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The abundance and spatial distribution of dwarf galaxies are excellentempirical benchmarks to test models of structure formation on small scales. Thenearby Centaurus group, with its two subgroups centered on CenA and M83, standsout as an important alternative to the Local Group for scrutinizingcosmological model predictions in a group of galaxies context. We have obtaineddeep optical images of three recently discovered M83 satellite galaxycandidates with the FORS2 instrument mounted on the Very Large Telescope. Weaim to confirm their group membership and study their stellar population. DeepVI-band photometry is used to resolve the brightest stars in our targets.Artificial star tests are performed to estimate the completeness anduncertainties of the photometry. The color-magnitude diagrams reveal the redgiant branch (RGB) stars allowing to use the Sobel edge detection method tomeasure the magnitude of the RGB tip and thus derive distances and groupmembership for our targets. The mean metallicity of the dwarf galaxies arefurther determined by fitting BASTI model isochrones to the mean RGB locus. Weconfirm the two candidates, dw1335-29 and dw1340-30, to be dwarf satellites ofthe M83 subgroup, with estimated distances of 5.03 +- 0.24 Mpc and 5.06 +- 0.24Mpc, respectively. Their respective mean metallicities of <[Fe/H]> = -1.79 +-0.4 and <[Fe/H]> = -2.27 +- 0.4 are consistent with the metallicity-luminosityrelation for dwarf galaxies. The third candidate, dw1325-33, could not beresolved into stars due to insufficiently deep images, implying its distancemust be larger than 5.3 Mpc. Using the two newly derived distances we assessthe spatial distribution of the galaxies in the M83 subgroup and discuss apotential plane-ofsatellites around M83.

Tip of the red giant branch distances to the dwarf galaxies dw1335-29 and dw1340-30 in the Centaurus group