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58 results on '"COSMOLOGY: OBSERVATIONS"'

1. Planck 2013 results. VI. high frequency instrument data processing

Author

Tauber, J, Ade, PAR, Aghanim, N, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Battaner, E, Benabed, K, Benoît, A, Benoit-Lévy, A, Bernard, JP, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bowyer, JW, Bridges, M, Bucher, M, Burigana, C, Cardoso, JF, Catalano, A, Chamballu, A, Chary, RR, Chen, X, Chiang, HC, Chiang, LY, Christensen, PR, Church, S, Clements, DL, Colombi, S, Colombo, LPL, Combet, C, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, JM, Désert, FX, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Dunkley, J, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Finelli, F, and Forni, O

Subjects
methods: data analysis, cosmic background radiation, cosmology: observations, surveys, astro-ph.CO, astro-ph.IM, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

© 2014 ESO. We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857 GHz with an angular resolution ranging from 9.I 7 to 4.I 6. The detector noise per (effective) beam solid angle is respectively, 10, 6, 12, and 39 μK in the four lowest HFI frequency channels (100-353 GHz) and 13 and 14 kJy sr-1 in the 545 and 857 GHz channels. Relative to the 143 GHz channel, these two high frequency channels are calibrated to within 5% and the 353 GHz channel to the percent level. The 100 and 217 GHz channels, which together with the 143 GHz channel determine the high-multipole part of the CMB power spectrum (50., 2500), are calibrated relative to 143 GHz to better than 0.2%.

Published
2014

2. Planck intermediate results: XVI. Profile likelihoods for cosmological parameters

Author

Ade, PAR, Aghanim, N, Arnaud, M, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartlett, JG, Battaner, E, Benabed, K, Benoit-Lévy, A, Bernard, JP, Bersanelli, M, Bielewicz, P, Bobin, J, Bonaldi, A, Bond, JR, Bouchet, FR, Burigana, C, Cardoso, JF, Catalano, A, Chamballu, A, Chiang, HC, Christensen, PR, Clements, DL, Colombi, S, Colombo, LPL, Couchot, F, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Dupac, X, Enßlin, TA, Eriksen, HK, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Galeotta, S, Galli, S, Ganga, K, Giard, M, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Hansen, FK, Harrison, DL, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Hovest, W, Huffenberger, KM, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, JM, Lasenby, A, Lawrence, CR, Leonardi, R, Liddle, A, Liguori, M, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Lubin, PM, Macías-Pérez, JF, Maffei, B, Maino, D, Mandolesi, N, and Maris, M

Subjects
cosmic background radiation, cosmology: observations, cosmology: theory, cosmological parameters, methods: statistical, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We explore the 2013 Planck likelihood function with a high-precision multi-dimensional minimizer (Minuit). This allows a refinement of the CDM best-fit solution with respect to previously-released results, and the construction of frequentist confidence intervals using profile likelihoods. The agreement with the cosmological results from the Bayesian framework is excellent, demonstrating the robustness of the Planck results to the statistical methodology. We investigate the inclusion of neutrino masses, where more significant differences may appear due to the non-Gaussian nature of the posterior mass distribution. By applying the Feldman-Cousins prescription, we again obtain results very similar to those of the Bayesian methodology. However, the profile-likelihood analysis of the cosmic microwave background (CMB) combination (Planck+WP+highL) reveals a minimum well within the unphysical negative-mass region. We show that inclusion of the Planck CMB-lensing information regularizes this issue, and provide a robust frequentist upper limit σmv ≤0:26 eV (95% confidence) from the CMB+lensing+BAO data combination. © ESO 2014.

Published
2014

3. KiDS and Euclid

Author

A. Loureiro, L. Whittaker, A. Spurio Mancini, B. Joachimi, A. Cuceu, M. Asgari, B. Stölzner, T. Tröster, A. H. Wright, M. Bilicki, A. Dvornik, B. Giblin, C. Heymans, H. Hildebrandt, H. Shan, A. Amara, N. Auricchio, C. Bodendorf, D. Bonino, E. Branchini, M. Brescia, V. Capobianco, C. Carbone, J. Carretero, M. Castellano, S. Cavuoti, A. Cimatti, R. Cledassou, G. Congedo, L. Conversi, Y. Copin, L. Corcione, M. Cropper, A. Da Silva, M. Douspis, F. Dubath, C. A. J. Duncan, X. Dupac, S. Dusini, S. Farrens, S. Ferriol, P. Fosalba, M. Frailis, E. Franceschi, M. Fumana, B. Garilli, B. Gillis, C. Giocoli, A. Grazian, F. Grupp, S. V. H. Haugan, W. Holmes, F. Hormuth, K. Jahnke, M. Kümmel, S. Kermiche, A. Kiessling, M. Kilbinger, T. Kitching, K. Kuijken, M. Kunz, H. Kurki-Suonio, S. Ligori, P.B. Lilje, I. Lloro, O. Mansutti, O. Marggraf, K. Markovic, F. Marulli, R. Massey, M. Meneghetti, G. Meylan, M. Moresco, B. Morin, L. Moscardini, E. Munari, S. M. Niemi, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, V. Pettorino, S. Pires, M. Poncet, L. Popa, F. Raison, J. Rhodes, H. Rix, M. Roncarelli, R. Saglia, P. Schneider, A. Secroun, S. Serrano, C. Sirignano, G. Sirri, L. Stanco, J. L. Starck, P. Tallada-Crespí, A. N. Taylor, I. Tereno, R. Toledo-Moreo, F. Torradeflot, E. A. Valentijn, Y. Wang, N. Welikala, J. Weller, G. Zamorani, J. Zoubian, S. Andreon, M. Baldi, S. Camera, R. Farinelli, G. Polenta, N. Tessore, National Aeronautics and Space Administration (US), European Research Council, European Space Agency, European Commission, Centre National d'Études Spatiales [Toulouse] (CNES), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), KiDS, Euclid, A. Loureiro, L. Whittaker, A. Spurio Mancini, B. Joachimi, A. Cuceu, M. Asgari, B. St??lzner, T. Tr??ster, A. H. Wright, M. Bilicki, A. Dvornik, B. Giblin, C. Heyman, H. Hildebrandt, H. Shan, A. Amara, N. Auricchio, C. Bodendorf, D. Bonino, E. Branchini, M. Brescia, V. Capobianco, C. Carbone, J. Carretero, M. Castellano, S. Cavuoti, A. Cimatti, R. Cledassou, G. Congedo, L. Conversi, Y. Copin, L. Corcione, M. Cropper, A. Da Silva, M. Douspi, F. Dubath, C. A. J. Duncan, X. Dupac, S. Dusini, S. Farren, S. Ferriol, P. Fosalba, M. Fraili, E. Franceschi, M. Fumana, B. Garilli, B. Gilli, C. Giocoli, A. Grazian, F. Grupp, S. V. H. Haugan, W. Holme, F. Hormuth, K. Jahnke, M. K??mmel, S. Kermiche, A. Kiessling, M. Kilbinger, T. Kitching, K. Kuijken, M. Kunz, H. Kurki-Suonio, S. Ligori, P.B. Lilje, I. Lloro, O. Mansutti, O. Marggraf, K. Markovic, F. Marulli, R. Massey, M. Meneghetti, G. Meylan, M. Moresco, B. Morin, L. Moscardini, E. Munari, S. M. Niemi, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, V. Pettorino, S. Pire, M. Poncet, L. Popa, F. Raison, J. Rhode, H. Rix, M. Roncarelli, R. Saglia, P. Schneider, A. Secroun, S. Serrano, C. Sirignano, G. Sirri, L. Stanco, J. L. Starck, P. Tallada-Cresp??, A. N. Taylor, I. Tereno, R. Toledo-Moreo, F. Torradeflot, E. A. Valentijn, Y. Wang, N. Welikala, J. Weller, G. Zamorani, J. Zoubian, S. Andreon, M. Baldi, S. Camera, R. Farinelli, G. Polenta, N. Tessore, Astronomy, Loureiro, A., Whittaker, L., Spurio Mancini, A., Joachimi, B., Cuceu, A., Asgari, M., Stölzner, B., Tröster, T., Wright, A. H., Bilicki, M., Dvornik, A., Giblin, B., Heymans, C., Hildebrandt, H., Shan, H., Amara, A., Auricchio, N., Bodendorf, C., Bonino, D., Branchini, E., Brescia, M., Capobianco, V., Carbone, C., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Cropper, M., Da Silva, A., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kümmel, M., Kuijken, K., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Meneghetti, M., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Raison, F., Rhodes, J., Rix, H., Roncarelli, M., Saglia, R., Schneider, P., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J. L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Baldi, M., Camera, S., Farinelli, R., Polenta, G., Tessore, N., Department of Physics, and Helsinki Institute of Physics

