We provide manganese abundances ( corrected for the effect of the hyperfine structure ) for a large number of stars in the dwarf spheroidal galaxies Sculptor and Fornax , and for a smaller number in the Carina and Sextans dSph galaxies . Abundances had already been determined for a number of other elements in these galaxies , including \alpha and iron-peak ones , which allowed us to build [ Mn/Fe ] and [ Mn/ \alpha ] versus [ Fe/H ] diagrams . The Mn abundances imply sub-solar [ Mn/Fe ] ratios for the stars in all four galaxies examined . In Sculptor , [ Mn/Fe ] stays roughly constant between [ Fe/H ] \sim - 1.8 and -1.4 and decreases at higher iron abundance . In Fornax , [ Mn/Fe ] does not vary in any significant way with [ Fe/H ] . The relation between [ Mn/ \alpha ] and [ Fe/H ] for the dSph galaxies is clearly systematically offset from that for the Milky Way , which reflects the different star formation histories of the respective galaxies . The [ Mn/ \alpha ] behavior can be interpreted as a result of the metal-dependent Mn yields of type II and type Ia supernovae . We also computed chemical evolution models for star formation histories matching those determined empirically for Sculptor , Fornax , and Carina , and for the Mn yields of SNe Ia , which were assumed to be either constant or variable with metallicity . The observed [ Mn/Fe ] versus [ Fe/H ] relation in Sculptor , Fornax , and Carina can be reproduced only by the chemical evolution models that include a metallicity-dependent Mn yield from the SNe Ia .