2) DMB satellites have flatter profiles than DMOs and thus suffer more tidal stripping (e.g., P10). The same goes between the baryon-richer DMB (filled circles) and baryon-poorer DMB (open circles). The maximum loss happen for DMB satellites in the vicinity of the host galaxy disc.

In Fig. \[fig:Dv-M\], we also plot the analytic fits from Eq. 8 of P10 (see also their Fig. 6), describing the change in $v_{{\rm max}}$ as a function of mass lost due to tidal stripping $$\frac{v_{{\rm max}}(z=0)}{v_{{\rm infall}}}=\frac{2^{\zeta}x^{\eta}}{(1+x)^{\zeta}}
\label{eq:pe}$$ where $x\equiv mass(z=0)/mass(z=infall)$.

The dashed line represents the above equation for central density profile logarithmic slopes $\gamma=1.5$, that corresponds to $\zeta=0.40$ and $\eta=0.24$, the solid line stands for the case $\gamma=1$, for which $\zeta=0.40$ and $\eta=0.30$, and the dotted line covers the case $\gamma=0$, with $\zeta=0.40$ and $\eta=0.37$, respectively.

The $\gamma=1$ curve in Fig. \[fig:Dv-M\] gives a good fit to the change in $v_{{\rm max}}$ for the DMO satellites, and corresponds to cuspy density profiles. Conversely, the $\gamma=0$ curve, that stands for cored profiles, presents a good approximation for the DMB satellites, particularly for those having large baryonic content (i.e., many stars).

Armed with the fit of Eq. (\[eq:pe\]), we propose to determine the VL2 satellites 