The bias of weighted dark matter halos from peak theory

Abstract

We give an analytical form for the weighted correlation function of peaks in a Gaussian random field. In a cosmological context, this approach strictly describes the formation bias and is the main result here. Nevertheless, we show its validity and applicability to the evolved cosmological density field and halo field, using Gaussian random field realisations and dark matter N-body numerical simulations. Using this result from peak theory we compute the bias of peaks (and dark matter halos) and show that it reproduces results from the simulations at the $\mathcal{O}(10\%)$ level. Our analytical formula for the bias predicts a scale-dependent bias with two characteristics: a broad band shape which, however, is most affected by the choice of weighting scheme and evolution bias, and a more robust, narrow feature localised at the BAO scale, an effect that is confirmed in simulations. This scale-dependent bias smooths the BAO feature but, conveniently, does not move it. We provide a simple analytic formula to describe this effect. We envision that our analytic solution will be of use for galaxy surveys that exploit galaxy clustering.

Submitted to MNRAS

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• Large-Scale Galaxy Bias
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• From Primordial Black Holes Abundance to Primordial Curvature Power Spectrum (and back)
• ShapeFit: extracting the power spectrum shape information in galaxy surveys beyond BAO and RSD
• Discrepancies between CFHTLenS cosmic shear & Planck: new physics or systematic effects?
• Lagrangian bias of generic large-scale structure tracers
• Measuring the Energy Scale of Inflation with Large Scale Structures
• Non-perturbative halo clustering from cosmological density peaks
• The Spatial Range of Conformity
• Symmetries, Invariants and Generating Functions: Higher-order Statistics of Biased Tracers