Two-Phase Galaxy Formation

TL;DR

This paper introduces a two-phase galaxy formation model based on the dual modes of halo growth, leading to improved understanding of galaxy components and matching observed properties of local galaxies.

Contribution

It presents a novel galaxy formation scenario incorporating two distinct halo growth phases and their impact on baryonic matter evolution, tested with semi-analytic methods.

Findings

Good agreement with observed galaxy properties

Supports the two-phase halo growth hypothesis

Models spheroid and disc development effectively

Abstract

We propose and test a scenario for the assembly and evolution of luminous matter in galaxies which substantially differs from that adopted by other semianalytic models. As for the dark matter (DM), we follow the detailed evolution of halos within the canonical LCDM cosmology using standard Montecarlo methods. However, when overlaying prescriptions for baryon evolution, we take into account an effect pointed out in the past few years by a number of studies mostly based on intensive N-body simulations, namely that typical halo growth occurs in two phases: an early, fast collapse phase featuring several major merger events, followed by a late, quiescent accretion onto the halo outskirts. We propose that the two modes of halo growth drive two distinct modes for the evolution of baryonic matter, favoring the development of the spheroidal and disc components of galaxies, respectively. We test this idea using the semianalytic technique. Our galaxy formation model envisages an early coevolution of spheroids and the central supermassive black holes, already tested in our previous works, followed by a relatively quiescent growth of discs around the preformed spheroids. In this exploratory study, we couple our model to the spectrophotometric code GRASIL, and compare our results on several properties of the local galaxy population with observations, Finding an encouraging agreement.