The Distribution of Gas in the Local Group: Results form Contsrained Simulations

F. PARISI; C. SCANNAPIECO; S. NUZA; S. GOTTLÖBER

Potsdam

Workshop; Structure of the Cosmic Web; 2012

Leibniz-Institut für Astrophysik Potsdam (AIP)

In this work we study the gas distribution around and between the Milky Way (MW) and M31 galaxies, as well as its history, using the CLUES  simulations. We first analyze the properties of the gas in each galaxy halo at z=0, namely, its spatial distribution (focusing on whether there is some excess inbetween the two galaxies), temperature, accretion modes and rates, etc.  We then look at the higher redshift distribution to show the gas evolution for this "Very Local Group". We discuss three different stages in its history, namely, an early epoch (redshifts greater than z = 1.2) when the two young galaxies are not connected and relay in different filaments, a second one (for z between 1.2 and 0.5) where they belong to the same filament, and a third recent stage (z<0.5) where they are again disconnected (in the sense that they do not share filament) but with a gas distribution that shows an excess in the region between them. We also study the interaction during their formation history, in particular, if the MW and M31 galaxies have interchanged gas material