Tidal features of classical Milky Way satellites in a $\Lambda$CDM
  universe
  We use the APOSTLE cosmological hydrodynamic simulations to examine the
effects of tidal stripping on cold dark matter (CDM) sub haloes that host three
of the most luminous Milky Way (MW) dwarf satellite galaxies: Fornax, Sculptor,
and Leo I. We identify simulated satellites that match the observed spatial and
kinematic distributions of stars in these galaxies, and track their evolution
after infall. We find $\sim$ 30$\%$ of subhaloes hosting satellites with
present-day stellar mass $10^6$-$10^8$ $M_{\odot}$ experience $>20\%$ stellar
mass loss after infall. Fornax analogues have earlier infall times compared to
Sculptor and Leo I analogues. Star formation in Fornax analogues continues for
$\sim3$-$6$ Gyr after infall, whereas Sculptor and Leo I analogues stop forming
stars $< 2$-$3$ Gyr after infall. Fornax analogues typically show more
significant stellar mass loss and exhibit stellar tidal tails, whereas Sculptor
and Leo I analogues, which are more deeply embedded in their host DM haloes at
infall, do not show substantial mass loss due to tides. When additionally
comparing the orbital motion of the host subaloes to the measured proper motion
of Fornax we find the matching more difficult; host subhaloes tend to have
pericentres smaller than that measured for Fornax itself. From the kinematic
and orbital data, we estimate that Fornax has lost $10-20\%$ of its infall
stellar mass. Our best estimate for the surface brightness of a stellar tidal
stream associated with Fornax is $\Sigma \sim$ 32.6 mag $ {\rm arcsec^{-2}}$,
which may be detectable with deep imaging surveys such as DES and LSST.
