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Diffuse interstellar bands (DIBs) trace warm neutral and weakly-ionizeddiffuse interstellar medium (ISM). Here we present a dedicated, highsignal-to-noise spectroscopic study of two of the strongest DIBs, at 5780 and5797 \AA, in optical spectra of 666 early-type stars in the Small and LargeMagellanic Clouds, along with measurements of the atomic Na\,{\sc i}\,D andCa\,{\sc ii}\,K lines. The resulting maps show for the first time thedistribution of DIB carriers across large swathes of galaxies, as well as theforeground Milky Way ISM. We confirm the association of the 5797 \AA\ DIB withneutral gas, and the 5780 \AA\ DIB with more translucent gas, generally tracingthe star-forming regions within the Magellanic Clouds. Likewise, the Na\,{\sci}\,D line traces the denser ISM whereas the Ca\,{\sc ii}\,K line traces themore diffuse, warmer gas. The Ca\,{\sc ii}\,K line has an additional componentat $\sim200$--220 km s$^{-1}$ seen towards both Magellanic Clouds; this may beassociated with a pan-Magellanic halo. Both the atomic lines and DIBs showsub-pc-scale structure in the Galactic foreground absorption; the 5780 and 5797\AA\ DIBs show very little correlation on these small scales, as do theCa\,{\sc ii}\,K and Na\,{\sc i}\,D lines. This suggests that good correlationsbetween the 5780 and 5797 \AA\ DIBs, or between Ca\,{\sc ii}\,K and Na\,{\sci}\,D, arise from the superposition of multiple interstellar structures.Similarity in behaviour between DIBs and Na\,{\sc i} in the SMC, LMC and MilkyWay suggests the abundance of DIB carriers scales in proportion to metallicity.

Mapping atomic and diffuse interstellar band absorption across the Magellanic Clouds and the Milky Way