tokens: and H i emission of several radio source populations. Assuming a luminosity dependence for the fractional polarization, O’Sullivan et al. ( 2008 ) realized a simulated polarized image based on the radio source catalogue of Wilman et al. ( 2008 ). Very recently a new simulated catalogue was produced (T-RECS; Bonaldi et al. 2019 ) based on cosmological dark matter simulations to reproduce the clustering of sources and it models the radio sky both in total intensity and polarization with updated information on radio sources. Our simulation, like the above simulations, aims at giving useful information for the advent of the SKA. Similarly, it is based on cosmological RLFs integrated over cosmological volumes but the models adopted to reproduce the characteristics of the radio sources and also the procedure are in general different. In addition, alternative to the previous works, we use observed high-quality images of extended radio sources to reproduce the morphology and the spectro-polarimetric properties of the simulated radio sources. This is especially important as these simulations will be used to study magnetic fields in galaxy clusters (Loi et al. in preparation). For each simulated radio source, our catalogue lists the following parameters: type , in principle we can classify our sources in several subclasses, radio-loud or radio-quiet AGN, SFG, quasar etc. Following Novak et al. ( 2017 ) and Smolčić et al. ( 2017a ) we consider two main families depending on the mechanism that triggers the radio emission: SFG and AGN; redshift , z; size , we used the relations adopted by Wilman et al. ( 2008 ) for radio-loud AGN and SFGs. The size model are redshift-dependent and in particular the SFG size depends also on luminosity; luminosity at 1.4 GHz , we extract this information from the RLFs of Novak et al. ( 2017 ) and Smolčić et al. ( 2017a ) for the SFGs and AGNs, respectively, based on the results of the VLA−COSMOS 3 GHz Large Project (Smolčić et al. 2017b ), extrapolated to 1.4 GHz assuming the spectral index derived in combination with the the VLA−COSMOS 1.4 GHz Large and Deep Projects (Schinnerer et al. 2010 , 2007 , 2004 ); coordinates , (x, y); morphology and spectro-polarimetry properties , we select a model of radio source from a dictionary depending on its luminosity and type. Each model of this dictionary consists of four 1.4 GHz images: the surface brightness I ν in total intensity; the spectral index distribution α determined by assuming that the flux density S ν at a frequency ν is S ν ∝ ν − α ; the fractional polarization defined as the ratio between the polarized intensity and the total intensity FPOL = P / I ; the intrinsic polarization angle which is defined with respect to the Q , and U Stokes parameters as: The images of the dictionary are real high-quality high-resolution images performed at high frequency. In particular, we used VLA images at C and X bands at arcsecond resolution so that the polarization properties
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