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Clumpy disc and bulge formation

ABSTRACT We present a set of hydrodynamical/Nbody controlled simulations of isolated gas richgalaxies that self-consistently include SN feedback and a detailed chemical evolutionmodel, both tested in cosmologicalsimulations. The initial conditions are motivated bythe observedstar forming galaxiesat z ∼2-3. We ﬁnd that the presence of a multiphaseinterstellar media in our models promotes the growth of disc instability favouring theformation of clumps which in general, are not easily disrupted on timescales comparedto the migration time. We show that stellar clumps migrate towards the central regionand contribute to form a classical-like bulge with a Sersic index, n >2. Our physically-motivated Supernova feedback has a mild inﬂuence on clump survival and evolution,partially limiting the mass growth of clumps as the energy released per Supernovaevent is increased, with the consequent ﬂattening of the bulge proﬁle. This regulationdoes not prevent the building of a classical-like bulge even for the most energeticfeedback tested. Our Supernova feedback model is able to establish a self-regulatedstar formation, producing mass-loaded outﬂows and stellar age spreads comparableto observations. We ﬁnd that the bulge formation by clumps may coexit with otherchannels of bulge assembly such as bar and mergers. Our results suggest that galacticbulges could be interpreted as composite systems with structural components andstellar populations storing archaeological information of the dynamical history of theirgalaxy.Key words: galaxies: formation, galaxies: evolution, galaxies: bulges, galaxies: in-teractions.