Assembly bias in the local PNG halo bias and its implication for $f_{\mathrm{NL}}$ constraints

Abstract

We use $N$-body simulations to study halo assembly bias (i.e., the dependence of halo clustering on properties beyond total mass) in the density and primordial non-Gaussianity (PNG) linear bias parameters $b_1$ and $b_{\varphi }$, respectively. We consider concentration, spin and sphericity as secondary halo properties, for which we find a clear detection of assembly bias for $b_1$ and $b_{\varphi }$. At fixed total mass, halo spin and sphericity impact $b_1$ and $b_{\varphi }$ in a similar manner, roughly preserving the shape of the linear $b_{\varphi }(b_1)$ relation satisfied by the global halo population. Halo concentration, however, drives $b_1$ and $b_{\varphi }$ in opposite directions. This induces significant changes to the $b_{\varphi }(b_1)$ relation, with higher concentration halos having higher amplitude of $b_{\varphi }(b_1)$. For $z=0.5$ and $b_1\approx 2$ in particular, the population comprising either all halos, those with the $33\%$ lowest or those with the $33\%$ highest concentrations have a PNG bias of $b_{\varphi }\approx 3$, $b_{\varphi }\approx -1$ and $b_{\varphi }\approx 9$, respectively. Varying the halo concentration can make $b_{\varphi }$ very small and even change its sign. These results have important ramifications for galaxy clustering constraints of the local PNG parameter $f_{\mathrm{NL}}$ that assume fixed forms for the $b_{\varphi }(b_1)$ relation. We illustrate the significant impact of halo assembly bias in actual data using the BOSS DR12 galaxy power spectrum: assuming that BOSS galaxies are representative of all halos, the $33\%$ lowest or the $33\%$ highest concentration halos yields ${\sigma }_{f_{\mathrm{NL}}}=44,165,19$, respectively. Our results suggest taking host halo concentration into account in galaxy selection strategies to maximize the signal-to-noise on $f_{\mathrm{NL}}$. They also motivate more simulation-based efforts to study the $b_{\varphi }(b_1)$ relation of halos and galaxies.

21 pages, 4 figures, comments welcome; V2 minor modifications throughout, published in JCAP

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