3.3.18  :  Henriques2015a

The database Henriques2015a contains standard snapshot tables: Henriques2015a.MRscPLANCK and Henriques2015a.MRIIscPLANCK; and pencil-beam like lightcones: Henriques2015a.cones.MRscPlanck1_M05_[001 to 024] (Maraston2005 stellar populations) and Henriques2015a.cones.MRscPlanck1_BC03_[001 to 024] (Bruzual&Charlot2003 stellar populations). It is an update of the Henriques2014a database following the revision by the referee and acceptance of the paper. The galaxy merger trees catalogues were produced by running the semi-analytic code L-Galaxies as described in Henriques et al. 2015, on the NEW PLANCK halo merger trees stored in the MPAHaloTrees database. In addition, there are separate tables containing information on the ages of the STAR FORMATION and METALLICITY HISTORIES bins now available in the main catalogues.

A full description of the galaxy formation model used to produce these catalogues, as well as download links for all predictions and combined observational data plotted in the paper can be found here. For questions related to the model please contact bhenriques@mpa-garching.mpg.de and for questions related to the database please contact lemson@mpa-garching.mpg.de.

Short description of the model: This model is built on subhalo merger trees constructed from the Millennium and Millennium-II simulations after scaling to represent the first-year Planck cosmology. A set of coupled differential equations allow us to follow the evolution of six baryonic components. Five of these are associated with individual galaxies - a hot gas atmosphere, cold interstellar gas, a reservoir of gas ejected in winds, stars split into bulge, disk and intracluster light components, and central supermassive black holes. The sixth, diffuse primordial gas, is associated with dark matter which is not yet part of any halo. Primordial gas falls with the dark matter onto sufficiently massive halos, where it is shock-heated. The efficiency of radiative cooling then determines whether it is added directly to the cold gas of the central galaxy, or resides for a while in a hot gas atmosphere. Cold interstellar gas forms stars both quiescently and in merger-induced starbursts which also drive the growth of central supermassive black holes. Stellar evolution not only determines the photometric appearance of the final galaxy, but also heats and enriches its gas compo- nents, in many cases driving material into the wind reservoir, from which it may later fall back into the galaxy again. Accretion of hot gas onto central black holes gives rise to 'radio-mode'€ feedback, regulating condensation of hot gas onto the galaxy. Environmental processes like tidal and ram-pressure stripping and merging affect the gas components of galaxies, as well as the partition of stars between disks, bulges and the intracluster light, a diffuse component built from tidally disrupted systems. Disk and bulge sizes are estimated form simple energy and angular momentum-based arguments.