The 6dF Galaxy Survey (6dFGS) has detected Baryon Acoustic Oscillations (BAO) and used them to constrain the distance-redshift relation at an effective redshift of $ z_{eff} = 0.106 $. This allows for a distance measurement of $ D_{V}(z_{eff}) = 456 \pm 27 $ Mpc and a distance ratio $ r_{s}(z_{d})/D_{V}(z_{eff}) = 0.336 \pm 0.015 $, with 4.5% precision. The BAO signal provides a competitive and independent method to constrain the Hubble constant $ H_0 $, yielding $ H_0 = 67 \pm 3.2 $ km s$^{-1}$ Mpc$^{-1}$ with 4.8% precision. This result depends only on the WMAP-7 calibration of the sound horizon and the galaxy clustering in 6dFGS. The analysis is less dependent on other cosmological parameters compared to earlier BAO studies at higher redshifts. The BAO signal can help break the degeneracy between the dark energy equation of state parameter $ w $ and $ H_0 $ in CMB data. The study finds $ w = -0.97 \pm 0.13 $ using only WMAP-7 and BAO data from 6dFGS and Percival et al. (2010). The 6dFGS survey is the largest galaxy survey in the local universe, covering almost half the sky. It provides a large volume for studying the BAO signal, which is sensitive to the Hubble constant. The survey's data are not very sensitive to $ \Omega_k $, $ w $, or other higher-dimensional parameters influencing the expansion history. The BAO signal is detected at a scale of $ \approx 105h^{-1} $ Mpc, and the analysis shows that the BAO peak is clearly visible in the correlation function. The study also discusses future surveys like WALLABY and TAIPAN, which are expected to detect BAO peaks and constrain the Hubble constant with 3% precision. The 6dFGS results are compared to other studies, showing that the BAO signal is consistent with $ \Lambda $ CDM predictions. The study concludes that the 6dFGS results provide a robust measurement of the distance scale and the Hubble constant, with implications for constraining cosmological parameters.The 6dF Galaxy Survey (6dFGS) has detected Baryon Acoustic Oscillations (BAO) and used them to constrain the distance-redshift relation at an effective redshift of $ z_{eff} = 0.106 $. This allows for a distance measurement of $ D_{V}(z_{eff}) = 456 \pm 27 $ Mpc and a distance ratio $ r_{s}(z_{d})/D_{V}(z_{eff}) = 0.336 \pm 0.015 $, with 4.5% precision. The BAO signal provides a competitive and independent method to constrain the Hubble constant $ H_0 $, yielding $ H_0 = 67 \pm 3.2 $ km s$^{-1}$ Mpc$^{-1}$ with 4.8% precision. This result depends only on the WMAP-7 calibration of the sound horizon and the galaxy clustering in 6dFGS. The analysis is less dependent on other cosmological parameters compared to earlier BAO studies at higher redshifts. The BAO signal can help break the degeneracy between the dark energy equation of state parameter $ w $ and $ H_0 $ in CMB data. The study finds $ w = -0.97 \pm 0.13 $ using only WMAP-7 and BAO data from 6dFGS and Percival et al. (2010). The 6dFGS survey is the largest galaxy survey in the local universe, covering almost half the sky. It provides a large volume for studying the BAO signal, which is sensitive to the Hubble constant. The survey's data are not very sensitive to $ \Omega_k $, $ w $, or other higher-dimensional parameters influencing the expansion history. The BAO signal is detected at a scale of $ \approx 105h^{-1} $ Mpc, and the analysis shows that the BAO peak is clearly visible in the correlation function. The study also discusses future surveys like WALLABY and TAIPAN, which are expected to detect BAO peaks and constrain the Hubble constant with 3% precision. The 6dFGS results are compared to other studies, showing that the BAO signal is consistent with $ \Lambda $ CDM predictions. The study concludes that the 6dFGS results provide a robust measurement of the distance scale and the Hubble constant, with implications for constraining cosmological parameters.