Same as Fig. 5 but for the galaxy G70. This latter undergoes a minor merger at z∼0.27. We thus take an interest in three different epochs: in the cosmic gas accretion phase prior the merger (&#Xtextcircled;f), close to the final plunge (&#Xtextcircled;g) and at z = 0.18 or 2.3 Gyr after the removal of the pre-existing disk (&#Xtextcircled;g). At epoch &#Xtextcircled;g, the satellite can be identified in both the ϵ_∗-r-age and ϵ_∗-r-metal diagrams. It is composed of a population of young stars with a global metallicty of log(Z/Z_⊙)∼-0.85 (green color). We note that some of the stars formed in the satellite are accreted by the main galaxy by tidal stripping at &#Xtextcircled;f. Then after the final plunge at epoch &#Xtextcircled;h, the counter-rotating stellar component (ϵ_* < 0) is composed of two main components: the in situ formed stars at r< 7.5 kpc, characterized by a high metalicity, and the stars formed in the satellite displayed at larger radii owing a lower metalicty.