The morgana model for the rise of galaxies and active nuclei

摘要: We present the Model for Rise of Galaxies and Active Nuclei (MORGANA), a new code formation evolution galaxies active galactic nuclei (AGNs). Starting from merger trees dark matter (DM) haloes model substructure within haloes, complex physics baryons is modelled with set state-of-the-art models that describe mass, metal energy flows between various components (baryonic halo, bulge, disc) phases (cold hot gas, stars) galaxy. These are then numerically integrated to produce predictions galaxies. The processes shock-heating cooling, star formation, feedback, winds superwinds, accretion on black holes AGN feedback described by models. In particular, halo gas explicitly follows thermal kinetic energies cold phases, while follow results multiphase recently proposed Monaco. increased level sophistication these allows move phenomenological description physics, based simple scalings depth DM potential, towards fully physically motivated one. deem this justified maturity rough convergence reached latest versions numerical semi-analytic galaxy formation. comparison MORGANA basic data reveals one hand an overall agreement, other highlights number well- or less-known problems: (i) producing cut-off luminosity function requires force quenching late cooling (ii) normalization Tully‐Fisher relation local spirals cannot be recovered unless assumed have very low concentration, (iii) mass H I not easily fitted at small masses, similarly concentration assumed, (iv) there excess elliptical z = 0. discrepancies, more than points agreement data, give important clues missing ingredients