Kavli Affiliate: Rainer Spurzem
| First 5 Authors: Seungjae Lee, Hyung Mok Lee, Ji-hoon Kim, Rainer Spurzem, Jongsuk Hong
| Summary:
We investigate the evolution of star clusters containing intermediate-mass
black hole (IMBH) of $300$ to $5000 mathrm{M}_odot$, focusing on the
formation and evolution of IMBH-stellar mass black holes (SBHs; $M_{rm BH}
lesssim 10^2 mathrm{M}_odot$) binaries. Dense stellar systems like globular
clusters (GCs) or nuclear star clusters offer unique laboratories for studying
the existence and impact of IMBHs. IMBHs residing in GCs have been under
speculation for decades, with their broad astrophysical implications for the
cluster’s dynamical evolution, stellar population, GW signatures, among others.
While existing GW observatories such as the Advanced Laser Interferometer
Gravitational-wave Observatory (aLIGO) target binaries with relatively modest
mass ratios, $q lesssim 10$, future observatories such as the Einstein
Telescope (ET) and the Laser Interferometer Space Antenna (LISA) will detect
intermediate-mass ratio inspirals (IMRIs) with $q > 10$. This work explores the
potential for detecting IMRIs adopting these upcoming telescopes. For our
experiments, we perform multiple direct $N$-body simulations with IMBHs
utilizing Nbody6++GPU, after implementing the GW merger schemes for IMBHs. We
then study the statistical properties of the resulting IMRIs, such as the event
rates and orbital properties. Assuming that IMRIs with a signal-to-noise ratio
$S/N > 8$ are detectable, we derive the following detection rates for each
observatory: $lesssim 0.02mathrm{yr}^{-1}$ for aLIGO, $sim 101 – 355
mathrm{yr}^{-1}$ for ET, $sim 186 – 200 mathrm{yr}^{-1}$ for LISA, $sim
0.24 – 0.34 mathrm{yr}^{-1}$ for aSOGRO, and $sim 3880 – 4890
mathrm{yr}^{-1}$ for DECIGO. Our result confirms the capability of detecting
IMRIs with future GW telescopes.
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