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The study of the radio properties of the AMIGA sample is intended tocharacterize the radio continuum emission for a sample least affected by localenvironment, thus providing a reference against which less isolated andinteracting samples can be compared. Radio continuum data at 325, 1420 and 4850MHz were extracted from the WENSS, NVSS/FIRST and GB6 surveys, respectively. Wefocus on the complete AMIGA subsample composed of 719 galaxies. Comparisonbetween the NVSS and FIRST detections indicates that the radio continuum iscoming from disk-dominated emission in spiral galaxies, in contrast to theresults found in high-density environments where nuclear activity is morefrequent. The comparison of the radio continuum power with a comparable sample,which is however not selected with respect to its environment, the Condon etal. UGC-SF sample of star-forming field galaxies, shows a lower mean value forthe AMIGA sample. We have obtained radio-to-optical flux ratios (R) using theNVSS radio continuum flux. The distribution of R for the AMIGA galaxies isconsistent with a sample dominated by radio emission from star formation (SF)and a small number of Active Galactic Nuclei (AGN), with less than 3% of thesample with R > 100. We derived the radio luminosity function (RLF) and totalpower density of the radio continuum emission for the AMIGA sample at 1.4 GHz,and compared them with results from other low redshift studies. The Schechterfit of the RLF indicates a major weight of the low-luminosity galaxies. Theresults indicate the very low level of radio continuum emission in our sampleof isolated galaxies, which is dominated by mild disk SF. It confirms hence theAMIGA sample as a suitable template to effectively quantify the role ofinteractions in samples extracted from denser environments.

The AMIGA sample of isolated galaxies. VI. Radio continuum properties of isolated galaxies: a very radio quiet sample