Study of the Intermediate Mass Ratio Black Hole Binary Merger up to
  1000:1 with Numerical Relativity
  We explicitly demonstrate that current numerical relativity technology is
able to accurately evolve black hole binaries with mass ratios of the order of
1000:1. This has direct implications for future third generation (3G)
gravitational wave detectors and space mission LISA, as by purely numerical
methods we are able to accurately compute gravitational waves, as directly
predicted by general relativity. We perform a sequence of simulations in the
intermediate to small mass ratio regime, $m_1^p/m_2^p = 1/7, 1/16, 1/32, 1/64,
1/128, 1/256, 1/512, 1/1024$, with the small hole starting from rest at a
proper distance $D\approx13M$. We compare this full numerical evolutions with
the corresponding semianalytic perturbative results finding a striking
agreement for the total gravitational radiated energy and linear momentum as
well as for the gravitational waveforms. We display numerical convergence of
the results and identify the minimal numerical resolutions required to
accurately solve these very low amplitude gravitational waves. We conclude that
we have the numerical technology to build up template banks in time for 3G
detectors and LISA.
