Stochastic Gravitational Wave Background originating from Halo Mergers

TL;DR

This paper models the stochastic gravitational wave background from halo mergers using a quasi-analytic approach, combining merger trees with N-body simulation data to estimate the GWB amplitude and its dominant sources.

Contribution

It introduces a novel semi-analytic method to estimate the GWB from halo mergers by integrating merger trees with N-body simulation results.

Findings

GWB amplitude estimated as Ω_GW ~ 10^{-19} at frequencies 10^{-17}-10^{-16} Hz.

Most GWB contribution comes from halos below 10^{15} solar masses.

Low redshift mergers (0<z<0.8) dominate the GWB signal.

Abstract

The stochastic gravitational wave background (GWB) from halo mergers is investigated by a quasi-analytic method. The method we employ consists of two steps. The first step is to construct a merger tree by using the Extended Press-Schechter formalism or the Sheth & Tormen formalism, with Monte-Carlo realizations. This merger tree provides evolution of halo masses. From $N$-body simulation of two-halo mergers, we can estimate the amount of gravitational wave emission induced by the individual merger process. Therefore the second step is to combine this gravitaional wave emission to the merger tree and obtain the amplitude of GWB. We find $\Omega_{GW}\sim 10^{-19}$ for $f\sim 10^{-17}-10^{-16}$ Hz, where $\Omega_{GW}$ is the energy density of the GWB. It turns out that most of the contribution on the GWB comes from halos with masses below $10^{15} M_\odot$ and mergers at low redshift, i.e., $0<z<0.8$.