Probing the large scale structure using gravitational-wave observations
  of binary black holes
  Third generation gravitational-wave (GW) detectors are expected to detect a
large number of binary black holes (BBHs) to large redshifts, opening up an
independent probe of the large scale structure using their clustering. This
probe will be complementary to the probes using galaxy clustering -- GW events
could be observed up to very large redshifts ($z \sim 10$) although the source
localization will be much poorer at large distances ($\sim$ tens of square
degrees). We explore the possibility of probing the large scale structure from
the spatial distribution of the observed BBH population, using their two-point
(auto)correlation function. We find that we can estimate the bias factor of
population of BBH (up to $z \sim 1$) with a few years of observations with
these detectors. Our method relies solely on the source-location posteriors
obtained the GW events and does not require any information from
electromagnetic observations. This will help in identifying the type of
galaxies that host the BBH population, thus shedding light on their origins.
