tokens: reduced to a negligible percentage (Magliocchetti etal. 2002 ; Mauch Sadler 2007 ). We then distinguished between AGN-powered galaxies and star-forming galaxies by means of equation ( 1 ) for z 1.8 and by fixing log 10 P cross ( z )23.5 [W Hz 1 sr 1 ] at higher redshifts. This procedure identifies 704 AGNs (corresponding to 33percent of the total radio population) and 1419 star-forming galaxies. With respect to our earlier work, these numbers imply an increase of a third of sources in both the AGN and the SF samples and allow us to draw conclusions on the properties of radio-selected sources with and without an FIR counterpart on much more solid grounds. Also, note that, due to the adopted selection criteria and thanks to the depth of the VLA-COSMOS survey, the AGN samples are complete with respect to radio selection at all redshifts z 3.5, i.e. the considered sample includes all radio-emitting AGNs selected at 1.4 GHz in the COSMOS field and endowed with a redshift determination z 3.5. 272 sources classified as AGNs and 901 sources classified as star-forming galaxies also show up in the Herschel maps. The redshift distribution of radio-selected AGNs is presented in Fig. 1 . The filled histogram shows the distribution of all AGNs, independent of their FIR emission, while the dashed (red) histogram represents that of those AGNs which also appear in the Herschel maps. The bottom panel highlights the ratio between these two quantities. Errorbars correspond to 1 Poissonian estimates. As already seen in Magliocchetti etal. ( 2014 ), also in the present case we have that the redshift distribution of radio-selected AGNs presents a marked peak at a redshift z 1. However, the better statistics of the present data allow us to identify a prominent tail which extends up to z 3.54 and which in Magliocchetti etal. ( 2014 ) only showed up as a secondary peak centred around z 2.5. There is no functional difference between the distribution of the parent AGN population and that which corresponds to AGNs with an FIR counterpart. One is the scaled version of the other, and the ratio between these two quantities is roughly constant and equal to the value of 0.5 throughout the whole redshift range probed by our data. Figure 1. Redshift distribution of COSMOS-VLA radio-selected AGNs with fluxes F 1.4GHz 0.06mJy. The AGN sample is complete up to z 3.5. The solid line represents all sources irrespective of their FIR emission, while the dashed line indicates those objects which are also FIR emitters. The bottom panel highlights the ratio between the two quantities. Errorbars correspond to 1 Poissonian estimates. Some more information on the sources under exam can be provided by investigations of the distribution of their radio luminosities, both in the presence and in absence of FIR emission. This is shown in Fig. 2 , whereby the left-hand plot shows the distribution of sources at all redshifts, while the one on the right-hand side that of sources divided into
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