The source of the discrepant SFRs for H02 between the low H$\alpha$ and even D$_n(4000)$ - derived values and the high IR - derived values could be either (1) an underestimate of the extinction compared to what is measured using the Balmer decrement, or (2) an underestimate of the dust heating from sources other than star formation, or a combination of both. The dust masses for the two galaxies are similar ($log$M$_{\rm dust} = 6.86 \pm 0.90, 7.00 \pm 0.16$ for H02 and S05 respectively, @Smercina2018), so if the extinction is much higher in H02, the geometry must be different. Given the uncertainties in accurately determining the dust heating contribution from AGN or A stars, we adopt a conservative upper limit of $<1$ M$_\sun$yr$^{-1}$ on the SFR of H02. We consider the effect of this uncertainty in the SFR of H02 in §\[sec:results\].

Results {#sec:results}
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We calculate the dense gas line luminosities using $$L^{\prime}_{line} = 3.25\times10^7 (1+z)^{-3} \ \nu_{\rm obs}^{-2} \ S_{line} \Delta v \ D_L^2$$ where $L^{\prime}$ is the line luminosity in Kkms$^{-1}$pc$^2$, $z$ is the redshift, $\nu_{\rm obs}$ is the observed line frequency in GHz, $S_{line}  \Delta v$ is the integrated flux density in Jy km/s, and 