the SF mechanism becomes less effective when going to lower masses: dwarfs with stellar mass $<10^{5}-10^{7}M_{\odot}$ have fewer stars and thus they contain, as a consequence, less supernovae explosions than dwarfs with stellar mass $>10^{7}M_{\odot}$ (Governato et al. 2012).

Evaluation of luminous satellites
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The previous section exposed how baryonic corrections to dissipationless N-body simulations reduce the number of massive satellites. We are then left with the task to determine whether indeed the baryonic corrections also reduce the number of luminous satellites that are expected in dissipationless N-body simulations, and in particular to the satellites in VL2, and if this number is in agreement with those observed in the MW. In order to check this, other corrections are needed.

Our correction (Eq. \[eq:mia\]), in the same way as the Z12 correction, produces satellites that reach $z=0$ with their central $v_{c}$ reduced by baryonic physics. However, some satellites are destroyed (by e.g. stripping or photo-heating) before $z=0$. In N-body simulations, like the VL2, baryonic effects are not taken into account. In the real universe, or even SPH simulations, enhanced tidal stripping (due to the presence of a disc) may totally destroy some of the satellites seen in those N-body simulations. Our 