Strong orientation dependence of surface mass density profiles of dark haloes at large scales

TL;DR

This study reveals that the surface mass density profiles of dark matter haloes significantly depend on their orientation relative to the line-of-sight, affecting large-scale clustering measurements and halo bias estimations.

Contribution

It demonstrates the strong orientation dependence of halo surface mass density profiles at large scales and quantifies its impact on bias and mass estimates using N-body simulations.

Findings

Orientation aligned haloes show higher surface density amplitudes.

The two-halo term exhibits up to 30% bias variation due to orientation.

Halo-matter correlation function is elliptical with axis ratio ~0.55.

Abstract

We study the dependence of surface mass density profiles, which can be directly measured by weak gravitational lensing, on the orientation of haloes with respect to the line-of-sight direction, using a suite of $N$-body simulations. We find that, when major axes of haloes are aligned with the line-of-sight direction, surface mass density profiles have higher amplitudes than those averaged over all halo orientations, over all scales from $0.1$ to $100\,\mathrm{Mpc}/h$ we studied. While the orientation dependence at small scales is ascribed to the halo triaxiality, our results indicate even stronger orientation dependence in the so-called two-halo regime, up to $100\,\mathrm{Mpc}/h$. The orientation dependence for the two-halo term is well approximated by a multiplicative shift of the amplitude and therefore a shift in the halo bias parameter value. The halo bias from the two-halo term can be overestimated or underestimated by up to $\sim 30 \%$ depending on the viewing angle, which translates into the bias in estimated halo masses by up to a factor of two from halo bias measurements. The orientation dependence at large scales originates from the anisotropic halo-matter correlation function, which has an elliptical shape with the axis ratio of $\sim 0.55$ up to $100\, \mathrm{Mpc}/h$. We discuss potential impacts of halo orientation bias on other observables such as optically selected cluster samples and a clustering analysis of large-scale structure tracers such as quasars.