LA-MC-ICP-MS and LA-SC-ICP-MS were used to generate large n (i.e., n = 1000) U–Pb detrital zircon age data sets with little sacrifice of precision and accuracy over more traditional methods.

We use hydrodynamical simulations in a (256 pc) 3 periodic box to model the impact of supernova (SN) explosions on the multi-phase interstellar medium (ISM) for initial densities n = 0.5-30 cm −3 and SN rates 1-720 Myr −1 . We include radiative cooling, diffuse heating, and the formation of molecular gas using a chemical network. The SNe explode either at random positions, at density peaks, or both. We further present a model combining thermal energy for resolved and momentum input for unresolved SNe. Random driving at high SN rates results in hot gas (T 10 6 K) filling > 90% of the volume. This gas reaches high pressures (10 4 < P/k B < 10 7 K cm −3 ) due to the combination of SN explosions in the hot, low density medium and confinement in the periodic box. These pressures move the gas from a two-phase equilibrium to the single-phase, cold branch of the cooling curve. The molecular hydrogen dominates the mass (> 50%), residing in small, dense clumps. Such a model might resemble the dense ISM in high-redshift galaxies. Peak driving results in huge radiative losses, producing a filamentary ISM with virtually no hot gas, and a small molecular hydrogen mass fraction ( 1%). Varying the ratio of peak to random SNe yields ISM properties in between the two extremes, with a sharp transition for equal contributions. The velocity dispersion in Hi remains 10 km s −1 in all cases. For peak driving the velocity dispersion in H α can be as high as 70 km s −1 due to the contribution from young, embedded SN remnants.