StarTrack predictions of the stochastic gravitational-wave background from compact binary mergers. (arXiv:2008.04890v2 [astro-ph.CO] UPDATED)

StarTrack predictions of the stochastic gravitational-wave background from compact binary mergers. (arXiv:2008.04890v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Perigois_C/0/1/0/all/0/1">C. P&#xe9;rigois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belczynski_C/0/1/0/all/0/1">C. Belczynski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulik_T/0/1/0/all/0/1">T. Bulik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Regimbau_T/0/1/0/all/0/1">T. Regimbau</a>

We model the gravitational-wave background created by double compact objects
from isolated binary evolution across cosmic time using the
textbf{textit{StarTrack}} binary population code. We include Population I/II
stars as well as metal-free Population III stars. Merging and non-merging
double compact object binaries are taken into account. In order to model the
low frequency signal in the band of the space antenna LISA, we account for the
evolution of the redshift and the eccentricity. We find an energy density of
$Omega_{GW} sim 7.5 times 10^{-10}$ at the reference frequency of 25 Hz for
population I/II only, making the background detectable after $sim$5.5 years of
observation with the current generation of ground based detectors, such as
LIGO, Virgo and Kagra, operating at design sensitivity. Adding the contribution
from population III increases the energy density to $Omega_{GW} sim 1.4
times 10^{-8}$, and also modifies the shape of the spectrum which starts
deviating from the usual power law $Omega_{GW}(f) sim f^{2/3}$ after $sim
10$ Hz. The contribution from the population of non merging binaries, on the
other hand, is negligible, being orders of magnitude below. Finally, we observe
that the eccentricity has no impact in the frequency band of LISA or ground
based detectors.

We model the gravitational-wave background created by double compact objects
from isolated binary evolution across cosmic time using the
textbf{textit{StarTrack}} binary population code. We include Population I/II
stars as well as metal-free Population III stars. Merging and non-merging
double compact object binaries are taken into account. In order to model the
low frequency signal in the band of the space antenna LISA, we account for the
evolution of the redshift and the eccentricity. We find an energy density of
$Omega_{GW} sim 7.5 times 10^{-10}$ at the reference frequency of 25 Hz for
population I/II only, making the background detectable after $sim$5.5 years of
observation with the current generation of ground based detectors, such as
LIGO, Virgo and Kagra, operating at design sensitivity. Adding the contribution
from population III increases the energy density to $Omega_{GW} sim 1.4
times 10^{-8}$, and also modifies the shape of the spectrum which starts
deviating from the usual power law $Omega_{GW}(f) sim f^{2/3}$ after $sim
10$ Hz. The contribution from the population of non merging binaries, on the
other hand, is negligible, being orders of magnitude below. Finally, we observe
that the eccentricity has no impact in the frequency band of LISA or ground
based detectors.

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