J. -L. Puget

Publications (281)248.37 Total impact

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  Available from: P. B. Lilje

  Article: Planck 2013 results. II. The Low Frequency Instrument data processing

  Planck Collaboration: N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, [......], N. Vittorio, L. A. Wade, B. D. Wandelt, R. Watson, I. K. Wehus, S. D. M. White, A. Wilkinson, D. Yvon, A. Zacchei, A. Zonca
  Astronomy and Astrophysics (Submitted). 03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. III. LFI systematic uncertainties

  Planck Collaboration: N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, [......], P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, R. Watson, A. Wilkinson, D. Yvon, A. Zacchei, A. Zonca
  [show abstract] [hide abstract]
  ABSTRACT: We present the current estimate of instrumental and systematic effect uncertainties of the Planck-Low Frequency Instrument relative to the first release of the Planck cosmological results. We discuss an overview of the main effects and of the tools and methods applied to assess the residuals on maps and power spectra. We also present an overall budget of systematic effect uncertainties, which are dominated by far sidelobe straylight pick-up and imperfect calibration. They are at least two orders of magnitude less than the CMB temperature power spectrum. A residual spurious signal above the noise level is present, especially at 30 GHz, in the multipole range l < 20 and is likely to be caused by residual galactic straylight contamination. Current analysis aims to further reduce the level of spurious signals in the data and to better model systematic effects, in particular straylight and calibration uncertainties.
  Astronomy and Astrophysics (Submitted). 03/2013;
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  Available from: Maurizio Tomasi

  Article: Planck 2013 results. I. Overview of products and scientific results

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], L. A. Wade, B. D. Wandelt, R. Watson, C. Watson, M. White, S. D. M. White, A. Wilkinson, D. Yvon, A. Zacchei, A. Zonca
  Astronomy and Astrophysics (Submitted). 03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XXIX. Planck catalogue of Sunyaev-Zeldovich sources

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, H. Aussel, C. Baccigalupi, A. J. Banday, [......], P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, M. White, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], J. Varis, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. Walter, B. D. Wandelt, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XXVI. Background geometry and topology of the Universe

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], B. Van Tent, J. Varis, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XXV. Searches for cosmic strings and other topological defects

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], B. Van Tent, J. Varis, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 Results. XXIV. Constraints on primordial non-Gaussianity

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, S. D. M. White, M. White, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XXIII. Isotropy and Statistics of the CMB

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, I. K. Wehus, M. White, A. Wilkinson, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XXII. Constraints on inflation

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, M. White, A. Wilkinson, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XXI. Cosmology with the all-sky Planck Compton parameter $y$-map

  Planck Collaboration, P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, [......], J. Varis, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, J. Weller, M. White, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XIX. The integrated Sachs-Wolfe effect

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, M. White, J.-Q. Xia, D. Yvon, A. Zacchei, A. Zonca
  [show abstract] [hide abstract]
  ABSTRACT: Based on CMB maps from the 2013 Planck Mission data release, this paper presents the detection of the ISW effect, i.e., the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4 sigma, depending on which method is used. We investigate three separate approaches, which cover essentially all previous studies, as well as breaking new ground. (i) Correlation of the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection is made using the lensing-induced bispectrum; the correlation between lensing and the ISW effect has a significance close to 2.5 sigma. (ii) Cross-correlation with tracers of LSS, yielding around 3 sigma significance, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) Aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yields a 4 sigma signal when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale compared to expectations. Recent catalogues give more moderate results, ranging from negligible to 2.5 sigma at most, but with a more consistent scale and amplitude, the latter being still slightly above what is expected from numerical simulations within LCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, which had already mapped these scales to the limits of cosmic variance. Planck's broader frequency coverage confirms that the signal is achromatic, bolstering the case for ISW detection. As a final step we use tracers of large-scale structure to filter the CMB data, presenting maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the current accelerated expansion of the Universe.
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XVIII. Gravitational lensing-infrared background correlation

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XVII. Gravitational lensing by large-scale structure

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, M. White, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XVI. Cosmological parameters

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], N. Vittorio, L. A. Wade, B. D. Wandelt, I. K. Wehus, M. White, S. D. M. White, A. Wilkinson, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XV. CMB power spectra and likelihood

  Planck collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, I. K. Wehus, M. White, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XIII. Galactic CO emission

  Planck Collaboration, P.A.R. Ade, N. Aghanim, M.I.R. Alves, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigaluppi, [......], P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, I. K. Wehus, H. Yamamoto T. Yoda, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results. XII. Component separation

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, I. K. Wehus, A. Wilkinson, J.-Q. Xia, D. Yvon, A. Zacchei, A. Zonca
  03/2013;
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  Available from: P. B. Lilje

  Article: Planck 2013 results X. Energetic particle effects: characterization, removal, and simulation

  Planck Collaboration: P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, [......], J. Valiviita, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, D. Yvon, A. Zacchei, A. Zonca
  [show abstract] [hide abstract]
  ABSTRACT: This paper presents the detection, interpretation and removal of the signal resulting from interactions of high energy particles with the Planck High Frequency Instrument (HFI). These interactions fall into two categories, heating the 0.1K bolometer plate and glitches in each detector time stream. Glitch shapes are not simple single pole exponential decays and fall into three families. The glitch shape for each family has been characterized empirically in flight data and removed from the detector time streams. The spectrum of the count rate per unit energy is computed for each family and a correspondence to where on the detector the particle hit is made. Most of the detected glitches are from galactic protons incident on the Si die frame supporting the micromachinced bolometric detectors. At HFI, the particle flux is � 5 cm􀀀2 s􀀀1 and is dominated by protons incident on the spacecraft with an energy >39MeV, leading to a rate of typically one event per second and per detector. Di�erent categories of glitches have di�erent signature in timestreams. Two of the glitch types have a low amplitude component that decays over nearly 1 second. This component produces an excess noise if not properly removed from the time ordered data. We have used a glitch detection and subtraction method based on the joint fit of population templates. The application of this novel glitch removal method removes excess noise from glitches. Using realistic simulations, we find this method does not introduce signal bias.
  03/2013;