2008MNRAS.386..953I

We have analysed the 24-µm properties of a radio-selected sample in the Subaru-XMM-Newton Deep Field in order to explore the behaviour of the far-infrared/radio (FIR/radio) relation at high redshifts. Statistically, the correlation is described by q₂₄, the ratio between the observed flux densities at 24µm and 1.4GHz, respectively. Using 24-µm data results in considerably more scatter in the correlation than previous work using data at 60-70µm. Nevertheless, we do observe a steady correlation as a function of redshift, up to z ∼ 3.5, suggesting its validity back to primeval times. We find q₂₄= 0.30±0.56 for the observed and q₂₄= 0.71±0.47 for the k-corrected radio sample, based on sources with 300 µJy < S_1.4GHz< 3.2 mJy and 24-µm detections. A suitable k-correction given by a M82-like mid-infrared (mid-IR) template suggests no extreme silicate absorption in the bulk of our radio sample. Using thresholds in q₂₄ to identify radio-excess sources, we have been able to characterize the transition from radio-loud active galactic nuclei (AGN) to star-forming galaxies and radio-quiet AGN at faint (≲1 mJy) radio-flux densities. Our results are in broad agreement with previous studies which show a dominant radio-loud AGN population at >1 mJy. The rest-frame U - B colours of the expected radio-excess population have a redder distribution than those that follow the correlation. This is therefore a promising way to select obscured type 2 AGN, with a radio-loud nature, missed by deep X-ray observations. Spectroscopic follow-up of these sources is required to fully test this method.