Detecting Black-Hole Binary Clustering via the Second-Generation
  Gravitational-Wave Detectors
  The first discovery of the gravitational wave (GW) event, GW150914, suggests
a higher merger rate of black-hole (BH) binaries. If this is true, a number of
BH binaries will be observed via the second-generation GW detectors, and the
statistical properties of the observed BH binaries can be scrutinized. A naive
but important question to ask is whether the spatial distribution of BH
binaries faithfully traces the matter inhomogeneities in the Universe or not.
Although the BH binaries are thought to be formed inside the galaxies in most
of the scenarios, there is no observational evidence to confirm such a
hypothesis. Here, we estimate how well the second-generation GW detectors can
statistically confirm the BH binaries to be a tracer of the large-scale
structure by looking at the auto- and cross-correlation of BH binaries with
photometric galaxies and weak lensing measurements, finding that, with a 3 year
observation, the $>3\sigma$ detection of non-zero signal is possible if the BH
merger rate today is $\dot{n}_0\gtrsim100$ Gpc$^{-3}$yr$^{-1}$ and the
clustering bias of BH binaries is $b_{\rm BH,0}\gtrsim1.5$.
