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We present the results of a series of adiabatic hydrodynamical simulations ofseveral quintessence models (both with a free and an interacting scalar field)in comparison to a standard \LCDM\ cosmology. For each we use $2\times1024^3$particles in a $250$\hMpc\ periodic box assuming WMAP7 cosmology. In this workwe focus on the properties of haloes in the cosmic web at $z=0$. The web isclassified into \emph{voids}, \emph{sheets}, \emph{filaments} and \emph{knots}depending on the eigenvalues of the velocity shear tensor, which are anexcellent proxy for the underlying overdensity distribution. We find that theproperties of objects classified according to their surrounding environmentshows a substantial dependence on the underlying cosmology; for example, while$V_{\rm max}$ shows average deviations of $\approx5$ per cent across thedifferent models when considering the full halo sample, comparing objectsclassified according to their environment, the size of the deviation can be aslarge as $20$ per cent.  We also find that halo spin parameters are positively correlated to thecoupling, whereas halo concentrations show the opposite behaviour. Furthermore,when studying the concentration-mass relation in different environments, wefind that in all cosmologies underdense regions have a larger normalization anda shallower slope. While this behaviour is found to characterize all themodels, differences in the best-fit relations are enhanced in (coupled) darkenergy, thus providing a clearer prediction for this class of models.

Hydrodynamical simulations of coupled and uncoupled quintessence models I: Halo properties and the cosmic web