We apply the scale-length method to several three dimensional samples of the Two degree Field Galaxy Redshift Survey .
This method allows us to map in a quantitative and powerful way large scale structures in the distribution of galaxies controlling systematic effects .
By determining the probability density function of conditional fluctuations we show that large scale structures are quite typical and correspond to large fluctuations in the galaxy density field .
We do not find a convergence to homogeneity up to the samples sizes , i.e . \approx 75 Mpc/h .
We then measure , at scales r \mathrel { \hbox to 0.0 pt { \lower 3.0 pt \hbox { $ \mathchar 536 $ } \hss } \raise 2.0 pt% \hbox { $ \mathchar 316 $ } } 40 Mpc/h , a well defined and statistically stable power-law behavior of the average number of galaxies in spheres , with fractal dimension D = 2.2 \pm 0.2 .
We point out that standard models of structure formation are unable to explain the existence of the large fluctuations in the galaxy density field detected in these samples .
This conclusion is reached in two ways : by considering the scale , determined by the linear perturbation analysis of a self-gravitating fluid , below which large fluctuations are expected in standard models and through the determination of statistical properties of mock galaxy catalogs generated from cosmological N-body simulations of the Millenium consortitum