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Typical galaxies emit about one third of their energy in the infrared. Theorigin of this emission reprocessed starlight absorbed by interstellar dustgrains and reradiated as thermal emission in the infrared. In particularlydusty galaxies, such as starburst galaxies, the fraction of energy emitted inthe infrared can be as high as 90%. Dust emission is found to be an excellenttracer of the beginning and end stages of a star's life, where dust is beingproduced by post-main-sequence stars, subsequently added to the interstellardust reservoir, and eventually being consumed by star and planet formation.This work reviews the current understanding of the size and properties of thisinterstellar dust reservoir, by using the Large Magellanic Cloud as an example,and what can be learned about the dust properties and star formation ingalaxies from this dust reservoir, using SPICA, building on previous workperformed with the Herschel and Spitzer Space Telescopes, as well as theInfrared Space Observatory.

The interstellar dust reservoir: SPICA's view on dust production and the interstellar medium in galaxies