The morphology of galaxies is typically characterised either by extensive visual inspection (e.g. Galaxy Zoo project, Lintott et al. 2011) or through the stellar kinematics (e.g. Emsellem et al. 2007). Read More »
Understanding the universal accretion history of dark matter haloes is the first step towards determining the origin of their structure. Previous studies have quantified halo mass accretion histories using catalogues of halos from numerical simulations, in this work (Correa C. A., Wyithe J. S. B., Schaye J., Duffy A. R., 2015a, MNRAS, 450, 1514) we take a different approach. Read More »
One of the major goals of modern galaxy formation theory is to understand the physical mechanisms that halt the star formation process, by either removing, heating or preventing the infall of cold gas onto the galactic disc. X-ray observations suggest that for haloes hosting massive galaxies the majority of baryonic matter resides not in the galaxies, but in the halo in the form of virialized hot gas (e.g. Lin et al. 2003; Crain et al. 2010; Anderson & Bregman 2011). This work (Correa, C. A.; Schaye, J.; Wyithe, J. S. B.; Duffy, A. R.; Theuns, T.; Crain, R. A.; Bower, R. G., MNRAS, 2018, 473, 1) investigates the formation of the hot gaseous corona (also refereed to as ‘hot halo’ or ‘hot atmosphere’) around galaxies, that may help reduce the rate of infall of gas onto galaxies, and has been suggested to explain the observed galaxy bimodality (Dekel & Birnboim 2006).
Over the past few years large cosmological simulations have been performed to determine the properties of dark matter haloes, including density profiles, shapes and accretion histories (see e.g. Bryan et al. 2013; Klypin et al. 2011; Springel et al. 2005). These properties are of particular interest, as forming galaxies depend on the structural properties of the haloes in which they are embedded.
Dark matter halos provide the potential wells inside which galaxies form. As a result, understanding their basic properties, including their formation history and internal structure, is an important step for understanding galaxy evolution. In this work (Correa C. A., Wyithe J. S. B., Schaye J., Duffy A. R., 2015b, MNRAS, 450, 1521) we explore the relation between the dark matter halos internal structure (described by their density profile) and their mass accretion history.