Galaxy bias and primordial non-Gaussianity: insights from galaxy formation simulations with IllustrisTNG

Abstract

We study the impact that large-scale perturbations of (i) the matter density and (ii) the primordial gravitational potential with local primordial non-Gaussianity (PNG) have on galaxy formation using the IllustrisTNG model. We focus on the linear galaxy bias b1 and the coefficient bϕ of the scale-dependent bias induced by PNG, which describe the response of galaxy number counts to these two types of perturbations, respectively. We perform our study using separate universe simulations, in which the effect of the perturbations is mimicked by changes to the cosmological parameters: modified cosmic matter density for b1 and modified amplitude \U0001d49cs of the primordial scalar power spectrum for bϕ. We find that the widely used universality relation bϕ = 2δc(b1 − 1) is a poor description of the bias of haloes and galaxies selected by stellar mass M*, which is instead described better by bϕ(M*) = 2δc(b1(M*) − p) with p ∊ [0.4, 0.7]. This is explained by the different impact that matter overdensities and local PNG have on the median stellar-to-halo-mass relation. A simple model of this impact allows us to describe the stellar mass dependence of b1 and bϕ fairly well. Our results also show a nontrivial relation between b1 and bϕ for galaxies selected by color and black hole mass accretion rate. Our results provide refined priors on bϕ for local PNG constraints and forecasts using galaxy clustering. Given that the widely used universality relation underpredicts bϕ(M*), existing analyses may underestimate the true constraining power on local PNG.