We analyse the properties of the circum-galactic medium and the relation
between its metal content and that of the stars comprising the central galaxy
in eight hydrodynamical `zoom-in' simulations of disc galaxy formation. The
simulations employ the moving-mesh code AREPO combined with a comprehensive
model for the galaxy formation physics, and succeed in forming realistic
late-type spirals in the set of `Aquarius' initial conditions of Milky
Way-sized haloes. Galactic winds significantly influence the morphology of the
circum-galactic medium and induce bipolar features in the distribution of heavy
elements. They also affect the thermodynamic properties of the circum-galactic
gas by supplying an energy input that sustains its radiative losses. Although a
significant fraction of the heavy elements are transferred from the central
galaxy to the halo, and even beyond the virial radius, the overall stellar
metallicity distribution is broadly consistent with observations, apart from an
overestimate of the O/Fe ratio in our default runs, an effect that can
however be rectified by an increase of the adopted SN type Ia rate. All our
simulations have difficulty in producing stellar metallicity gradients of the
same strength as observed in the Milky Way.
Description
[1403.4934] Diffuse gas properties and stellar metallicities in cosmological simulations of disc galaxy formation
%0 Generic
%1 marinacci2014diffuse
%A Marinacci, Federico
%A Pakmor, Ruediger
%A Springel, Volker
%A Simpson, Christine M.
%D 2014
%K arepo cgm low-z metallicities simulation
%T Diffuse gas properties and stellar metallicities in cosmological
simulations of disc galaxy formation
%U http://arxiv.org/abs/1403.4934
%X We analyse the properties of the circum-galactic medium and the relation
between its metal content and that of the stars comprising the central galaxy
in eight hydrodynamical `zoom-in' simulations of disc galaxy formation. The
simulations employ the moving-mesh code AREPO combined with a comprehensive
model for the galaxy formation physics, and succeed in forming realistic
late-type spirals in the set of `Aquarius' initial conditions of Milky
Way-sized haloes. Galactic winds significantly influence the morphology of the
circum-galactic medium and induce bipolar features in the distribution of heavy
elements. They also affect the thermodynamic properties of the circum-galactic
gas by supplying an energy input that sustains its radiative losses. Although a
significant fraction of the heavy elements are transferred from the central
galaxy to the halo, and even beyond the virial radius, the overall stellar
metallicity distribution is broadly consistent with observations, apart from an
overestimate of the O/Fe ratio in our default runs, an effect that can
however be rectified by an increase of the adopted SN type Ia rate. All our
simulations have difficulty in producing stellar metallicity gradients of the
same strength as observed in the Milky Way.
@misc{marinacci2014diffuse,
abstract = {We analyse the properties of the circum-galactic medium and the relation
between its metal content and that of the stars comprising the central galaxy
in eight hydrodynamical `zoom-in' simulations of disc galaxy formation. The
simulations employ the moving-mesh code AREPO combined with a comprehensive
model for the galaxy formation physics, and succeed in forming realistic
late-type spirals in the set of `Aquarius' initial conditions of Milky
Way-sized haloes. Galactic winds significantly influence the morphology of the
circum-galactic medium and induce bipolar features in the distribution of heavy
elements. They also affect the thermodynamic properties of the circum-galactic
gas by supplying an energy input that sustains its radiative losses. Although a
significant fraction of the heavy elements are transferred from the central
galaxy to the halo, and even beyond the virial radius, the overall stellar
metallicity distribution is broadly consistent with observations, apart from an
overestimate of the [O/Fe] ratio in our default runs, an effect that can
however be rectified by an increase of the adopted SN type Ia rate. All our
simulations have difficulty in producing stellar metallicity gradients of the
same strength as observed in the Milky Way.},
added-at = {2014-03-21T11:49:33.000+0100},
author = {Marinacci, Federico and Pakmor, Ruediger and Springel, Volker and Simpson, Christine M.},
biburl = {https://www.bibsonomy.org/bibtex/2a578ef876120ad72d34342a187549921/miki},
description = {[1403.4934] Diffuse gas properties and stellar metallicities in cosmological simulations of disc galaxy formation},
interhash = {2c6f988c211a7e1bb021e2bd00d64276},
intrahash = {a578ef876120ad72d34342a187549921},
keywords = {arepo cgm low-z metallicities simulation},
note = {cite arxiv:1403.4934Comment: 16 pages, 10 figures, submitted to MNRAS},
timestamp = {2014-03-21T11:49:33.000+0100},
title = {Diffuse gas properties and stellar metallicities in cosmological
simulations of disc galaxy formation},
url = {http://arxiv.org/abs/1403.4934},
year = 2014
}