The morgana model for the rise of galaxies and active nuclei

By P. Monaco, F. Fontanot, Giuliano Taffoni Daut, U. D. T. -. I. I. -. O. A. Mpia, Heidelberg · Germany. 2006

209 citations recorded by the source corpus.

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

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei (2008, methodology): “When Zibetti adopts the same decomposition method as Gonzalez, he finds much more consistent values f DSH 0.67 (Zibetti 2008). solve the overcooling problem and other related problems (Bower et al. 2006; Croton et al. 2006; Monaco et al. 2007).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “Other SAMs use similar scalings, some with more attempted explicit connection with the invoked physical processes and/or with observations (e.g. Monaco et al. 2007, Somerville et al. 2008), but these appear to produce similar results at z = 0, and even for the redshift evolution of massive galaxies…”
The Hierarchical Build-Up of Massive Galaxies and the Intracluster Light since z = 1 (2007, result): “Our approach is similar in spirit to that of a recent study by Monaco et al. (2006), who used theMORGANASAM (Monaco et al. 2007) to follow the evolution of galaxies.”
The correlation of star formation quenching with internal galaxy properties and environment (2008, methodology): “The others are the Millennium models (Croton et al. 2006; De Lucia et al. 2006, hereafter dL06) and the MORGANA (MOdel for the Rise of GAlaxies aNd Active nuclei) models (Fontanot et al. 2006, 2007; Monaco et al. 2007).”
Galaxy formation theory (2010, background): “Since then numerous studie(Kauffmann et al. 1993; Baugh et al. 1999b, 1998; Somerville and Primack 1999; Cole et al. 2000; Benson et al. 2002a; Hatton et al. 2003; Monaco et al. 2007) have extended and improved this original framework.”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “However, we have compared with a number of other such models and find similar results (including e.g. Benson et al. 2003; Baugh et al. 2005; Kang et al. 2005; Cattaneo et al. 2006; Monaco et al. 2007; Bertone et al. 2007).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, background): “Disk formation and semi-analytic models still struggle to simultaneously reproduce the TF relation (a subset of the LV relation) and the abundance of galaxies (e.g., Benson et al. 2003; Monaco et al. 2007; Benson & Bower 2010).”
A census of metals and baryons in stars in the local universe (2007, background): “Model predictions are from (12) Pei et al. (1999), (13) Calura & Matteucci (2004), (14) Monaco et al. (2007), (15) Nagamine et al. (2006) and integration of the analytic fit of Cole et al. (2001) to ρ̇∗ data of Steidel et al. (1999) (16) (the two values are without and with correction for dust…”
THE NON-CAUSAL ORIGIN OF THE BLACK-HOLE–GALAXY SCALING RELATIONS (2010, methodology): “The orbital parameters of the halo are extracted from suitable distributions that reproduce the results of Nbody simulations as described in Monaco et al. (2007).”
A new measurement of the evolving near-infrared galaxy luminosity function out to z≃ 4: a continuing challenge to theoretical models of galaxy formation (2008, methodology): “This nuclear feedback was first successfully introduced into a cosmological framework of galaxy formation by Granato et al. (2001, 2004) and then implemented by many other authors (e.g. Di Matteo et al. 2005; Croton et al. 2006; Bower et al. 2006; Menci et al 2006; Monaco et al. 2007).”
zCOSMOS – 10k-bright spectroscopic sample - The bimodality in the galaxy stellar mass function: exploring its evolution with redshift (2009, methodology): “…the baryonic component, such as its star-formation history/timescale, of the role of feedback, dust content, and/or AGN feedback (Menci et al. 2006; Monaco et al. 2007; Bower et al. 2006), and the introduction of the uncertainties in the mass determination, may help to reduce the disagreement…”
Galacticus: A Semi-Analytic Model of Galaxy Formation (2010, methodology): “such models were ﬁrst contemplated by White and Rees (1978) and have since been developed further, notably by White and Frenk (1991), Kaumann et al. (1993), Cole et al. (2000), Hatton et al. (2003), Monaco et al. (2007), Somerville et al. (2008) among others. Models of this type aim to begin with th”
Dynamical friction and galaxy merging time-scales (2007, result): “Our results can be compared to the fitting formulae provided by Taffoni et al. (2003) [and updated by Monaco et al. 2007], which are valid for 0.3 ≤ rc(E)/rvir ≤ 0.9.”