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), kilo-degree survey, Large-scale structure of Universe, statistical-analysis, spectroscopic survey measurement, Cosmological parameters, FOS: Physical sciences, 2-point statistics, parameter constraints, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, Gravitational lensing: weak, dark energy survey, data release, cosmology: observation, weak lensing surveys, Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 115 Astronomy, Space science, galaxy shape measurement, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], growth-rate, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A. Loureiro et al., We present a tomographic weak lensing analysis of the Kilo Degree Survey Data Release 4 (KiDS-1000), using a new pseudo angular power spectrum estimator (pseudo-Cℓ) under development for the ESA Euclid mission. Over 21 million galaxies with shape information are divided into five tomographic redshift bins, ranging from 0.1 to 1.2 in photometric redshift. We measured pseudo-Cℓ using eight bands in the multipole range 76, M.A. and T.T. acknowledge support from the European Research Council under grant number 647112. A.H.W. and A.D. acknowledge support from the European Research Council Consolidator Grant (No. 770935). M.B. is supported by the Polish National Science Center through grants no. 2020/38/E/ST9/00395, 2018/30/E/ST9/00698 and 2018/31/G/ST9/03388, and by the Polish Ministry of Science and Higher Education through grant DIR/WK/2018/12. B.G. acknowledges support from the European Research Council under grant number 647112 and from the Royal Society through an Enhancement Award (RGF/EA/181006). C.H. acknowledges support from the European Research Council under grant number 647112, and support from the Max Planck Society and the Alexander von Humboldt Foundation in the framework of the Max Planck-Humboldt Research Award endowed by the Federal Ministry of Education and Research. H. Hildebrandt is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1) as well as an ERC Consolidator Grant (No. 770935). H.Y.S. acknowledges the support from NSFC of China under grant 11973070, the Shanghai Committee of Science and Technology grant No. 19ZR1466600 and Key Research Program of Frontier Sciences, CAS, Grant No. ZDBS-LY-7013. The KiDS-1000 data products in this paper are based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017 and 177.A-3018, and on data products produced by Target/OmegaCEN, INAF-OACN, INAF-OAPD and the KiDS production team, on behalf of the KiDS consortium. The authors acknowledge the Euclid Consortium, the European Space Agency, and a number of agencies and institutes that have supported the development of Euclid, in particular the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the French Centre National d’Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Romanian Space Agency, the State Secretariat for Education, Research and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid web site (http://www.euclid-ec.org). Author Contributions: All authors contributed to the development and writing of this paper. The authorship list is given in several groups: the lead authors (A.L., L.W., A.S.M., B.J., A.C.), followed by an alphabetical group that includes those who are key contributors to both the scientific analysis and the KiDS data products, and a further alphabetical group covering those who have either made a significant contribution to the KiDS data products or to the scientific analysis.

Published
2022

4. KiDS-1000: Constraints on the intrinsic alignment of luminous red galaxies

Author

Fortuna, Maria Cristina, Hoekstra, Henk, Johnston, Harry, Vakili, Mohammadjavad, Kannawadi, Arun, Georgiou, Christos, Joachimi, Benjamin, Wright, Angus H., Asgari, Marika, Bilicki, Maciej, Heymans, Catherine, Hildebrandt, Hendrik, Kuijken, Konrad, Wietersheim-Kramsta, Maximilian Von, Sub String Theory Cosmology and ElemPart, Theoretical Physics, Sub String Theory Cosmology and ElemPart, and Theoretical Physics

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, Measure (mathematics), Luminosity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, weak [ravitational lensing], Astrophysics::Galaxy Astrophysics, Physics, COSMIC cancer database, Astrophysics of Galaxies, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, observations [cosmology], Observations Large-Scale Structure of Universe Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, Gravitational Lensing: Weak Cosmology, ravitational lensing: weak, large-scale structure of Universe, Linear growth, Cosmology and Nongalactic Astrophysics, Data release, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We constrain the luminosity and redshift dependence of the intrinsic alignment (IA) of a nearly volume-limited sample of luminous red galaxies selected from the fourth public data release of the Kilo-Degree Survey (KiDS-1000). To measure the shapes of the galaxies, we used two complementary algorithms, finding consistent IA measurements for the overlapping galaxy sample. The global significance of IA detection across our two independent luminous red galaxy samples, with our favoured method of shape estimation, is $\sim10.7\sigma$. We find no significant dependence with redshift of the IA signal in the range $0.2, Comment: 21 pages, 14 figures. Accepted for publication in A&A

Published
2021

5. KiDS+VIKING-450 and DES-Y1 combined: Cosmology with cosmic shear

Subjects
galaxies: photometry, gravitational lensing: weak, surveys, cosmology: observations, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

We present a combined tomographic weak gravitational lensing analysis of the Kilo Degree Survey (KV450) and the Dark Energy Survey (DES-Y1). We homogenize the analysis of these two public cosmic shear datasets by adopting consistent priors and modeling of nonlinear scales, and determine new redshift distributions for DES-Y1 based on deep public spectroscopic surveys. Adopting these revised redshifts results in a 0.8σ reduction in the DES-inferred value for S​8, which decreases to a 0.5σ reduction when including a systematic redshift calibration error model from mock DES data based on the MICE2 simulation. The combined KV450+DES-Y1 constraint on S8 = 0.762−0.024+0.025 is in tension with the Planck 2018 constraint from the cosmic microwave background at the level of 2.5σ. This result highlights the importance of developing methods to provide accurate redshift calibration for current and future weak-lensing surveys.

Published
2020

6. KiDS+VIKING-450

Author

A. H. Wright, Christopher B. Morrison, Hendrik Hildebrandt, Ami Choi, Peter Schneider, Benjamin Giblin, Thomas Erben, Alexandra Amon, Mario Radovich, Cristóbal Sifón, F. Köhlinger, S. Brieden, Lance Miller, John A. Peacock, Catherine Heymans, Marika Asgari, Tilman Tröster, Henk Hoekstra, Chris Blake, Alexander Mead, J. L. van den Busch, Benjamin Joachimi, Arun Kannawadi, Maria Archidiacono, J. T. A. de Jong, Shahab Joudaki, Konrad Kuijken, M. Tewes, European Commission, German Research Foundation, Alexander von Humboldt Foundation, Ministry of Education, Culture, Sports, Science and Technology (Japan), Max Planck Society, Federal Ministry of Education and Research (Germany), and Kapteyn Astronomical Institute

