A new scale in the bias expansion

Abstract

The fact that the spatial nonlocality of galaxy formation is controlled by some short length scale like the Lagrangian radius is the cornerstone of the bias expansion for large-scale-structure tracers. However, the first sources of ionizing radiation between $z\approx 15$ and $z\approx 6$ are expected to have significant effects on the formation of galaxies we observe at lower redshift, at least on low-mass galaxies. These radiative-transfer effects introduce a new scale in the clustering of galaxies, i.e. the finite distance which ionizing radiation travels until it reaches a given galaxy. This mean free path can be very large, of order $100h^{-1}\mathrm{Mpc}$. Consequently, higher-derivative terms in the bias expansion could turn out to be non-negligible even on these scales: treating them perturbatively would lead to a massive loss in predictivity and, for example, could spoil the determination of the BAO feature or constraints on the neutrino mass. Here, we investigate under what assumptions an explicit non-perturbative model of radiative-transfer effects can maintain the robustness of large-scale galaxy clustering as a cosmological probe.

arXiv comment33 pages, 5 figures, 2 tables. Added discussion on time dependence of galaxy response. Extended conclusions with discussion on velocity bias and redshift-space distortions. Main results unchanged

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• An $n$-th order Lagrangian Forward Model for Large-Scale Structure
• Biased Tracers of Two Fluids in the Lagrangian Picture
• Intensity mapping with neutral hydrogen and the Hidden Valley simulations
• Baryon-CDM isocurvature galaxy bias with IllustrisTNG
• Responses of Halo Occupation Distributions: a new ingredient in the halo model & the impact on galaxy bias
• Neutrino mass bounds from confronting an effective model with BOSS Lyman-alpha data
• The Compressed 3D Lyman-Alpha Forest Bispectrum