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We compare the central mass distribution of galaxies simulated with threedifferent models of the interstellar medium (ISM) with increasing complexity:primordial (H+He) cooling down to 10^4K, additional cooling via metal lines andto lower temperatures, and molecular hydrogen (H_2) with shielding of atomicand molecular hydrogen, in addition to metal line cooling. In order to analyzethe effect of these models, we follow the evolution of four field galaxies withV_peak < 120 km/s to a redshift of zero using high-resolution Smoothed ParticleHydrodynamic simulations in a fully cosmological LCDM context. The spiralgalaxies produced in simulations with either primordial cooling or H_2 physicshave realistic, rising rotation curves. In contrast, the simulations with metalline cooling and otherwise similar feedback and star formation producedgalaxies with the peaked rotation curves typical of most previous LCDMsimulations of spiral galaxies. The less-massive bulges and non-peaked rotationcurves in the galaxies simulated with primordial cooling or H_2 are linked tochanges in the angular momentum distribution of the baryons. These galaxies hadsmaller amounts of low-angular momentum baryons because of increased gas lossfrom stellar feedback. When there is only primordial cooling, the star forminggas is hotter and the feedback-heated gas cools more slowly than when metalline cooling is included and so requires less energy to be expelled. When H_2is included, the accompanying shielding produces large amounts of clumpy, coldgas where H_2 forms. Star formation in clumpy gas results in more concentratedsupernova feedback and greater efficiency of mass loss. The higher feedbackefficiency causes a decrease of low-angular momentum material. (abridged)

The effect of models of the interstellar media on the central mass distribution of galaxies