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, 01 natural sciences, symbols.namesake, Gravitational lensing: weak, 0103 physical sciences, Planck, observations [Cosmology], 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, COSMIC cancer database, 010308 nuclear & particles physics, photometry [Galaxies], Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxies: photometry, Redshift, Galaxy, photometry / surveys [galaxies], Space and Planetary Science, astro-ph.CO, symbols, Dark energy, Neutrino, weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a tomographic cosmic shear analysis of the Kilo-Degree Survey (KiDS) combined with the VISTA Kilo-Degree Infrared Galaxy Survey (VIKING). This is the first time that a full optical to near-infrared data set has been used for a wide-field cosmological weak lensing experiment. This unprecedented data, spanning $450~$deg$^2$, allows us to improve significantly the estimation of photometric redshifts, such that we are able to include robustly higher-redshift sources for the lensing measurement, and - most importantly - solidify our knowledge of the redshift distributions of the sources. Based on a flat $\Lambda$CDM model we find $S_8\equiv\sigma_8\sqrt{\Omega_{\rm m}/0.3}=0.737_{-0.036}^{+0.040}$ in a blind analysis from cosmic shear alone. The tension between KiDS cosmic shear and the Planck-Legacy CMB measurements remains in this systematically more robust analysis, with $S_8$ differing by $2.3\sigma$. This result is insensitive to changes in the priors on nuisance parameters for intrinsic alignment, baryon feedback, and neutrino mass. KiDS shear measurements are calibrated with a new, more realistic set of image simulations and no significant B-modes are detected in the survey, indicating that systematic errors are under control. When calibrating our redshift distributions by assuming the 30-band COSMOS-2015 photometric redshifts are correct (following the Dark Energy Survey and the Hyper Suprime-Cam Survey), we find the tension with Planck is alleviated. The robust determination of source redshift distributions remains one of the most challenging aspects for future cosmic shear surveys., Comment: 31 pages, 14 figures, accepted for publication by A&A; data products available at http://kids.strw.leidenuniv.nl

Published
2020

8. The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release

Author

Shrinivas R. Kulkarni, Kunal Mooley, Julie Banfield, G. Zamorani, Mark Sargent, Frank Bertoldi, Sarah K. Leslie, Stephen Bourke, Eric J. Murphy, N. Baran, F. Navarrete, Eva Schinnerer, H. J. McCracken, Mladen Novak, Ivan Delvecchio, J. Delhaize, Alexander Karim, E. Middleberg, Vibor Jelić, Peter Capak, Gregg Hallinan, Dale A. Frail, Clotilde Laigle, Eleni Vardoulaki, Heng Hao, Mislav Baloković, Chris Carilli, H. R. Kloeckner, Nick Scoville, J. Krpan, Huib Intema, O. Ilbert, Kartik Sheth, Steven T. Myers, Paolo Ciliegi, M. Bondi, Vernesa Smolčić, Oskari Miettinen, Assaf Horesh, N. Herrera Ruiz, 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), 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), and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, Spectral shape analysis, PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, Monte Carlo method, AZTEC MILLIMETER SURVEY, FOS: Physical sciences, Astrophysics, 01 natural sciences, Jansky, 0103 physical sciences, LARGE-SCALE STRUCTURE, RADIO SPECTRAL INDEX, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, atalogs, cosmology: observations, radio continuum: galaxies, Source counts, 010303 astronomy & astrophysics, Very Long Baseline Array, QB, Physics, LEGACY SURVEY, Spectral index, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, 20 CM, POINT-SOURCE CATALOG, PHOENIX DEEP SURVEY, Astronomy and Astrophysics, Astrometry, STAR-FORMATION HISTORY, Astrophysics - Astrophysics of Galaxies, observations [cosmology], galaxies [radio continuum], Square degree, SOURCE POPULATION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), catalogs
Abstract

We present the VLA-COSMOS 3 GHz Large Project based on 384 hours of observations with the Karl G. Jansky Very Large Array (VLA) at 3 GHz (10 cm) toward the two square degree Cosmic Evolution Survey (COSMOS) field. The final mosaic reaches a median rms of 2.3 uJy/beam over the two square degrees at an angular resolution of 0.75". To fully account for the spectral shape and resolution variations across the broad (2 GHz) band, we image all data with a multiscale, multifrequency synthesis algorithm. We present a catalog of 10,830 radio sources down to 5 sigma, out of which 67 are combined from multiple components. Comparing the positions of our 3 GHz sources with those from the Very Long Baseline Array (VLBA)-COSMOS survey, we estimate that the astrometry is accurate to 0.01" at the bright end (signal-to-noise ratio, S/N_3GHz > 20). Survival analysis on our data combined with the VLA-COSMOS 1.4~GHz Joint Project catalog yields an expected median radio spectral index of alpha=-0.7. We compute completeness corrections via Monte Carlo simulations to derive the corrected 3 GHz source counts. Our counts are in agreement with previously derived 3 GHz counts based on single-pointing (0.087 square degrees) VLA data. In summary, the VLA-COSMOS 3 GHz Large Project simultaneously provides the largest and deepest radio continuum survey at high (0.75") angular resolution to date, bridging the gap between last-generation and next-generation surveys., 19 pages, 18 figures, 5 tables, accepted for publication in A&A

Published
2017

23. Planck 2013 results

Author

Tauber, Jan, Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Chamballu, A., Chiang, L. Y., Christensen, P. R., Church, S., Colombi, S., Colombo, L. P. L., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dick, J., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Gaier, T. C., Galeotta, S., Ganga, K., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Kangaslahti, P., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Paci, F., Pagano, L., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, D., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Ricciardi, S., Riller, T., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubinõ Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, R., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A., Universidad de Cantabria, Tauber, Jan, Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Chamballu, A., Chiang, L. Y., Christensen, P. R., Church, S., Colombi, S., Colombo, L. P. L., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dick, J., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Gaier, T. C., Galeotta, S., Ganga, K., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Kangaslahti, P., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Paci, F., Pagano, L., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, D., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Ricciardi, S., Riller, T., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubinõ Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, R., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A., Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), 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), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), PLANCK, University of Paris, University of Oxford, University of Paris Diderot, Kavli Institute for Cosmology, University of Salamanca, International School for Advanced Studies, Université de Toulouse, University of Granada, Pierre and Marie Curie University, California Institute of Technology, Istituto Nazionale Astrofisica - Italy, University of Manchester, University of Toronto, University of California Berkeley, Telecom ParisTech, Université Grenoble Alpes, Academia Sinica - Institute of Astronomy and Astrophysics, Niels Bohr Institute, University of Copenhagen, Stanford University, Sapienza University of Rome, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, Department of Physics, Helsinki Institute of Physics, Hélium : du fondamental aux applications (NEEL - HELFA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université 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), École normale supérieure - Paris (ENS-PSL), 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), 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), 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), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)

Subjects
Calibration (statistics), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Cosmic microwave background, data analysis, Astrophysics, cosmic background radiation, Residual, Cosmic background radiation, 7. Clean energy, 01 natural sciences, MAPS, Range (statistics), RADIOMETERS, 010303 astronomy & astrophysics, Cosmology: observations, Methods: data analysis, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science::Computers and Society, observations [cosmology], PLANCK, Physics::Space Physics, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], education, FOS: Physical sciences, observation [Cosmology], Computer Science::Digital Libraries, NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, data analysis [methods], Planck, Spurious relationship, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, Spectral density, PERFORMANCE, Astronomy and Astrophysic, 115 Astronomy, Space science, Computational physics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], data analysi [Methods], 13. Climate action, Multipole expansion, SKY, cosmology
Abstract

© 2014 ESO. We present the current estimate of instrumental and systematic effect uncertainties for the Planck-Low Frequency Instrument relevant to the first release of the Planck cosmological results. We give an overview of the main effects and of the tools and methods applied to assess residuals in maps and power spectra. We also present an overall budget of known systematic effect uncertainties, which are dominated by sidelobe straylight pick-up and imperfect calibration. However, even these two effects are at least two orders of magnitude weaker than the cosmic microwave background fluctuations as measured in terms of the angular temperature power spectrum. A residual signal above the noise level is present in the multipole range â.,> < 20, most notably at 30 GHz, and is probably caused by residual Galactic straylight contamination. Current analysis aims to further reduce the level of spurious signals in the data and to improve the systematic effects modelling, in particular with respect to straylight and calibration uncertainties., 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 and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).

