Speaker
Description
Accurate characterization of galaxy clusters in millimetre-wavelength surveys requires rigorous separation of the thermal Sunyaev-Zeldovich (tSZ) distortion of the CMB signal from its contaminants. This task should ideally disentangle extended components, such as Galactic dust, Cosmic Microwave, and sub-millimetre backgrounds, whose spectral shapes and spatial distributions exhibit specific statistics. In this work, we present a spectral imaging approach that combines a locally parametric modelling and a sparse representation of all-sky tSZ, Galatic thermal dust and CMB signals, as observed by the Planck High Frequency Instrument. In contrast to alternative component separation algorithms, this method does not presuppose component independence, stationarity or Gaussianity. These maps serve as a robust framework for extracting cluster-specific features, such as filaments and shocks. By providing an alternative methodology for analyzing the properties of the intracluster medium, this approach enhances our ability to probe galaxy cluster physics and their connections to large-scale cosmic structures.
| Would you be interested in presenting a poster if the conference is oversubcribed? | No |
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