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tokens: the methodology of Rowan-Robinson et al. (2005 , 2008) and as in Wang Rowan-Robinson (2009) , with a combination of two cirrus templates, three starburst templates and an AGN dust torus template. The total IR luminosity L IR (integrated between 8 and 1000 μ m) is estimated based on the fitted templates. The methodology of Rowan-Robinson et al. (2008) is followed to calculate stellar masses and SFR. Briefly, the rest-frame 3.6 μ m luminosity is estimated and converted to stellar mass using the mass-to-light ratio derived from stellar synthesis models. To estimate SFR, the conversion recipes of Rowan-Robinson et al. (1997) and Rowan-Robinson (2001) are used where η is the fraction of UV light absorbed by dust, taken as 2/3. The SFRs are calculated for a Salpeter (1955) IMF between 0.1 and 100 M ⊙ . To convert to Kroupa (2001) IMF, we divide the values by 1.5. We can also estimate SFR based on the total IR luminosity L IR following the widely used recipe of Kennicutt (1998) after converting to Kroupa IMF, In principle, the formula of Eq. ( 2 ) is only suitable for dusty starburst galaxies in which all of the radiation from young stars is assumed to be absorbed by dust and subsequently re-emitted in the IR. In practice, Eq. ( 2 ) has been found to also apply to normal galaxies (e.g. Rosa-González et al. 2002 ; Charlot et al. 2002 ). The explanation is that there are two competing effects, which are overestimation in SFR caused by assuming all of the IR luminosity arises from recent star formation (as opposed to old stellar populations) and underestimation in SFR caused by neglecting the possibility that some of the young stellar radiation is not absorbed by dust. It is a coincidence that these two effects cancel out (e.g. Inoue 2002 ; Hirashita et al. 2003 ). For sources in the RIFSCz which have been cross-matched to SDSS DR 10, we also have SFR estimates based on the H α line luminosity, SFR Hα , corrected for dust attenuation and aperture effects provided in the MPA-JPU database ( Brinchmann et al. 2004 ). 2.2. The LOFAR survey Exploiting the unique capabilities of LOFAR ( van Haarlem et al. 2013 ), LoTSS is an ongoing sensitive, high-resolution, low-frequency (120−168 MHz) radio survey of the northern sky and is described in Shimwell et al. (2017) . LoTSS provides the astrometric precision needed for accurate and robust identification of optical and NIR counterparts (e.g. McAlpine et al. 2012 ) and a sensitivity that, for typical radio sources, is superior to previous wide area surveys at higher frequencies such as the NRAO VLA Sky Survey (NVSS; Condon et al. 1998 ) and Faint Images of the Radio Sky at Twenty-Centimeters (FIRST; Becker et al. 1995 ) and is similar to forthcoming higher frequency surveys such as the Evolutionary Map of the Universe (EMU; Norris et al. 2011 ), and the APERture Tile In Focus survey (e.g. Röttgering et al. 2011 ). The primary observational objectives of LoTSS are to reach a sensitivity of less than 100 μ Jy