Didier Vibert

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We present a determination by the Archeops experiment of the angular power spectrum of the cosmic microwave background anisotropy in 16 bins over the multipole range l = 15 − 350. Archeops was conceived as a precursor of the Planck HFI instrument by using the same optical design and the same technology for the detectors and their cooling. Archeops is a(More)
This is the first paper of a series that describes the methods and basic results of the galics model (for Galaxies In Cosmological Simulations). galics is a hybrid model for hierarchical galaxy formation studies, combining the outputs of large cosmological Nbody simulations with simple, semi-analytic recipes to describe the fate of the baryons within dark(More)
We analyze the cosmological constraints that Archeops (Benoı̂t et al. 2002) places on adiabatic cold dark matter models with passive power-law initial fluctuations. Because its angular power spectrum has small bins in l and large l coverage down to COBE scales, Archeops provides a precise determination of the first acoustic peak in terms of position at(More)
We describe the processing of the 336 billion raw data samples from the High Frequency Instrument (HFI) which we performed to produce six temperature maps from the first 295 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 9.9 to 4.4′.(More)
  • T . Moutard, S. Arnouts, +15 authors L . Van Werbaeke
  • 2016
We present observations collected in the CFHTLS-VIPERS region in the ultraviolet with the GALEX satellite (farand near-ultraviolet channels) and in the near-infrared with the CFHT/WIRCam camera (Ks band) over an area of 22 and 27 deg2, respectively. The depth of the photometry was optimised to measure the physical properties (e.g., star formation rate,(More)
We present a new photoclinometric reconstruction method based on the deformation of a 3D mesh. The optimization process of our method relies on a maximum-likelihood estimation with a density function measuring discrepancies between observed images and the corresponding synthetic images calculated from the progressively deformed 3D mesh. An input mesh is(More)
PFS (Prime Focus Spectrograph), a next generation facility instrument on the 8.2-meter Subaru Telescope, is a very wide-field, massively multiplexed, optical and near-infrared spectrograph. Exploiting the Subaru prime focus, 2394 reconfigurable fibers will be distributed over the 1.3 deg field of view. The spectrograph has been designed with 3 arms of blue,(More)
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