We present observations of the Pisces A and B galaxies with the on the . Photometry from these images clearly resolve a for both objects , demonstrating that they are nearby dwarf galaxies . We describe a Bayesian inferential approach to determining the distance to these galaxies using the magnitude of the , and then apply this approach to these galaxies . This reveals the distance to these galaxies as 5.64 ^ { +0.13 } _ { -0.15 } { Mpc } and 8.89 ^ { +0.75 } _ { -0.85 } { Mpc } for Pisces A and B , respectively , placing both within the Local Volume but not the Local Group . We estimate the \aclp SFH of these galaxies , which suggests that they have recently undergone an increase in their star formation rates . Together these yield luminosities for Pisces A and B of M _ { V } = -11.57 ^ { +0.06 } _ { -0.05 } and -12.9 \pm 0.2 , respectively , and estimated stellar masses of \log ( M _ { * } / M _ { \odot } ) = 7.0 ^ { +0.4 } _ { -1.7 } and 7.5 ^ { +0.3 } _ { -1.8 } . We further show that these galaxies are likely at the boundary between nearby voids and higher-density filamentary structure . This suggests that they are entering a higher-density region from voids , where they would have experienced delayed evolution , consistent with their recent increased star formation rates . If this is indeed the case , they are useful for study as proxies of the galaxies that later evolved into typical satellite galaxies .