Published
2014

24. Planck 2013 results

Author

Jérôme Bobin, Davide Maino, M. Frailis, Carlo Baccigalupi, E. Hivon, Luigi Danese, A. Chamballu, J.-F. Sygnet, D. J. Marshall, Simon D. M. White, Luca Terenzi, Luca Valenziano, Ben Rusholme, D. Yvon, C. Hernández-Monteagudo, E. P. S. Shellard, S. Ricciardi, D. Herranz, M. Sandri, Jussi-Pekka Väliviita, G. Patanchon, F. Paci, Jörg P. Rachen, C. Renault, A. Mennella, Nabila Aghanim, Bruno Maffei, Reijo Keskitalo, Nicola Bartolo, F. Pajot, Alessandro Melchiorri, Jacques Delabrouille, E. Martínez-González, J. A. Murphy, R. A. Sunyaev, A.-S. Suur-Uski, Alan Heavens, M. Piat, Peter Meinhold, A. Curto, M. Tucci, N. Mandolesi, Charles R. Lawrence, Julien Lesgourgues, Andrew H. Jaffe, Philip Lubin, Kendrick M. Smith, F. Pasian, James R. Fergusson, René J. Laureijs, J. González-Nuevo, M. Bridges, O. Perdereau, Fabio Finelli, S. Donzelli, Michael P. Hobson, James G. Bartlett, P. Vielva, Marian Douspis, W. A. Holmes, Marcella Massardi, R. C. Butler, B. Racine, K. Ganga, A. Renzi, Krzysztof M. Gorski, Allan Hornstrup, A. Coulais, Davide Pietrobon, W. Hovest, Andrea Zacchei, L. Mendes, Sabino Matarrese, Olivier Forni, M.-A. Miville-Deschênes, Jose Alberto Rubino-Martin, M. Tristram, Etienne Pointecouteau, Jose M. Diego, Domenico Marinucci, Adam Moss, Anthony Challinor, I. D. Novikov, D. Tavagnacco, D. L. Harrison, G. de Zotti, G. Polenta, M. Linden-Vørnle, Sarah E. Church, Theodore Kisner, G. Prézeau, Giorgio Savini, Hiranya V. Peiris, J. Tuovinen, B. Van Tent, F. K. Hansen, Rafael Rebolo, Calvin B. Netterfield, A. Catalano, P. R. Christensen, H. Dole, Subhabrata Mitra, J. A. Tauber, L. Perotto, M. Maris, Silvia Masi, S. R. Hildebrandt, Carlo Burigana, L. Montier, Andrea Zonca, A. Gregorio, M. Tomasi, A. J. Banday, Peter A. R. Ade, S. Colombi, F. Couchot, N. Ponthieu, Michele Liguori, F. Piacentini, H. C. Chiang, E. Franceschi, A. Moneti, Jean-Luc Starck, P. de Bernardis, J. P. Leahy, R. D. Davies, P. B. Lilje, Jean-François Cardoso, Marco Bersanelli, Guilaine Lagache, A. Benoit-Lévy, C. Rosset, François R. Bouchet, M. Giard, F. Noviello, Kevin M. Huffenberger, Francesca Perrotta, Torsten A. Enßlin, Joanna Dunkley, J.-P. Bernard, K. Benabed, M. Ashdown, M. López-Caniego, H. K. Eriksen, B. P. Crill, Lung-Yih Chiang, T. Riller, Anne Lähteenmäki, F. Elsner, Laura Bonavera, R. V. Sudiwala, J. Aumont, J. F. Macías-Pérez, X. Dupac, L. Popa, J. R. Bond, Daniel J. Mortlock, Antony Lewis, Fabrizio Villa, S. Galeotta, Benjamin D. Wandelt, Julian Borrill, Stéphane Plaszczynski, E. Pierpaoli, R. Leonardi, Nicola Vittorio, Graca Rocha, C. Armitage-Caplan, R. B. Barreiro, Radek Stompor, Serge Gratton, Pasquale Mazzotta, F.-X. Désert, L. P. L. Colombo, J.-M. Delouis, W. C. Jones, Fernando Atrio-Barandela, Anna Mangilli, J.-L. Puget, Dmitry Novikov, Mika Juvela, L. A. Wade, T. Poutanen, Daniela Paoletti, A. Ducout, Dipak Munshi, George Efstathiou, Michael Seiffert, F. Matthai, Duncan Hanson, Martin White, M. Bucher, Douglas Scott, G. W. Pratt, F. Cuttaia, Gianluca Morgante, James J. Bock, Paul M. Sutter, Anna Bonaldi, D. Santos, T. R. Jaffe, M. Migliaccio, Sophie Henrot-Versille, Paolo Natoli, Y. Giraud-Héraud, I. Ristorcelli, F. Lacasa, Monique Arnaud, Hans Ulrik Nørgaard-Nielsen, Peter G. Martin, E. Battaner, Pavel Naselsky, R. J. Davis, Jussi Varis, Olivier Doré, L. Toffolatti, Anthony Lasenby, E. Keihänen, Alain Benoit, Alessandro Gruppuso, J.-M. Lamarre, S. Osborne, D. Sutton, F. Sureau, A. de Rosa, Hannu Kurki-Suonio, Lloyd Knox, Locke D. Spencer, David L. Clements, J. Knoche, Simon Prunet, P. Bielewicz, G. Roudier, Carol Anne Oxborrow, M. Reinecke, V. Stolyarov, Martin Kunz, Mathieu Remazeilles, L. Pagano, Anne Lähteenmäki Group, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Institut Néel (NEEL), 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), AstroParticule et Cosmologie (APC (UMR_7164)), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, PLANCK, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), 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), 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), 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), Tauber, Jan, Ade, P. A. R., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Challinor, A., Chamballu, A., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dunkley, J., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Heavens, A., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lacasa, F., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Lewis, A., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., MacIás Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mangilli, A., Marinucci, D., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Peiris, H. V., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Racine, B., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rubinõ Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Smith, K., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutter, P., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, M., White, S. D. M., Yvon, D., Zacchei, A., Zonca, A., Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Department of Physics, and Helsinki Institute of Physics

Subjects
POINT SOURCES, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Cosmic microwave background, data analysis, POLARIZATION ANISOTROPIES, Astrophysics, cosmic background radiation, 7. Clean energy, OBSERVATIONS COSMOLOGICAL INTERPRETATION, cosmology: theory, 3-POINT CORRELATION-FUNCTION, Statistical physics, QB, Physics, theory [cosmology], Astrophysics::Instrumentation and Methods for Astrophysics, Estimator, early Universe, Computer Science::Computers and Society, observations [cosmology], Physics::Space Physics, Physical Sciences, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, COMPONENT SEPARATION, Cosmology and Nongalactic Astrophysics (astro-ph.CO), education, Cosmic background radiation, MINKOWSKI FUNCTIONALS, FOS: Physical sciences, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, cosmic background radiation / cosmology: observations / cosmology: theory / early Universe / inflation / methods: data analysis, Computer Science::Digital Libraries, NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Non-Gaussianity, MICROWAVE BACKGROUND BISPECTRUM, LARGE-SCALE STRUCTURE, data analysis [methods], NONLINEAR COUPLING PARAMETER, Planck, inflation, Inflation (cosmology), Science & Technology, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, methods: data analysis, Ekpyrotic universe, Settore MAT/06 - Probabilita' e Statistica Matematica, data analysi [Methods], Cosmology: observations, Cosmology: theory, Early Universe, Inflation, Methods: data analysis, 13. Climate action, Space and Planetary Science, cosmology: observations, PROBE WMAP OBSERVATIONS, Bispectrum, cosmology
Abstract

The Planck nominal mission cosmic microwave background (CMB) maps yield unprecedented constraints on primordial non-Gaussianity (NG). Using three optimal bispectrum estimators, separable template-fitting (KSW), binned, and modal, we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result fNLlocal = 2.7 ± 5.8, fNLequil = -42 ± 75, and fNLorth = -25 ± 39 (68% CL statistical). Non-Gaussianity is detected in the data; using skew-Cl statistics we find a nonzero bispectrum from residual point sources, and the integrated-Sachs-Wolfe-lensing bispectrum at a level expected in the ?CDM scenario. The results are based on comprehensive cross-validation of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of tests, and are confirmed by skew-Cl, wavelet bispectrum and Minkowski functional estimators. Beyond estimates of individual shape amplitudes, we present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and thus derive constraints on early-Universe scenarios that generate primordial NG, including general single-field models of inflation, excited initial states (non-Bunch-Davies vacua), and directionally-dependent vector models. We provide an initial survey of scale-dependent feature and resonance models. These results bound both general single-field and multi-field model parameter ranges, such as the speed of sound, cs ≥ 0.02 (95% CL), in an effective field theory parametrization, and the curvaton decay fraction rD ≥ 0.15 (95% CL). The Planck data significantly limit the viable parameter space of the ekpyrotic/cyclic scenarios. The amplitude of the four-point function in the local model τNL< 2800 (95% CL). Taken together, these constraints represent the highest precision tests to date of physical mechanisms for the origin of cosmic structure., 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 and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).

