Chemical evolution and the galactic habitable zone of M31 (the Andromeda Galaxy)

We have computed the Galactic Habitable Zones (GHZs) of the Andromeda galaxy (M31) based on the probability of terrestrial planet formation, which depends on the metallicity (Z) of the interstellar medium, and the number of formed stars per surface unit. The GHZ was therefore obtained from a chemical evolution model built to reproduce a precise metallicity gradient in the galactic disk, [O/H](r) $ = -0.015 \pm 0.003 dex kpc^{-1} x r(kpc) + 0.44 \pm 0.04 dex $. This gradient is the most probable when intrinsic scatter is present in the observational data. The chemical evolution model predicted a higher star formation history in both the halo and disk components of M31 and a less efficient inside-out galactic formation, compared to those of the Milky Way. If we assumed that Earth-like planets form with a probability law that follows the Z distribution shown by stars with detected planets and the SFH predicted by the CEM, the most probable GHZ per pc$^2$ is located between 3 and 7 kpc for planets with ages between 6 and 7 Gy, approximately. But the highest number of stars with habitable planets is in a ring located between 12 and 14 kpc with mean age of $\sim$7 Gy. 11 % and 6.5 % of the all formed stars in M31 may have planets with basic and complex life, respectively.