| Abstract
| - Abstract. We discuss how different theoretical predictions for the variance σ2 of the counts-in-cells distribution of radio sources can be matched to measurements from the FIRST survey at different flux limits. The predictions are given by the integration of models for the angular correlation function w(θ) for three different functional forms of the redshift distribution N(z), different spatial correlation functions that match the observed present-day shape and by different evolutions of the bias b(z) with redshift. We also consider the two cases of open and flat universes. Although the predicted w(θ) show substantial differences because of differences in the values of N(z), these differences are not significant compared to the uncertainties in the current observations. It turns out that, independent of the geometry of the universe and the flux limit, the best fit is provided by models with constant biasing at all times, although the difference between models with epoch-independent bias and models with bias that evolves linearly with redshift is not very large. All models with strong evolution of bias with epoch are ruled out, as they grossly overestimate the amplitude of the variance over the whole range of angular scales sampled by the counts-in-cells analysis. As a further step we directly calculated wobs(θ) at 3 mJy from the catalogue and matched it with our models for the angular correlation function, in the hypothesis that the clustering signal comes from two different populations, namely AGN-powered sources and starbursting galaxies. The results are consistent with a scenario for hierarchical clustering where the fainter starbursting galaxies trace the mass at all epochs, while the brighter AGNs are strongly biased, with b(z) evolving linearly with redshift, as suggested by some theories of galaxy formation and evolution.
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