  In this letter we present, for the first time, a study of star formation
rate, gas fraction and galaxy morphology of a constrained simulation of the
Milky Way (MW) and Andromeda (M31) galaxies, compared to other MW-mass
galaxies. By combining with unconstrained simulations we cover a sufficient
volume to compare these galaxies environmental densities ranging from the field
to that of the Local Group (LG). This is particularly relevant as it has been
shown that, quite generally, galaxy properties depend intimately upon their
environment, most prominently when galaxies in clusters are compared to those
in the field. For galaxies in loose groups such as the LG, however,
environmental effects have been less clear. We consider the galaxy's
environmental density in spheres of 1200 kpc (comoving) and find that whilst
environment does not appear to directly affect morphology, there is a positive
trend with star formation rates. This enhancement in star formation occurs
systematically for galaxies in higher density environments, regardless whether
they are part of the LG or in filaments. Our simulations suggest that the
richer environment at Mpc-scales may help replenish the star-forming gas,
allowing higher specific star formation rates in galaxies such as the MW.
