-- The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of the ($\alpha$, $\delta$) position, and can be fitted by a plane in the three--dimensional space ($\alpha$, $\delta$, $v$): the distribution of the galaxy distances around the best fit plane is described by a Gaussian with $\sigma =3.8$ \hmpc.
-- Using the 1440 galaxies of our sample in the magnitude range $17 - 18.8$, we reconstructed the density profile in the central part of the Shapley Concetration and we detected another significant overdensity at $\sim 30000$ km/s.
-- We estimate the total overdensity in galaxies, the mass and the dynamical state of these structures, discussing the effect of considering a bias between the galaxy distribution and the underlying matter. The estimated total overdensity in galaxies of these two structures is $\displaystyle{ N \over \bar{N}}\sim 5.2$ on scale of $15.5$ \hmpc for the Shapley Concentration and $\displaystyle{ N \over \bar{N}} \sim 2.9$ on scale of $24.8$ \hmpc for S300. If light traces the mass distribution, the corresponding masses are $2.3\times 10^{16}$ $\Omega$ h$^{-1}$ M$_{\odot}$ and $5.1\times 10^{16}$ $\Omega$ h$^{-1}$ M$_{\odot}$ for Shapley Concentration and S300, respectively.
The dynamical analysis reveals that, if light traces mass and $\Omega=1$, the Shapley Concentration already reached its turnaround radius and started to collapse: the final collapse will happen in $\sim 3 \ 10^9$ h$^{-1}$ yrs.
-- We compare our mass estimates on various scales with other results in the literature, finding a general agreement.
-- We find an indication that the value of the bias between clusters and galaxies in the Shapley Concentration is higher than that reported in literature, confirming the impression that this supercluster is very rich in clusters.
-- Finally from the comparison with some theoretical scenarios, we find that the Shapley Concentration is consistent with the predictions of the models with more power on large scale (such as Open and $\Lambda$ CDM), while it is inconsistent with the standard CDM normalized to the cluster abundance.
PAPERS
Bi-dimensional distribution of galaxies from the COSMOS catalogue in the central part of the Shapley Concentration. Not the two clusters complexes (dominated by the A3558 and A3528 clusters).