Published
2014

27. Planck 2013 results

Author

T. Poutanen, Olivier Doré, K. Ganga, O. Perdereau, Peter A. R. Ade, Jose M. Diego, Krzysztof M. Gorski, V. Stolyarov, Y. Giraud-Héraud, E. Franceschi, I. Ristorcelli, Martin Kunz, Duncan Hanson, P. R. Christensen, C. Hernández-Monteagudo, P. M. McGehee, Mathieu Remazeilles, Anthony Lasenby, L. Sanselme, Monique Arnaud, Charles R. Lawrence, Jon E. Gudmundsson, L. Pagano, S. Galeotta, F. Piacentini, E. Keihänen, W. Hovest, F. Melot, William T. Reach, Guilaine Lagache, Jean-François Cardoso, Francesca Perrotta, L. Perotto, Allan Hornstrup, George Helou, Etienne Pointecouteau, M. López-Caniego, Alessandro Melchiorri, Kevin M. Huffenberger, Alain Benoit, D. L. Harrison, R. Leonardi, Michele Liguori, Theodore Kisner, Hans Ulrik Nørgaard-Nielsen, C. North, C. Leroy, M. Maris, N. Ponthieu, A. de Rosa, R.-R. Chary, Jo Dunkley, M. Tucci, Stéphane Colombi, J. J. Bock, M. Ashdown, Pavel Naselsky, R. J. Davis, Andrea Zacchei, H. K. Eriksen, Francine R. Marleau, J. W. Bowyer, Fabrizio Villa, M. Bridges, M. Tomasi, F. Cuttaia, W. A. Holmes, B. Racine, A. Chamballu, Torsten A. Enßlin, Locke D. Spencer, Olivier Forni, J. Aumont, S. R. Hildebrandt, A. Benoit-Lévy, Daniel J. Mortlock, M.-A. Miville-Deschênes, M. Giard, E. Pierpaoli, Aurelien A. Fraisse, M. Frailis, Carlo Baccigalupi, E. Hivon, S. Techene, S. Mottet, P. B. Lilje, D. Sutton, W. C. Jones, F. K. Hansen, J. Knoche, Marco Bersanelli, Roberta Paladini, Simon Prunet, Carlo Burigana, Simon D. M. White, P. Bielewicz, B. P. Crill, Lung-Yih Chiang, S. Donzelli, D. Girard, A. Curto, Peter G. Martin, François R. Bouchet, Serge Gratton, A. Sauvé, F.-X. Désert, J. Bobin, G. W. Pratt, D. Herranz, M. Le Jeune, D. Yvon, Michael Rowan-Robinson, Nicola Vittorio, L. P. L. Colombo, F. Matthai, C. Armitage-Caplan, Giorgio Savini, A. Catalano, Gianluca Morgante, T. Riller, Dmitry Novikov, Bruno Maffei, Clive Dickinson, Xin Chen, J.-L. Puget, Pasquale Mazzotta, J.-F. Sygnet, Stéphane Plaszczynski, L. Vibert, X. Dupac, Carol Anne Oxborrow, M. Reinecke, Davide Pietrobon, E. Battaner, L. A. Wade, Daniela Paoletti, F. Pajot, Reijo Keskitalo, M. Bucher, Douglas Scott, Luigi Danese, Dipak Munshi, George Efstathiou, L. Popa, Ben Rusholme, P. Vielva, D. Santos, A. Mennella, Nabila Aghanim, Luca Valenziano, A. Coulais, F. Atrio-Barandela, Calvin B. Netterfield, G. Giardino, T. R. Jaffe, O. Herent, Marcella Massardi, R. Kneissl, Jacques Delabrouille, François Orieux, J.-M. Delouis, M. Migliaccio, N. Mandolesi, J. A. Murphy, A. Moneti, Radek Stompor, Federico Nati, E. P. S. Shellard, Luca Terenzi, C. Combet, Andrew H. Jaffe, G. Umana, G. de Zotti, René J. Laureijs, Mika Juvela, F. Boulanger, Jussi-Pekka Väliviita, G. Patanchon, F. Couchot, I. D. Novikov, Philip Lubin, Fabio Finelli, Peter Meinhold, F. Paci, Sophie Henrot-Versille, Alessandro Gruppuso, Z. Hou, R. D. Davies, F. Noviello, J. González-Nuevo, G. Prézeau, Paolo Natoli, Andrea Zonca, K. Benabed, A. Gregorio, Marian Douspis, H. C. Chiang, J. R. Bond, Michael P. Hobson, Franck Sureau, B. Van Tent, J.-M. Lamarre, L. Mendes, S. Osborne, A. J. Banday, A.-S. Suur-Uski, Sabino Matarrese, H. Dole, Subhabrata Mitra, J. A. Tauber, Hannu Kurki-Suonio, J. Lesgourgues, G. Hurier, C. J. MacTavish, Lloyd Knox, David L. Clements, G. Roudier, P. de Bernardis, C. Rosset, Silvia Masi, Jean-Luc Starck, D. J. Marshall, J. F. Macías-Pérez, Graca Rocha, L. Montier, F. Pasian, J.-P. Bernard, Benjamin D. Wandelt, M. Tristram, Julian Borrill, G. Polenta, M. Linden-Vørnle, Sarah E. Church, E. Martínez-González, M. Piat, D. Tavagnacco, Rafael Rebolo, R. B. Barreiro, R. Sudiwala, S. Ricciardi, Jörg P. Rachen, C. Renault, Tauber, Jan, Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cappellini, B., Cardoso, J. F., Catalano, A., Chamballu, A., Chen, X., Chiang, L. Y., Christensen, P. R., Church, S., Colombi, S., Colombo, L. P. L., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falvella, M. C., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Gaier, T. C., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Kangaslahti, P., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lattanzi, M., Laureijs, R. J., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lubin, P. M., MacIás Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Moneti, A., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Moss, A., Munshi, D., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Paci, F., Pagano, L., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Ricciardi, S., Riller, T., Robbers, G., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubinõ Martín, J. A., Rusholme, B., Salerno, E., Sandri, M., Santos, D., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., White, S. D. M., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A., Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, 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)-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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), 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), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), PLANCK, Universidad de Cantabria, Hélium : du fondamental aux applications (NEEL - HELFA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), École normale supérieure - Paris (ENS-PSL), 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), 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), Anne Lähteenmäki Group, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, HELFA - Hélium : du fondamental aux applications, Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Department of Physics, and Helsinki Institute of Physics

