μ₀−M relation for the Local Group and Centaurus group galaxies. We added nine dwarf candidates (red squares) adopting the distances of background galaxies that were close to the dwarf in the sky. If a candidate is a satellite of the background galaxy, it should follow the same relation as defined by the Centaurus and Local Group dwarfs. We crossed out the candidates that we dismissed as possible background galaxies, meaning that they are more probably Centaurus group members. The candidates that are closer than 1 mag (radial distance) from any known dwarf in the relation could be background dwarf galaxies and are indicated as bg? in Table 1. All such bg? candidates are still outside of the relation, making them unlikely to be background dwarfs; this is why we still present them as possible Centaurus group members.