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Dwarf barred galaxies are the perfect candidates for hosting slowly-rotatingbars. They are common in dense environments and they have a relatively shallowpotential well, making them prone to heating by interactions. When aninteraction induces bar formation, the bar should rotate slowly. They reside inmassive and centrally-concentrated dark matter halos, which slow down the barrotation through dynamical friction. While predictions suggest that slow barsshould be common, measurements of bar pattern speed, using theTremaine-Weinberg method, show that bars are mostly fast in the local Universe.We present a photometric and kinematic characterisation of bars hosted by twodwarf galaxies in the Virgo Cluster, NGC 4483 and NGC 4516. We derive the barlength and strength using the Next Generation Virgo Survey imaging and thecircular velocity, bar pattern speed, and rotation rate using spectroscopy fromthe Multi Unit Spectroscopic Explorer. Including the previously studied galaxyIC 3167, we compare the bar properties of the three dwarf galaxies with thoseof their massive counterparts from literature. Bars in the dwarf galaxies areshorter and weaker, and rotate slightly slower with respect to those in massivegalaxies. This could be due to a different bar formation mechanism and/or to alarge dark matter fraction in the centre of dwarf galaxies. We show that it ispossible to push the application of the Tremaine-Weinberg method to the galaxylow mass regime.

The dynamical state of bars in cluster dwarf galaxies: The cases of NGC 4483 and NGC 4516