Events

Date: 20 February 2026   Time: 14:30 - 15:30

Location: Room 610, G. O. Jones, Mile End Campus

How do we reconstruct the Universe's thermal and star-forming history without being fooled by galaxy bias? Using the FLAMINGO hydrodynamic simulations, we show that cross-correlation tomography can be made robust against small-scale clustering effects. We build estimators for the halo bias-weighted electron pressure 〈bPe〉 and star-formation density 〈bρSFR〉—quantities accessible through tomographic analyses of the SZ and CIB signals—and demonstrate 1–3% accuracy across redshift and sample type. This work opens the way to unbiased reconstructions of cosmic evolution from current and future large-scale surveys.