  Dwarf barred galaxies are the perfect candidates for hosting slowly-rotating
bars. They are common in dense environments and they have a relatively shallow
potential well, making them prone to heating by interactions. When an
interaction induces bar formation, the bar should rotate slowly. They reside in
massive and centrally-concentrated dark matter halos, which slow down the bar
rotation through dynamical friction. While predictions suggest that slow bars
should be common, measurements of bar pattern speed, using the
Tremaine-Weinberg method, show that bars are mostly fast in the local Universe.
We present a photometric and kinematic characterisation of bars hosted by two
dwarf galaxies in the Virgo Cluster, NGC 4483 and NGC 4516. We derive the bar
length and strength using the Next Generation Virgo Survey imaging and the
circular velocity, bar pattern speed, and rotation rate using spectroscopy from
the Multi Unit Spectroscopic Explorer. Including the previously studied galaxy
IC 3167, we compare the bar properties of the three dwarf galaxies with those
of their massive counterparts from literature. Bars in the dwarf galaxies are
shorter and weaker, and rotate slightly slower with respect to those in massive
galaxies. This could be due to a different bar formation mechanism and/or to a
large dark matter fraction in the centre of dwarf galaxies. We show that it is
possible to push the application of the Tremaine-Weinberg method to the galaxy
low mass regime.
