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We report the detection of the far-infrared (FIR) fine-structure line ofsingly ionised nitrogen, \Nplusa, within the peak epoch of galaxy assembly,from a strongly lensed galaxy, hereafter ``The Red Radio Ring''; the RRR, at z= 2.55. We combine new observations of the ground-state and mid-J transitionsof CO (J$_{\rm up} =$ 1,5,8), and the FIR spectral energy distribution (SED),to explore the multi-phase interstellar medium (ISM) properties of the RRR. Allline profiles suggest that the HII regions, traced by \Nplusa, and the (diffuseand dense) molecular gas, traced by the CO, are co-spatial when averaged overkpc-sized regions. Using its mid-IR-to-millimetre (mm) SED, we derive anon-negligible dust attenuation of the \Nplusa line emission. Assuming auniform dust screen approximation results a mean molecular gas column density$> 10^{24}$\, cm$^{-2}$, with a molecular gas-to-dust mass ratio of 100. It isclear that dust attenuation corrections should be accounted for when studyingFIR fine-structure lines in such systems. The attenuation corrected ratio of$L_{\rm NII205} / L_{\rm IR(8-1000\mu m)} = 2.7 \times 10^{-4}$ is consistentwith the dispersion of local and $z >$ 4 SFGs. We find that the lower-limit,\Nplusa -based star-formation rate (SFR) is less than the IR-derived SFR by afactor of four. Finally, the dust SED, CO line SED and $L_{\rm NII205}$line-to-IR luminosity ratio of the RRR is consistent with a starburst-poweredISM.

The "Red Radio Ring": Ionised and Molecular Gas in a Starburst/Active Galactic Nucleus at $z \sim 2.55$