tracers \[NeII\]+\[NeIII\] and \[CII\]. S05 has a TIR SFR consistent with the other measures from the optical and radio, at 0.71 M$_\sun$yr$^{-1}$, and a lower SFR from \[NeII\]+\[NeIII\] of $<0.09$ M$_\sun$yr$^{-1}$. H02 has a significantly higher TIR SFR, at 4.6 M$_\sun$yr$^{-1}$. However, @Smercina2018 find that the TIR flux is affected by A stellar population heating of the dust, which enhances the SFR estimate by a factor of $\gtrsim 3-4\times$, consistent with TIR being a much longer duration SFR tracer.

The TIR flux could be an even larger overestimate of the true SFR, as @Hayward2014 find the TIR flux overestimates the true SFR by $\gtrsim30\times$ during the post-starburst phase. If AGN heating is important, it would also act to boost the TIR flux, causing this tracer to be an overestimate of the SFR. A TIR SFR for H02 of $\sim 1$ M$_\sun$yr$^{-1}$ with the correction for A star heating would be consistent with the SFR estimated from \[CII\] for H02 (1.3 M$_\sun$yr$^{-1}$), and the 3$\sigma$ upper limit on the 1.4 GHz non-detection (1.8 M$_\sun$yr$^{-1}$).

Thus, the SFRs from various tracers are consistent with a range of 0.09 (H$\alpha$) - 1 (TIR) M$_\sun$yr$^{-1}$ for H02, and 0.58 M$_\sun$yr$^{-1}$ or less for S05. 