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arXiv · 1204.1439

Stochastic Gravitational Wave Background originating from Halo Mergers

Takahiro Inagaki·Keitaro Takahashi·Naoshi Sugiyama
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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 $Ω_{GW}\sim 10^{-19}$ for $f\sim 10^{-17}-10^{-16}$ Hz, where $Ω_{GW}$ 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., $0<z<0.8$.

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Takahiro Inagaki, Keitaro Takahashi, Naoshi Sugiyama. 2012-04-06. Stochastic Gravitational Wave Background originating from Halo Mergers. https://doi.org/10.1103/physrevd.85.104051

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