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In the upcoming months I plan to run a suite of simulations of much higher volume than the ones conducted in the past twelve months used for testing the modifications to the codes in the pipeline.\\  With those we will be able to study the imprint of a set of models on the non-linear clustering of dark matter. This will be possible thanks to the improved resolution that will allow to measure the Power Spectrum with high precision on both large and small scales to quantify the non-linear signatures of the models. Then the extension of the new halo catalogues will provide a smoother realization of the halo mass function even at higher redshift, allowing us to investigate possible differences in the high redshift statistics, those will allow to shed light on problems like the Missing Satellite Problem or the Too Big to Fail problem by concentrating on Milky Way-sized halos. We will also get better statistics about important properties of Dark Matter Halos such as concentration, velocity dispersion and mass accretion history that will give us important insights into the new dynamics induced by different gravitational interactions and screening mechanism simulated. Those results will be summarized in my first paper.\\   Following this analysis and with the same dataset it will be possible to run the semi-analytical model of galaxy formation created by Darren Croton. This will then allow to compare the size of differences in galactic properties induced by the underlying dark energy model. The extent of the new galaxy catalogue will provide enough statistics up to redshift $z=6$ to study the evolution of the stellar mass function, correlation function, stellar mass density and star formation rate density. This analysis will be the first step towards producing a specific dataset that will allow direct comparision with observations once they will be publicily available trough the Theoretical Astrophysical Observatory [ ] and this will be the main focus of my second paper.\\  Another interesting project I would like to pursue is one that concerns the necessity to have multiple realization of the same model simulation using different initial conditions to build many mock catalogues and quantify the cosmic variance using covariance matrices to get a more robust predictions. Due to the computational costs this is currently unfeasible using full blown cosmological N-body simulations. Recent developments though allow to get many realization using a tecnique called Comoving Lagrangian Acceleration (COLA) [ ] that provides an accuracy comparable to that of N-Body simulations on large scale by smoothing over the details on the smaller scales. This could be coupled with a recently developed approximation technique that allows to simulate Modified Gravity Theories without resorting to solve the full field equations [ ] that showed promising results. I would like to investigate if it's possible to combine the two approaches and I think this would be eased by the fact that the COLA code was improved and completed here at CAS by Jun Koda and his team. This could led to the inclusion of Modified Gravity mock catalogues in the observational pipelines and allow to hilight possible signature and constrain each models'parameters with an unprecedented precision.