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We present here the first of a series of papers aimed at better understandingthe evolution and properties of giant molecular clouds (GMCs) in a galacticcontext. We perform high resolution, three-dimensional {\sc arepo} simulationsof an interacting galaxy inspired by the well-observed M51 galaxy. Our fiducialsimulations include a non-equilibrium, time-dependent, chemical network thatfollows the evolution of atomic and molecular hydrogen as well as carbon andoxygen self-consistently. Our calculations also treat gas self-gravity andsubsequent star formation (described by sink particles), and coupled supernovafeedback. In the densest parts of the simulated interstellar medium (ISM) wereach sub-parsec resolution, granting us the ability to resolve individual GMCsand their formation and destruction self-consistently throughout the galaxy. Inthis initial work we focus on the general properties of the ISM with aparticular focus on the cold star-forming gas. We discuss the role of theinteraction with the companion galaxy in generating cold molecular gas andcontrolling stellar birth. We find that while the interaction driveslarge-scale gas flows and induces spiral arms in the galaxy, it is of secondaryimportance in determining gas fractions in the different ISM phases and theoverall star-formation rate. The behaviour of the gas on small GMC scalesinstead is mostly controlled by the self-regulating property of the ISM drivenby coupled feedback.

Simulations of the star-forming molecular gas in an interacting M51-like galaxy