The place of the Milky Way and Andromeda in the Cosmic Web

As it has been widely demonstrated from observations and cosmological simulations, the present universe harbours a complex large-scale structure of entangled filaments of clumped matter permeated by vast low-density regions. This structure is called comic web and is one of the mainly emergent features of the non-linear regime of the universe. Numerous studies have been performed aimed to quantify the effects of the cosmic web on different physical properties of systems like dark matter halos, galaxies and galaxy clusters. Some important correlations have already been found for some of those properties, such as the mass of the halos, the spin parameter and their shape. There is also a growing interest in studying the properties of the local group of galaxies (dominated gravitationally by the Milky Way and Andromeda galaxy) in a cosmological context as a test of the standard cosmological model. Motivated to continue this line of research, the current work is pointed to study LG-like systems in a set of dark matter cosmological simulations in a cosmological context. It is used three constrained simulations (CLUES) aimed to mimic our local environment and an unconstrained simulation (Bolshoi) used for the statistic treatment. As one of the key proposals of this work is to introduce a new method for constructing LG-like systems in simulations by using the V-web scheme to classify the local environment in the constrained simulations. It is demonstrated that the LG-like sample constructed by this way is consistent and has biases in some physical properties with respect to the distribution of halos. Specially, it is found that unlike halos, which are formed in high-density regions, LG-like systems rather lie in low-density regions, like voids and sheets.