Context : We use the GALEX data of the GUViCS survey to construct the NUV luminosity function of the Virgo cluster over \sim 300 deg . ^ { 2 } , an area covering the cluster and its surrounding regions up to \sim 1.8 virial radii .
The NUV luminosity function is also determined for galaxies of different morphological type and NUV - i colour , and for the different substructures within the cluster .
These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift ( 808 ) or high-quality optical scaling relations ( 10 ) .
We fit these luminosity functions with a Schechter function , and compare the fitted parameters with those determined for other nearby clusters and for the field .
The faint end slope of the Virgo NUV luminosity function ( \alpha = -1.19 ) , here sampled down to \sim NUV = -11.5 mag , is significantly flatter than the one measured in other nearby clusters and similar to the field one .
Similarly M ^ { * } = -17.56 is one-to-two magnitudes fainter than measured in Coma , A1367 , the Shapley supercluster , and the field .
These differences seem due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters .
We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery .
We notice , however , that the relative contribution of red-to-blue galaxies at the faint end is inverted , with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius .
These observational evidences are discussed in the framework of galaxy evolution in dense environments .

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