Subjects
Astronomy, Cosmic microwave background, data analysis, Astrophysics, cosmic background radiation, Surveys, Cosmic background radiation, NOISE, RADIOMETERS, data analysis [Methods], observations [Cosmology], Survey, cosmology: observations, surveys [cosmic background radiation, methods], Physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science::Computers and Society, DATA SETS, Physics::Space Physics, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Astrophysics and Astronomy, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], education, FOS: Physical sciences, observation [Cosmology], Computer Science::Digital Libraries, NO, Settore FIS/05 - Astronomia e Astrofisica, surveys, Calibration, PRE-LAUNCH STATUS, Angular resolution, Instrumentation and Methods for Astrophysics (astro-ph.IM), methods: data analysis, Radiometer, MAP-MAKING ALGORITHM, Instrument Data, Spectral density, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, Cosmology: observations, Methods: data analysis, Space and Planetary Science, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], data analysi [Methods], cosmology
Abstract

We describe the data processing pipeline of the Planck Low Frequency Instrument (LFI) data processing centre (DPC) to create and characterize full-sky maps based on the first 15.5 months of operations at 30, 44, and 70 GHz. In particular, we discuss the various steps involved in reducing the data, from telemetry packets through to the production of cleaned, calibrated timelines and calibrated frequency maps. Data are continuously calibrated using the modulation induced on the mean temperature of the cosmic microwave background radiation by the proper motion of the spacecraft. Sky signals other than the dipole are removed by an iterative procedure based on simultaneous fitting of calibration parameters and sky maps. Noise properties are estimated from time-ordered data after the sky signal has been removed, using a generalized least squares map-making algorithm. A destriping code (Madam) is employed to combine radiometric data and pointing information into sky maps, minimizing the variance of correlated noise. Noise covariance matrices, required to compute statistical uncertainties on LFI and Planck products, are also produced. Main beams are estimated down to the ≈−20 dB level using Jupiter transits, which are also used for the geometrical calibration of the focal plane., This work was supported by the Academy of Finland grants 253204, 256265, and 257989. We acknowledge financial support provided by the Spanish Ministerio de Ciencia e Innovaciõn through the Plan Nacional del Espacio y Plan Nacional de Astronomia y Astrofisica. 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 and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).

Published
2014

29. X-ray observations and mass determinations in the cluster of galaxies Cl0024+17

Author

Soucail, G., Ota, N., Bohringer, H., Czoske, O., Hattori, M., Mellier, Y., Laboratoire Astrophysique de Toulouse-Tarbes (LATT), 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), 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), Observatoire de Paris, and Université Paris sciences et lettres (PSL)

Subjects
X-RAYS: GALAXIES, COSMOLOGY: DARK MATTER, GALAXIES: CLUSTERS: GENERAL, [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, COSMOLOGY: OBSERVATIONS, Astrophysics (astro-ph), FOS: Physical sciences, GALAXIES: CLUSTERS: INDIVIDUAL: CL0024+17, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, COSMOLOGY: GRAVITATIONAL LENSING
Abstract

We present a detailed analysis of the mass distribution in the rich and distant cluster of galaxies Cl0024+17. X-ray data come from both a deep ROSAT/HRI image of the field (Bohringer et al. 1999) and ASCA spectral data. Using a wide field CCD image of the cluster, we optically identify all the faint X-ray sources, whose counts are compatible with deep X-ray number counts. In addition we marginally detect the X-ray counter-part of the gravitational shear perturbation detected by Bonnet et al. (1994) at a 2.5 $\sigma$ level. A careful spectral analysis of ASCA data is also presented. In particular, we extract a low resolution spectrum of the cluster free from the contamination by a nearby point source located 1.2 arcmin from the center. The X-ray temperature deduced from this analysis is $T_X = 5.7 ^{+4.9}_{-2.1}$ keV at the 90% confidence level. The comparison between the mass derived from a standard X-ray analysis and from other methods such as the Virial Theorem or the gravitational lensing effect lead to a mass discrepancy of a factor 1.5 to 3. We discuss all the possible sources of uncertainties in each method of mass determination and give some indications on the way to reduce them. A complementary study of optical data is in progress and may solve the X-ray/optical discrepancy through a better understanding of the dynamics of the cluster., Comment: Revised version, accepted in Astronomy and Astrophysics (Main Journal). Few changes in the discussion

Published
2000

30. Removal of two large-scale cosmic microwave background anomalies after subtraction of the integrated Sachs-Wolfe effect

Author

A. Rassat, Jean-Luc Starck, François-Xavier Dupé, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Laboratoire d'informatique Fondamentale de Marseille (LIF), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), and Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Inpainting, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, methods: statistical, 010308 nuclear & particles physics, Cosmology: observations, Subtraction, Astronomy and Astrophysics, early Universe, Sachs–Wolfe effect, Missing data, Galaxy, Planarity testing, Space and Planetary Science, large-scale structure of Universe, Cosmology: theory, Focus (optics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Though debated, the existence of claimed large-scale anomalies in the CMB is not totally dismissed. In parallel to the debate over their statistical significance, recent work focussed on masks and secondary anisotropies as potential sources of these anomalies. In this work we investigate simultaneously the impact of the method used to account for masked regions and the impact of the ISW effect, which is the large-scale secondary anisotropy most likely to affect the CMB anomalies. In this sense, our work is an update of both Francis & Peacock 2010 and Kim et al. 2012. Our aim is to identify trends in CMB data with different mask treatments. We reconstruct the ISW signal due to 2MASS and NVSS galaxies. We account for missing data using the sparse inpainting technique of Abrial et al. 2008 and sparse inpainting of the CMB, LSS and ISW and find that it constitutes a bias-free reconstruction method suitable to study large-scale statistical isotropy and the ISW effect. We focus on three large-scale CMB anomalies: the low quadrupole, the quad/oct alignment, and the octopole planarity. After sparse inpainting, the low quadrupole becomes more anomalous, whilst the quad/oct alignment becomes less anomalous. The significance of the low quadrupole is unchanged after subtraction of the ISW effect, while the trend is that the quad/oct alignment has reduced significance, yet other hypotheses remain possible as well (e.g. exotic physics). Our results also suggest that both of these anomalies may be due to the quadrupole alone. The octopole planarity significance is also reduced after inpainting and after ISW subtraction, however, we do not find that it was very anomalous to start with. In the spirit of reproducible research, we make all codes and resulting products which constitute main results of this paper public here: http://www.cosmostat.org/anomaliesCMB.html., Updated Figs 4-6, A.5, and Tables 2-6. Main conclusions unchanged, except low quadrupole is still low after ISW subtraction. Accepted for publication in A&A. In the spirit of reproducible research, all codes and resulting products which constitute main results of this paper are made public here: http://www.cosmostat.org/anomaliesCMB.html. Table 6 is the overall summary. Astro-ph abstract abridged

Published
2013
Full Text
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32. Planck early results. XII

