance matrix, Euclid, Matrice de covariance, Physique non linéaire, Large-scale structures, Weak gravitational lensing, Grandes structures, Cosmologie, Cosmology
Abstract: In this thesis, we address key points for an efficient implementation of likelihood codes for modern weak lensing large-scale structure surveys. Specifically, we will focus on the joint weak lensing convergence power spectrum-bispectrum probe and we will tackle the numerical challenges required by realistic analyses. In order to clearly convey the importance of our research, we first provide an in-depth review of the background material required for a comprehensive understanding of the final results. The cosmological context of the study is provided, followed by a description of the technical elements inherent to unbiased covariance matrix estimation for the probe considered. Under the assumption of multivariate Gaussian likelihood, we developed a high performance code that allows highly parallelised prediction of the binned tomographic observables and of their joint non-Gaussian covariance matrix accounting for terms up to the 6-point correlation function and super-sample effects. This performance allows us to qualitatively address several interesting scientific questions. We find that the bispectrum provides an improvement in terms of signal-to-noise ratio (S/N) of about 10% on top of the power spectrum alone, making it a non-negligible source of information for future surveys. Furthermore, we are capable to address the impact of theoretical uncertainties in the halo model used to build our observables; with presently allowed variations we conclude that the impact is negligible on the S/N. Finally, we consider data compression possibilities to optimise future analyses of the weak lensing bispectrum. We find that, ignoring systematics, 5 equipopulated redshift bins are enough to recover the information content of a Euclid-like survey, with negligible improvement when increasing to 10 bins. We also explore principal component analysis and dependence on the triangle shapes as ways to reduce the numerical complexity of the problem.; Nous détaillons dans cette thèse les différentes étapes nécessaires l’implémentation numérique optimale du calcul de la vraisemblance des paramètres cosmologiques appliqué aux relevés modernes de lentillage gravitationnel faible des grandes structures. En particulier, nous nous concentrons sur la détection conjointe du spectre de puissance et du bispectre du lentillage gravitationnel faible. Pour ce faire, nous avons relevé les défis numériques requis par une analyse complète. Dans un premier temps, nous dressons l'état de l'art nécessaire à la compréhension du formalisme de la sonde cosmologique susmentionnée et nous décrivons comment obtenir une estimation non biaisée de la matrice de covariance pour les observables considérées. En supposant une vraisemblance gaussienne multivariée, nous avons développé un algorithme de haute performance permettant de prédire les observables tomographiques rééchantillonnées avec leur matrice de covariance conjointe en tenant compte des fonctions de corrélations de 2 à 6 points et des corrélations avec les modes hors du relevé. La performance de notre code nous permet de répondre aux exigences scientifiques des relevés de galaxies des dix prochaines années. Nous montrons que le bispectre du lentillage gravitationnel faible améliore le signal sur bruit (S/N) de notre analyse conjointe du spectre et du bispectre d'environ 10% en comparaison avec une analyse du spectre seulement. Par conséquent, le bispectre est une source non négligeable d’information cosmologique pour les relevés futurs. En outre, nous sommes capables de quantifier l’impact des incertitudes théoriques liées à la description de la matière noire dans le “modèle des halos” qui est utilisé pour construire nos observables; cet impact se trouve être négligeable pour l’analyse du S/N. Finalement, nous étudions la possibilité de réduire les données pour optimiser les analyses futures du bispectre du lentillage. Nous trouvons qu’en ignorant les erreurs systématiques une analyse ne concernant que 5 échantillons en décalage vers le rouge permet d’obtenir la même quantité d’information que dans le cas d’un relevé semblable à celui d'Euclid, qui utilise 10 échantillons sans améliorer le S/N. Nous explorons également l’analyse en composantes principales et la dépendance de l’information cosmologique en fonction de la forme des triangles comme méthodes permettant de réduire la complexité du problème.
Published: 2019

