Research

RESEARCH IN COSMOLOGY

  • Cosmic Microwave Background (CMB): the cleanest CMB map.  The cosmic microwave background (CMB) is a relic radiation, which was emitted 370,000 years after the Big Bang at the epoch of recombination. This is when our Universe became neutral and transparent. The CMB radiation has travelled the Universe since decoupling and its precise measurement is critical to observational cosmology.

GMCA_WPR1Using both WMAP and Planck PR1 data, we have reconstructed an extremely clean CMB map. A more detailed description can be found here. The same method has been used on Planck and PR2 data (Bobin et al, 2016). We have shown that large scale analysis does not require masking anymore when using our estimated CMB map (Bobin et al, A&A, 2014), and that CMB large scales are compatible with the standard l-CDM cosmological model (Rassat et al, 2014). More details can be found here. Finally, we have estimated the primordial power spectrum using our PRISM method on both WMAP9 (Paykari et al., A&A, 2014) and Planck data (Lanusse et al., A&A, 2014) and we find no significant departure from the Planck PR1 best fit.

  • Weak Lensing:
    • 2D mass mapping: Using both shear and flexion, we have shown how very high resolution convergence maps can be reconstructed (Lanusse et al, 2016). More details are available here.
    • The 3D tomographic window is now open for cosmology.  Underlying the link between weak lensing and the compressed sensing theory, we have proposed a completely new approach to reconstruct the dark matter distribution in three dimensions using photometric redshift information, and we have shown we can estimate with a very good accuracy level the mass and the redshift of dark matter haloes, which is crucial for unveiling the nature of the Dark Universe (Leonard, Lanusse et Starck, A&A, 2014).  Full details are here.
    • Point Spread Function Modeling: For weak lensing shear measurements to be useful for cosmological studies, it is also necessary to model properly the point spread function (PSF) of the instrument. In the case of the Euclid project, this PSF is subsampled, and we have proposed the SPRITE  method (Ngolè, Starck et al, A&A, 2014) to achieve surperresolution, which will increase the cosmological constraining power of Euclid significantly. See here for more details.
  • Spatial/Color Distribution of Galaxies:
    • New data require new representations. We have investigated benefits of performing a full 3D Fourier-Bessel analysis of spectroscopic galaxy surveys, such as the Euclid spectroscopic survey, compared to more traditional tomographic analysis. We have shown that the 3D analysis optimally extracts the information and is more robust to uncertainties on the coupling between the galaxies and the dark matter (Lanusse, Rassat and Starck, A&A, 2015).
    • Late type/Early type galaxy separation: We have also shown how sparsity can help to separate automatically early type galaxies from late type galaxies, using multichannel data set (Joseph et al, A&A, 2016). Such a method could be extremely useful for Strong Lensing.  See here for more details.

RESEARCH IN SIGNAL PROCESSING/STATISTICS

CygA

Sparse recovery allows us to reconstruct an image with a resolution increased by a factor two (Garsden, Girard, Starck, Corbel et al, A&A, 2015).  This has been confirmed by comparing two images of the  Cygnus A radio source, the first from the LOFAR instrument and reconstructed using sparsity, and the second one from Very Large Array at a higher frequency (and therefore with a better resolution). The contour the VLA image matches perfectly the high resolution features that can be seen in the LOFAR color map image. More details here.