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19 April 2024 |
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Article overview
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How to get cool in the heat: comparing analytic models of halo gas cooling with EAGLE | | Adam R. H. Stevens
; Claudia del P. Lagos
; Sergio Contreras
; Darren J. Croton
; Nelson D. Padilla
; Matthieu Schaller
; Joop Schaye
; Tom Theuns
; | | Date: |
15 Aug 2016 | | Abstract: | We use the hydrodynamic, cosmological EAGLE simulations to investigate how
hot gas in haloes condenses to form and grow galaxies. We select haloes from
the simulations that are actively cooling and study the temperature,
distribution, and metallicity of their hot, cold, and transitioning ’cooling’
gas, placing these in context of semi-analytic models. Our selection criteria
lead us to focus on Milky Way-like haloes. We find the hot-gas density profiles
of the haloes form a progressively stronger core over time, the nature of which
can be captured by a beta profile that has a simple dependence on redshift. In
contrast, the hot gas that actually cools is broadly consistent with a singular
isothermal sphere. We find that cooling gas carries a few times the specific
angular momentum of the halo and is offset in spin direction from the rest of
the hot gas. The gas loses ~60% of its specific angular momentum during the
cooling process, generally remaining greater than that of the halo, and is
better aligned with the cold gas already in the disc than anything else.
Angular-momentum losses are slightly larger when cooling onto
dispersion-supported galaxies. We show that an exponential surface density
profile for gas arriving on a disc remains a reasonable approximation, but a
cusp is always present, and disc scale radii are larger than predicted by a
vanilla Fall & Efstathiou model. These scale radii are still closely correlated
with the halo spin parameter, for which we suggest an updated prescription for
galaxy formation models. | | Source: | arXiv, 1608.4389 | | Services: | Forum | Review | PDF | Favorites | |
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