blazar candidates within the $\gamma$-ray positional error regions of the UGSs. One of the main advantages of our method is that it reduces the number of potential counterparts for the UGSs and provides their positions with arcsec resolution, thus restricting the search regions for future followup observations necessary to confirm their blazar nature. Unfortunately, only a restricted number of UGSs falls within the portion of the sky currently covered by the IR observations of the [[*WISE*]{}]{} Preliminary Data Release corresponding to $\sim$ 57% of the whole sky. Then, when the [[*WISE*]{}]{} survey will be completely released in March 2012[^3], it will be possible to apply the method to the whole sky, even in regions not covered at radio, optical and X-ray frequencies, where the other methods for establishing counterpart associations for the 2FGL cannot be used.

This paper is organized as follows: in Section \[sec:sample\] we describe the samples used in our investigation; in Section \[sec:method\] we illustrate the new association method; then, in Section \[sec:ugs\] we apply the new association technique to the UGSs and describe the subset of sources that has been associated with $\gamma$-ray blazar candidates. In Section \[sec:comparison\], we also compare our results with those found 