32. Development and assessment of a blind component separation method for cosmological parameter estimation

Author: Umiltà, Caterina, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Pierre et Marie Curie - Paris VI, Karim Benabed, Jean-François Cardoso, and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Component, Planck, Avant-Plans, Rayonnement fossile, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Séparation de composantes, Cosmological parameters, Paramètres cosmologiques, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmic background radiation, Cosmologie
Abstract: The Planck satellite observed the whole sky at various frequencies in the microwave range. These data are of high value to cosmology, since they help understanding the primordial universe through the observation of the cosmic microwave background (CMB) signal. To extract the CMB information, astrophysical foreground emissions need to be removed via component separation techniques. In this work I use the blind component separation method SMICA to estimate the CMB angular power spectrum with the aim of using it for the estimation of cosmological parameters. In order to do so, small scales limitations as the residual contamination of unresolved point sources and the noise need to be addressed. In particular, the point sources are modelled as two independent populations with a flat angular power spectrum: by adding this information, the SMICA method is able to recover the joint emission law of point sources. Auto-spectra deriving from one sky map have a noise bias at small scales, while cross-spectra show no such bias. This is particularly true in the case of cross-spectra between data-splits, corresponding to sky maps with the same astrophysical content but different noise properties. I thus adapt SMICA to use data-split cross-spectra only. The obtained CMB spectra from simulations and Planck 2015 data are used to estimate cosmological parameters. Results show that this estimation can be biased if the shape of the (weak) foreground residuals in the angular power spectrum is not well known. In the end, I also present results of the study of a Modified Gravity model called Induced Gravity.; Le rayonnement fossile, ou CMB, est un sujet d’étude clé pour la cosmologie car il indique l’état de l’univers à une époque primordiale. Le CMB est observable dans le ciel dans la bande de fréquences des micro-ondes. Cependant, il existe des processus astrophysiques, les avant-plans, qui émettent dans les micro-ondes, et rendent indispensable le traitement des données avec des méthodes de séparation de composantes. J'utilisé la méthode aveugle SMICA pour obtenir une estimation directe du spectre de puissance angulaire du CMB. La détermination des petites échelles de ce spectre est limité par les avant-plans comme les galaxies lointaines, et par le biais du bruit. Dans cette analyse, ces deux limitations sont abordées. En ajoutant des hypothèses sur la physique des galaxies lointaines, il est possible de guider l’algorithme pour estimer leur loi d'émission. Un spectre de puissance angulaire obtenu d'une carte du ciel a un biais dû au bruit à petites échelles. Toutefois, les spectres obtenus en croisant différentes cartes n'ont pas ce biais. J'ai donc adapté la méthode SMICA pour qu'elle n'utilise que ces derniers, diminuant l'incertitude due au bruit dans l'estimation du CMB. Cette méthode a été étudiée sur des nombreuses simulations et sur les données Planck 2015, afin d'estimer des paramètres cosmologiques. Les résultats montrent que la contamination résiduelle des avant-plans présente dans le spectre CMB, même si fortement réduite, peut introduire des biais dans l'estimation des paramètres si la forme des résiduels n'est pas bien connue. Dans cette thèse, je montre les résultats obtenus en étudiant un modèle de gravité modifiée.
Published: 2017

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32 results on '"Karim Benabed"'

1. Accurate CMB covariance matrices: exact calculation and approximations

2. Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data

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

4. Breaking the degeneracy between polarization efficiency and cosmological parameters in CMB experiments

5. Planck intermediate results

6. Tomographic weak lensing bispectrum: a thorough analysis towards the next generation of galaxy surveys

7. Redshift and luminosity evolution of the intrinsic alignments of galaxies in Horizon-AGN

8. Semi-blind Bayesian inference of CMB map and power spectrum

9. TEASING: a fast and accurate approximation for the low multipole likelihood of the cosmic microwave background temperature

10. Simulating weak lensing of CMB maps

11. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

12. Cosmic shear analysis with CFHTLS deep data

13. Dancing in the dark: galactic properties trace spin swings along the cosmic web

14. Intrinsic alignment of simulated galaxies in the cosmic web: implications for weak lensing surveys

15. Full-sky CMB lensing reconstruction in presence of sky-cuts

16. CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing

17. Planck intermediate results (Corrigendum). V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect

18. Planck pre-launch status: The HFI instrument, from specification to actual performance

19. ASKI: full-sky lensing map-making algorithms

20. Evidence for the accelerated expansion of the Universe from weak lensing tomography with COSMOS

21. Simulating weak lensing on CMB maps

22. The cosmic shear three-point functions

23. Constraining dark energy evolution with gravitational lensing by large scale structures

24. Testing Quintessence models with large-scale structure growth

25. CMB B-polarization to map the Large-scale Structures of the Universe

26. Conservative constraints on early cosmology with M<scp>ONTE</scp>P<scp>YTHON</scp>

27. Probing inflation with cosmic microwave background polarization: the weak lensing effect on the covariance of cosmic microwave background spectra

28. Estimation of cosmological parameters using adaptive importance sampling

29. Performance and characterization of the SPT-3G digital frequency-domain multiplexed readout system using an improved noise and crosstalk model

30. Non-Gaussian cosmology : theoretical and statistical challenges for modern galaxy surveys

31. Cosmologie non-Gaussienne : défis théoriques et statistiques pour les relevés de galaxie modernes

32. Development and assessment of a blind component separation method for cosmological parameter estimation

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32 results on '"Karim Benabed"'

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