Empirical models of the incident Poynting flux (PF), associated with auroral processes, have been separately constructed for the northern and southern hemispheres using data from the Fast Auroral SnapshoT (FAST) satellite (Carlson et al. (1998)). The models are constructed by fitting a set of basis functions to the PF measured by the electric and magnetic field sensors on board FAST (Ergun et al. (2001);Elphic et al. (2001)), where the basis function coefficients are expressed as quadratic equations in a chosen set of geophysical parameters. The modeling methodology was explained in detail by Cosgrove et al. (2014), and has changed very little. Basis functions are constructed from the data as empirical orthogonal functions, and are used to describe variations from a background state that is essentially an IMF-average. However, the lead author has recently put the data itself through a process of quality control that has reduced the number of orbits deemed useable from 8,085 to 7,301 for the NH, and from 5,501 to 4,953 for the SH, with the benefit of providing additional confidence in the results presented here (which were noted earlier, but not published). Some details concerning the quality control process are given in the Supporting Information S1.The models output flux maps for the regions above 60° magnetic latitude (MLAT) and below − 60° MLAT as a function of (a) clock angle of the interplanetary magnetic field (IMF), (b) magnitude of the IMF in the GSM y-z