Modelling the Canes Venatici I dwarf spheroidal galaxy
  The aim of this work is to find a progenitor for Canes Venatici I (CVn I),
under the assumption that it is a dark matter free object that is undergoing
tidal disruption. With a simple point mass integrator, we searched for an orbit
for this galaxy using its current position, position angle, and radial velocity
in the sky as constraints. The orbit that gives the best results has the pair
of proper motions $\mu_\alpha$ = -0.099 mas yr$^{-1}$ and $\mu_\delta$ = -0.147
mas yr$^{-1}$, that is an apogalactic distance of 242.79 kpc and a perigalactic
distance of 20.01 kpc. Using a dark matter free progenitor that undergoes tidal
disruption, the best-fitting model matches the final mass, surface brightness,
effective radius, and velocity dispersion of CVn I simultaneously. This model
has an initial Plummer mass of 2.47 x $10^7$ M$_\odot$ and a Plummer radius of
653 pc, producing a remnant after 10 Gyr with a final mass of 2.45 x 10$^5$
M$_\odot$, a central surface brightness of 26.9 mag arcsec$^{-2}$, an effective
radius of 545.7 pc, and a velocity dispersion with the value 7.58 km s$^{-1}$.
Furthermore, it is matching the position angle and ellipticity of the projected
object in the sky.
