Binary intermediate-mass black hole mergers in globular clusters
  We consider the formation of binary intermediate black holes (BIMBH) in
globular clusters (GC), which could happen either in situ or due to the mergers
between clusters. We simulate the evolution of the BIMBH orbit (and its
subsequent merger) due to stellar ejections. We also take into account the
evaporation of GCs due to the tidal field of the host galaxy and two-body
relaxation. Our results show that if at least $10^{-3}$ of all GCs become BIMBH
hosts and the BIMBH masses are $\sim1\%$ of the GC mass, at least one of the
inspiralling (or merging) BIMBHs will be detected by LISA during its 4-year
mission lifetime. Most of the detected BIMBHs come 1) from heavy GCs
($\gtrsim3\times10^5M_\odot$), as lower-mass GCs end up being disrupted before
their BIMBHs have time to merge, and 2) from redshifts $1<z<3$, assuming that
most of GCs form around $z\sim4$ and given that the merger timescale for most
BIMBHs is $\sim1$ Gyr. If the BIMBH to GC mass ratio is lower ($\sim10^{-3}$)
but the fraction of BIMBH hosts among GCs is higher ($\gtrsim10^{-2}$), some of
their mergers will also be detected by LIGO, VIRGO, and KAGRA and the proposed
Einstein Telescope.
