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Cosmological feedback from a halo assembly perspective

Luisa Lucie-Smith1,*, Hiranya V. Peiris2,3,†, Andrew Pontzen4,‡, Anik Halder2, Joop Schaye5, Matthieu Schaller5,6, John Helly4, Robert J. McGibbon5, and Willem Elbers4

  • 1Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany
  • 2Institute of Astronomy and Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
  • 3The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, Stockholm SE-106 91, Sweden
  • 4Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham, DH1 3LE, United Kingdom
  • 5Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
  • 6Lorentz Institute for Theoretical Physics, Leiden University, PO Box 9506, NL-2300 RA Leiden, The Netherlands

  • *Contact author: luisa.lucie-smith@uni-hamburg.de
  • †Contact author: hiranya.peiris@ast.cam.ac.uk
  • ‡Contact author: andrew.p.pontzen@durham.ac.uk
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Phys. Rev. D 112, 063541 – Published 19 September, 2025

DOI: https://doi.org/10.1103/vh8n-9cr2

Abstract

The impact of feedback from galaxy formation on cosmological probes is typically quantified in terms of the suppression of the matter power spectrum in hydrodynamical compared to gravity-only simulations. In this paper, we instead study how baryonic feedback impacts halo assembly histories and thereby imprints on cosmological observables. We investigate the sensitivity of the thermal Sunyaev-Zel’dovich effect (tSZ) power spectrum, X-ray number counts, weak lensing and kinetic Sunyaev-Zel’dovich (kSZ) stacked profiles to halo populations as a function of mass and redshift. We then study the imprint of different feedback implementations in the FLAMINGO suite of cosmological simulations on the assembly histories of these halo populations, as a function of radial scale. We find that kSZ profiles target lower-mass halos (M200  m∼1013.1M⊙) compared to all other probes considered (M200  m∼1015M⊙). Feedback is inefficient in high-mass clusters with ∼1015M⊙ at z=0, but was more efficient at earlier times in the same population, with a ∼5–10% effect on mass at 2<z<4 (depending on radial scale). Conversely, for lower-mass halos with ∼1013M⊙ at z=0, feedback exhibits a ∼5–20% effect on mass at z=0 but had little impact at earlier times (z>2). These findings are tied together by noting that, regardless of redshift, feedback most efficiently redistributes baryons when halos reach a mass of M200  m≃1012.8M⊙ and ceases to have any significant effect by the time M200  m≃1015M⊙. We put forward strategies for minimizing sensitivity of lensing analyses to baryonic feedback, and for exploring baryonic resolutions to the unexpectedly low tSZ power in cosmic microwave background observations.

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Phys. Rev. D 112, 063541– Published 19 September, 2025
  • Received 11 June 2025
  • Accepted 28 August 2025
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