Author

Poutanen, T., Natoli, P., Polenta, G., Bartlett, J.G., Bucher, M., Cardoso, J.-F., Catalano, A., Delabrouille, J., Fromenteau, S., Ganga, K., Giraud-Héraud, Y., Patanchon, G., Piat, M., Rosset, C., Smoot, G.F., Ashdown, M., Brown, M.L., Chon, G., Hobson, M., Lasenby, A., Stolyarov, V., Bhatia, R., Kneissl, R., Bond, J.R., Miville-Deschênes, M.-A., Banday, A.J., Bernard, J.-P., Forni, O., Giard, M., Montier, L., Pointecouteau, E., Ristorcelli, I., Bock, J.J., Doré, O., Hildebrandt, S.R., Mei, S., Prézeau, G., Rocha, G., Seiffert, M.D., Dahle, H., Da Silva, A., Challinor, A., Shellard, P., Melin, J.-B., Piffaretti, R., Starck, J.-L., Yvon, D., Linden-Vørnle, Michael, Nørgaard-Nielsen, Hans Ulrik, Toffolatti, L., Marleau, F., Netterfield, C.B., Scott, D., Pierpaoli, E., Juvela, M., Keihänen, E., Keskitalo, R., Kurki-Suonio, H., Chiang, C., Jones, W.C., Cayón, L., White, M., Knox, L., Leonardi, R., Lubin, P.M., Zonca, A., Wandelt, B.D., Matarrese, S., De Bernardis, P., Masi, S., Melchiorri, A., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Tomasi, M., Gregorio, A., Balbi, A., Cabella, P., De Gasperis, G., Mazzotta, P., Vittorio, N., Christensen, P.R., Naselsky, P., Flores-Cacho, I., Génova-Santos, R.T., Rebolo, R., Rubiño-Martín, J.A., Dupac, X., Mendes, L., Giardino, G., Laureijs, R.J., Tauber, J.A., Bonaldi, A., De Zotti, G., Colafrancesco, S., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Zacchei, A., Burigana, C., Cuttaia, F., De Rosa, A., Finelli, F., Franceschi, E., Gruppuso, A., Mandolesi, N., Morgante, G., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Donzelli, S., Stivoli, F., Désert, F.-X., Chamballu, A., Clements, D.L., Jaffe, A.H., Mortlock, D., Novikov, D., Rusholme, B., Benoît, A., Aghanim, N., Aumont, J., Douspis, M., Lagache, G., Noviello, F., Pajot, F., Ponthieu, N., Puget, J.-L., Torre, J.-P., Vibert, L., Benabed, K., Bouchet, F.R., Colombi, S., Delouis, J.-M., Hivon, E., Moneti, A., Prunet, S., Sygnet, J.-F., Chiang, L.-Y., Efstathiou, G., Gratton, S., Harrison, D., Munshi, D., Hoyland, R.J., Barreiro, R.B., Diego, J.M., Herranz, D., López-Caniego, M., Martínez-González, E., Vielva, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Mitra, S., O'Dwyer, I.J., Davis, R.J., Maffei, B., MacTavish, C.J., Coulais, A., Lamarre, J.-M., Arnaud, M., Pratt, G.W., MacÍas-Pérez, J.F., Perotto, L., Renault, C., Couchot, F., Henrot-Versillé, S., Perdereau, O., Plaszczynski, S., Tristram, M., Borrill, J., Kisner, T.S., Bartelmann, M., Churazov, E., Dolag, K., Dörl, U., Enßlin, T.A., Hernández-Monteagudo, C., Hovest, W., Matthai, F., Reinecke, M., Riller, T., Sunyaev, R., White, S.D.M., Tuovinen, J., Murphy, A., Novikov, I., Savini, G., Baccigalupi, C., Danese, L., González-Nuevo, J., Leach, S., Perrotta, F., Mann, R., Sudiwala, R., Osborne, S., Schaefer, B.M., Battaner, E., Huffenberger, K.M., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartelmann, M., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. P., Bersanelli, M., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Finelli, F., Flores, I., Forni, O., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova Santos, R. T., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Harrison, D., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Linden Vornle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Mactavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Mei, S., Melchiorri, A., Melin, J. B., Mendes, L., Mennella, A., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Norgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. P., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., White, S. D. M., White, M., Yvon, D., Zacchei, A., Zonca, A., Department of Physics, Helsinki Institute of Physics, APC - Cosmologie, 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)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), APC - Gravitation (APC-Gravitation), 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), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PLANCK, Universidad de Cantabria, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), 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), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), 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), 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
Experimental Physics, Large-scale structure of Universe, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics, clusters: general [Galaxies], Cosmic background radiation, 01 natural sciences, Power law, CMB physic, CMB physics, clusters, observations [Cosmology], 010303 astronomy & astrophysics, intracluster medium, media_common, Physics, Planck ESA mission, Cosmology, observations, galaxies: clusters: general, cosmic backround radiation, symbols, large-scale structure of Universe, Galaxies: clusters: intracluster medium, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, education, Galaxies, general, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: intracluster medium [Galaxies], Measure (mathematics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, galaxies: clusters: intracluster medium – cosmic background radiation – large-scale structure of Universe – cosmology: observations – galaxies: clusters: general, Settore FIS/05 - Astronomia e Astrofisica, galaxies: clusters: intracluster medium, galaxies, cosmology: observations, cosmic background radiation, cosmology, large-scale structure of universe, 0103 physical sciences, Cluster (physics), Galaxy formation and evolution, clusters: intracluster medium – cosmic background radiation – large-scale structure of Universe – cosmology: observations – galaxies: clusters: general [galaxies], Planck, Scaling, 010308 nuclear & particles physics, Matched filter, Astronomy and Astrophysics, 115 Astronomy, Space science, Space and Planetary Science, Sky
Abstract

10 páginas, 6 figuras, 2 tablas.-- Planck Collaboration: et al., We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling relation (Y500 − N200) for the MaxBCG cluster catalogue. Employing a multi-frequency matched filter on the Planck sky maps, we measure the SZ signal for each cluster by adapting the filter according to weak-lensing calibrated mass-richness relations (N200 − M500). We bin our individual measurements and detect the SZ signal down to the lowest richness systems (N200 = 10) with high significance, achieving a detection of the SZ signal in systems with mass as low as M500 ≈ 5 × 1013 M⊙. The observed Y500 − N200 relation is well modeled by a power law over the full richness range. It has a lower normalisation at given N200 than predicted based on X-ray models and published mass-richness relations. An X-ray subsample, however, does conform to the predicted scaling, and model predictions do reproduce the relation between our measured bin-average SZ signal and measured bin-average X-ray luminosities. At fixed richness, we find an intrinsic dispersion in the Y500 − N200 relation of 60% rising to of order 100% at low richness. Thanks to its all-sky coverage, Planck provides observations for more than 13000 MaxBCG clusters and an unprecedented SZ/optical data set, extending the list of known cluster scaling laws to include SZ-optical properties. The data set offers essential clues for models of galaxy formation. Moreover, the lower normalisation of the SZ-mass relation implied by the observed SZ-richness scaling has important consequences for cluster physics and cosmological studies with SZ clusters.

Published
2011

34. Planck early results. XVIII

Author

Planck, Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoit, A., Bernard, J. P., Bersanelli, M., Bhatia, R., Blagrave, K., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Cabella, Paolo, Cardoso, J. F., Catalano, Andrea, Cayon, L., Challinor, A., Chamballu, A., Chiang, L. Y., Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., DE BERNARDIS, Paolo, De Gasperis, G., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Desert, F. X., Dole, H., Donzelli, S., Dore, O., Dorl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud Heraud, Y., Gonzalez Nuevo, J., Gorski, K. M., Grain, J., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Helou, G., Henrot Versille, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Leroy, C., Lilje, P. B., Linden Vørnle, M., Linden Vornle, M., Lockman, F. J., Lopez Caniego, M., Lubin, P. M., Macias Perez, J. F., Mactavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martin, P., Martinez Gonzalez, E., Masi, Silvia, Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, Alessandro, Mendes, L., Mennella, A., Mitra, S., Miville Deschenes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Norgaard Nielsen, H. U., Novikov, D., Novikov, I., O'Dwyer, I. J., Oliver, S., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, Francesco, Piat, M., Goncalves, D. P., Pinheiro Goncalves, D., Plaszczynski, S., Pointecouteau, E., Polenta, Gianluca, Ponthieu, N., Poutanen, T., Prezeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, Sara, Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan Robinson, M., Rubino Martin, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, Giorgio, Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. L., Stivoli, Federico, Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, M., Yvon, D., Zacchei, A., Zonca, A., Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoit, A., Bernard, J. P., Bersanelli, M., Bhatia, R., Blagrave, K., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. F., Catalano, A., Cayon, L., Challinor, A., Chamballu, A., Chiang, L. Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. M., Desert, F. X., Dole, H., Donzelli, S., Dore, O., Dorl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud Heraud, Y., Gonzalez Nuevo, J., Gorski, K. M., Grain, J., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Harrison, D., Helou, G., Henrot Versille, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Leroy, C., Lilje, P. B., Linden Vornle, M., Lockman, F. J., Lopez Caniego, M., Lubin, P. M., Macias Perez, J. F., Mactavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martin, P., Martinez Gonzalez, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Mitra, S., Miville Deschenes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Norgaard Nielsen, H. U., Novikov, D., Novikov, I., O'Dwyer, I. J., Oliver, S., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pinheiro Goncalves, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prezeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan Robinson, M., Rubino Martin, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, M., Yvon, D., Zacchei, A., Zonca, A., Universidad de Cantabria, Department of Physics, Helsinki Institute of Physics, APC - Cosmologie, 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)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), APC - Gravitation (APC-Gravitation), 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), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PLANCK, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université 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), 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), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), 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), 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)

