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In order to examine the far‐infrared (far‐IR)/radio correlation at high redshift, we have studied the  Spitzer  70 μm /far‐IR properties of sub‐mJy radio sources from the  13 H   XMM–Newton/Chandra  Deep Field by redshift and galaxy type: active galactic nucleus (AGN) or star‐forming galaxy (SFG). We directly detect  70 μm  counterparts (at  &gt;3σ  significance) for 22.5 per cent (92/408) of the radio sources, while for the rest we perform stacking analysis by redshift and galaxy type. For the sources detected at  70 μm , we find that the median and scatter of the observed flux density ratio,  q  70 , are similar to previous results in the literature, but with a slight decrease in  q  70  towards higher redshifts. Of the radio sources detected at  70 μm 8/92  were already classified as AGN, but two of which maybe SFGs. For the stacked sources, we obtain a detection for the SFGs at every redshift bin which implies they have mean flux densities a factor ∼5 below the original  70 μm  detection limit. For the stacked AGN, we obtain a detection only in our highest redshift bin  (1 ≤ z ≤ 5)  where we may be sampling hot dust associated with the AGN at rest frame  12−35 μm . The combined observed mean value of  q 70   for the SFGs (detected and non‐detected at  70 μm ) decreases gradually with redshift, consistent with tracks derived from empirical spectral energy distributions (SEDs) of local SFGs. Upon closer inspection and when comparing with tracks of appropriate luminosity, the values of  q 70   broadly agree at low redshift. However, at   z ∼ 1 , the observed  q  70 [for ultraluminous infrared galaxies (ULIRGs)] is  2 σ  below the value seen for local ULIRGs tracks, implying a difference in the SED between local and   z ∼ 1  ULIRGs. At higher redshifts, the convergence of the tracks and the higher uncertainties in  q  70  do not allow us to determine if such a difference persists.

Investigating the far‐IR/radio correlation of star‐forming Galaxies to z = 3