An estimate of the stochastic gravitational wave background from the MassiveBlackII simulation. Issue 4 (14th February 2022)

• Record Type: Journal Article
• Authors: Sykes, Bailey; Middleton, Hannah; Melatos, Andrew; Di Matteo, Tiziana; DeGraf, Colin; Bhowmick, Aklant
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 511:Issue 4(2022)
• Page Start: 5241
• Page End: 5250
• Publication Date: 2022-02-14
• Subjects: gravitational waves -- galaxy: kinematics and dynamics -- black hole mergers -- quasars: supermassive black holes; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac388
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: A population of supermassive black hole (SMBH) binaries is expected to generate a stochastic gravitational wave background (SGWB) in the pulsar timing array (PTA) frequency range of 10 −9 to $10^{-7}\, {\rm Hz}$ . Detection of this signal is a current observational goal and so predictions of its characteristics are of significant interest. In this work, we use SMBH binary mergers from the MassiveBlackII simulation to estimate the characteristic strain of the stochastic background. We examine both a gravitational wave (GW) driven model of binary evolution and a model which also includes the effects of stellar scattering and a circumbinary gas disc. Results are consistent with PTA upper limits and similar to estimates in the literature. The characteristic strain at a reference frequency of $1\, {\rm yr}^{-1}$ is found to be $A_{\rm {yr}^{-1}}= 6.9 \times 10^{-16}$ and $A_{\rm {yr}^{-1}}= 6.4 \times 10^{-16}$ in the GW-driven and stellar scattering/gas disc cases, respectively. Using the latter approach, our models show that the SGWB is mildly suppressed compared to the purely GW-driven model as frequency decreases inside the PTA frequency band.