Galaxies hosting co-spatial radio sources show roughly twice the Compton-y signal at fixed stellar mass compared to those without, persisting to halo scales, with two competing explanations: higher halo mass or AGN thermal energy injection.
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4 Pith papers cite this work, alongside 14 external citations. Polarity classification is still indexing.
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FLAMINGO simulation analysis shows IA amplitude for LRGs depends on halo assembly history and exhibits redshift evolution beyond mass effects, yielding an empirical mass-redshift model.
tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.
SKA FRB dispersion measures and their cross-correlations with Stage IV shear and clustering can pin down baryonic feedback and improve cosmological constraints by factors of ~2–5 under optimistic detection rates.
citing papers explorer
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Thermal Sunyaev-Zel'dovich Measurements of Locally Bright Galaxies with ACT DR6: Radio Source Contamination and Excess Compton-y Signal
Galaxies hosting co-spatial radio sources show roughly twice the Compton-y signal at fixed stellar mass compared to those without, persisting to halo scales, with two competing explanations: higher halo mass or AGN thermal energy injection.
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Assembly bias and the redshift evolution of intrinsic alignments for LRGs
FLAMINGO simulation analysis shows IA amplitude for LRGs depends on halo assembly history and exhibits redshift evolution beyond mass effects, yielding an empirical mass-redshift model.
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FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics
tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.
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Probing the Baryon Distribution with Fast Radio Bursts
SKA FRB dispersion measures and their cross-correlations with Stage IV shear and clustering can pin down baryonic feedback and improve cosmological constraints by factors of ~2–5 under optimistic detection rates.