Subjects
Experimental Physics, Diffuse radiation, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, submillimeter: diffuse background, galaxies, cosmology: observations, submillimeter: galaxies, diffuse radiation, diffuse background, cosmology, submillimeter, observations, Astrophysics, 7. Clean energy, 01 natural sciences, CMB physic, CMB physics, Cosmic infrared background, observations [Cosmology], 010303 astronomy & astrophysics, QB, Physics, Planck ESA mission, Cosmology: observations, Cosmology, Wavelength, diffuse radiation – submillimeter: diffuse background – submillimeter: galaxies – cosmology: observations, symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Cosmology and Nongalactic Astrophysics, diffuse backround, Cosmology and Nongalactic Astrophysics (astro-ph.CO), education, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Halo occupation distribution, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies [Submillimeter], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, diffuse background [Submillimeter], diffuse background – submillimeter: galaxies – cosmology: observations [diffuse radiation – submillimeter], Planck, Astrophysics::Galaxy Astrophysics, Submillimeter: diffuse background, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Submillimeter: galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

30 páginas, 21 figuras, 7 tablas.-- Planck Collaboration: et al., Using Planck maps of six regions of low Galactic dust emission with a total area of about 140 deg2, we determine the angular power spectra of cosmic infrared background (CIB) anisotropies from multipole ℓ = 200 to ℓ = 2000 at 217, 353, 545 and 857 GHz. We use 21-cm observations of Hi as a tracer of thermal dust emission to reduce the already low level of Galactic dust emission and use the 143 GHz Planck maps in these fields to clean out cosmic microwave background anisotropies. Both of these cleaning processes are necessary to avoid significant contamination of the CIB signal. We measure correlated CIB structure across frequencies. As expected, the correlation decreases with increasing frequency separation, because the contribution of high-redshift galaxies to CIB anisotropies increases with wavelengths. We find no significant difference between the frequency spectrum of the CIB anisotropies and the CIB mean, with ΔI / I = 15% from 217 to 857 GHz. In terms of clustering properties, the Planck data alone rule out the linear scale- and redshift-independent bias model. Non-linear corrections are significant. Consequently, we develop an alternative model that couples a dusty galaxy, parametric evolution model with a simple halo-model approach. It provides an excellent fit to the measured anisotropy angular power spectra and suggests that a different halo occupation distribution is required at each frequency, which is consistent with our expectation that each frequency is dominated by contributions from different redshifts. In our best-fit model, half of the anisotropy power at ℓ = 2000 comes from redshifts z < 0.8 at 857 GHz and z < 1.5 at 545 GHz, while about 90% come from redshifts z > 2 at 353 and 217 GHz, respectively., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU).

Published
2011

39. Planck early results. VIII. The all-sky early Sunyaev-Zeldovich cluster sample

Subjects
ta115, SOUTH-POLE TELESCOPE, ta213, COSMOLOGICAL PARAMETERS, NEARBY CLUSTERS, MICROWAVE BACKGROUND TEMPERATURE, COSMIC DISTANCE SCALE, galaxies: clusters: general, cosmology: observations, CORONA BOREALIS SUPERCLUSTER, MASSIVE GALAXY CLUSTERS, HYDRODYNAMICAL SIMULATIONS, X-RAY-PROPERTIES, catalogs, HUBBLE CONSTANT
Published
2011

40. K+a galaxies in the zCOSMOS survey

Subjects
galaxies: luminosity function, mass function, cosmology: observations, galaxies: formation, galaxies: fundamental parameters, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

Aims: The identities of the main processes triggering and quenching star-formation in galaxies remain unclear. A key stage in evolution, however, appears to be represented by post-starburst galaxies. To investigate the prevalence of these galaxies and their impact on galaxy evolution in general, we initiated a multiwavelength study of galaxies with k+a spectral features in the well-studied COSMOS field. Methods: We examine a mass-selected sample of k+a galaxies in the COSMOS field at z = 0.48-1.2 using the spectroscopic zCOSMOS sample. To classify galaxies in their k+a phase, we use a spectroscopic criterion, based on the amplitude of the Hδ absorption line and the absence of the [OII] emission line. We develop our analysis for a well-defined sample by imposing stringent confidence levels on the spectroscopic redshifts and spectral measurements. We compare our results for two mass-selected samples of star-forming and quiescent galaxies selected using a purely spectral classification scheme from the 10 000 zCOSMOS catalogue (i.e. , based on measurements of 4000 Å break and EW[OII]). Results: In our mass-limited sample, k+a galaxies occupy the brightest tail of the luminosity distribution. They are as massive as quiescent galaxies and populate the green valley in the colour versus luminosity (or stellar mass) distribution. A small percentage (

Published
2010

41. The ESO/VLT 3rd year Type Ia supernova data set from the supernova legacy survey

Author

Sebastien Fabbro, Julien Guy, Stéphane Basa, J. Le Du, Pierre Astier, V. Ruhlmann-Kleider, Nicolas Regnault, D. Hardin, Kathy Perrett, I. M. Hook, Nathalie Palanque-Delabrouille, A. Conley, Emmanuel Pecontal, J. Rich, Reynald Pain, Christopher J. Pritchet, A. Mourao, V. Arsenijevic, M. Mouchet, D. A. Howell, Chris Lidman, S. Baumont, Raymond G. Carlberg, Christophe Balland, Dominique Fouchez, Mark Sullivan, P. Antilogus, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), APC - Cosmologie, 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)-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), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), SNLS, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Spectral line, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], supernovae: general, law, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Very Large Telescope, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, methods: data analysis, Redshift, Supernova, 13. Climate action, Space and Planetary Science, cosmology: observations, Supernova Legacy Survey, Astrophysics::Earth and Planetary Astrophysics, techniques: spectroscopic, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present 139 spectra of 124 Type Ia supernovae (SNeIa) that were observed at the ESO/VLT during the first three years of the Canada-France-Hawai Telescope (CFHT) Supernova Legacy Survey (SNLS). This homogeneous data set is used to test for redshift evolution of SNeIa spectra, and will be used in the SNLS 3rd year cosmological analyses. Spectra have been reduced and extracted with a dedicated pipeline that uses photometric information from deep CFHT Legacy Survey (CFHT-LS) reference images to trace, at sub-pixel accuracy, the position of the supernova on the spectrogram as a function of wavelength. It also separates the supernova and its host light in 60% of cases. The identification of the supernova candidates is performed using a spectrophotometric SNIa model. A total of 124 SNeIa, roughly 50% of the overall SNLS spectroscopic sample, have been identified using the ESO/VLT during the first three years of the survey. Their redshifts range from z=0.149 to z=1.031. The average redshift of the sample is z=0.63+/-0.02. This constitutes the largest SNIa spectral set to date in this redshift range. The spectra are presented along with their best-fit spectral SNIa model and a host model where relevant. In the latter case, a host subtracted spectrum is also presented. We produce average spectra for pre-maximum, maximum and post-maximum epochs for both z=0.5 SNeIa. We find that z= 0.5 spectra. The differences with redshift are consistent with the selection of brighter and bluer supernovae at higher redshift., Accepted for publication in Astronomy and Astrophysics, 103 pages, 11 main figures (+139 figures of VLT spectra)

Published
2009

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