and 31 of class C, have only a single $\gamma$-ray blazar candidate within the SR. In Figure \[fig:strip\_pln1\] we show the [[*WISE*]{}]{} colors of the 156 $\gamma$-ray blazar candidates in comparison with those of the blazars in the 2FB sample for the \[3.4\]-\[4.6\]-\[12\] $\mu$m 2D projection of the [[*WGS*]{}]{}.

![The \[3.4\]-\[4.6\]-\[12\] $\mu$m 2D projection of the [[*WGS*]{}]{} is shown. Red dashed lines show the boundaries of the [[*WGS*]{}]{} used in our analysis (see Paper III for more details). The orange background filled circles are the blazars associated with the 2FGL constituting the 2FB sample while the balck filled circles indicate the 156 $\gamma$-ray blazars that have been associated by our procedure.[]{data-label="fig:strip_pln1"}](./strip_pln1.pdf){height="6.0cm" width="9.7cm"}

By restricting our sample of UGSs only to those at high Galactic latitudes, i.e. $|b|>$15$^\circ$, we found a $\gamma$-ray blazar candidate for 72 UGSs, 16 of class A, 29 of class B and 27 of class C; where for 34 out of these 74, the low energy counterpart associated with our method is univocal.

![The distribution of the Galactic latitude for all the UGSs analyzed in comparison with that for the 156 associated by our procedure.[]{data-label="fig:glat_distrib"}](./glat_distrib.pdf){height="6.0cm" width="9.7cm"}

In Figure \[fig:glat\_distrib\], we shown the distribution of the Galactic latitude 