PIRSA:09050013

How non-thermal processes of the intracluster medium affect the Sunyaev-Zeldovich angular power spectrum

Battagalia, N. (2009). How non-thermal processes of the intracluster medium affect the Sunyaev-Zeldovich angular power spectrum. Perimeter Institute. https://pirsa.org/09050013

Battagalia, Nick. How non-thermal processes of the intracluster medium affect the Sunyaev-Zeldovich angular power spectrum. Perimeter Institute, Apr. 28, 2009, https://pirsa.org/09050013 

          @misc{ pirsa_PIRSA:09050013,
            doi = {10.48660/09050013},
            url = {https://pirsa.org/09050013},
            author = {Battagalia, Nick},
            keywords = {Cosmology},
            language = {en},
            title = {How non-thermal processes of the intracluster medium affect the Sunyaev-Zeldovich angular power spectrum},
            publisher = {Perimeter Institute},
            year = {2009},
            month = {apr},
            note = {PIRSA:09050013 see, \url{https://pirsa.org}}
          }

Nick Battagalia

Canadian Institute for Theoretical Astrophysics (CITA)

Talk number
PIRSA:09050013
Collection
Talk Type
Subject
Abstract
"There is considerable uncertainty in the theoretical predictions for the angular power spectrum from the Sunyaev-Zeldovich effect (SZe). The level of precision reached by ACT, SPT, and Planck for measurements of the normalization of the SZe power spectrum, sigma_8, will be limited by the uncertainty in the theoretical models for the angular power spectrum. The uncertainties in the predicted spectrum arise from the complicated physics of the ICM. We have explored these ICM complexities using hydrodynamical simulations in a cosmological setting with several different variants of simulated physics, including cooling and star formation, star formation feedback by galactic winds and supernovae as well as cosmic ray physics. Our statistics were compiled from two independently stacked cluster samples consisting of cosmological box simulations and individual high-resolution cluster simulations. We show that a simple parametrized fit describes averaged ICM pressure profiles sufficiently well and compare this finding to previous hydrostatic models. We find that radiative cooling and the associated star formation is the dominant physical process that modifies our fit parameters for these profiles and the angular power spectrum. "