  This thesis presents the analysis of the clustering of galaxies in the 6dF
Galaxy Survey (6dFGS). At large separation scales the baryon acoustic
oscillation (BAO) signal is detected which allows to make an absolute distance
measurement at $z_{\rm eff} = 0.106$. Such a measurement can be used to
constrain the Hubble constant, $H_0 = 67.0\pm3.2\;$km s$^{-1}\;$Mpc$^{-1}$
(4.8% precision).
  Modelling the 2D galaxy correlation function of 6dFGS, $\xi(r_p,\pi)$, allows
a measure of the parameter combination $f(z_{\rm eff})\sigma_8(z_{\rm eff}) =
0.423 \pm 0.055$, where $f \simeq \Omega_m^{\gamma}(z)$ is the growth rate of
cosmic structure and $\sigma_8$ is the r.m.s. of matter fluctuations in
$8h^{-1}\,$Mpc spheres. Such a measurement allows to test the relationship
between matter and gravity on cosmic scales by constraining the growth index of
density fluctuations, $\gamma$. The 6dFGS measurement of $f\sigma_8$ combined
with WMAP-7, results in $\gamma = 0.547 \pm 0.088$, consistent with the
prediction of General Relativity ($\gamma_{\rm GR} \approx 0.55$).
  The last chapter of this thesis studies the stellar-mass dependence of galaxy
clustering in the 6dF Galaxy Survey. Using the Halo Occupation Distribution
(HOD) model, this analysis investigates the trend of dark matter halo mass and
satellite fraction with stellar mass by measuring the projected correlation
function, $w_p(r_p)$. The findings of this analysis are, that the typical halo
mass ($M_1$) as well as the satellite power law index ($\alpha$) increase with
stellar mass. The 6dFGS results are compared to two different semi-analytic
models derived from the Millennium Simulation, as well as weak lensing
measurements.
