Dust in and around galaxies: dust in cluster environments and its impact on gas cooling. (arXiv:1811.05477v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Vogelsberger_M/0/1/0/all/0/1">Mark Vogelsberger</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+McKinnon_R/0/1/0/all/0/1">Ryan McKinnon</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+ONeil_S/0/1/0/all/0/1">Stephanie O&#x27;Neil</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Marinacci_F/0/1/0/all/0/1">Federico Marinacci</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Torrey_P/0/1/0/all/0/1">Paul Torrey</a> (1,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Kannan_R/0/1/0/all/0/1">Rahul Kannan</a> (1,2) ((1) MIT, (2) CfA/Harvard, (3) UF)

Simulating the dust content of galaxies and their surrounding gas is
challenging due to the wide range of physical processes affecting the dust
evolution. Here we present cosmological hydrodynamical simulations of a cluster
of galaxies, $M_text{200,crit}=6 times 10^{14},{rm M}odot$, including a
novel dust model for the moving mesh code Arepo. This model includes dust
production, growth, supernova-shock-driven destruction, ion-collision-driven
thermal sputtering, and high temperature dust cooling through far infrared
re-radiation of collisionally deposited electron energies. Consistent with
observations we predict a present-day overall dust-to-gas ratio of $sim
2times 10^{-5}$, a total dust mass of $sim 2times 10^9,{rm M}odot$ and a
dust mass fraction of $sim 3times 10^{-6}$. The typical thermal sputtering
timescales within $sim 100,{rm kpc}$ are around $sim 10,{rm Myr}$, and
increase towards the outer parts of the cluster to $sim 10^3,{rm Myr}$ at a
cluster-centric distance of $1,{rm Mpc}$. The condensation of gas phase
metals into dust grains reduces high temperature metal-line cooling, but also
leads to additional dust infrared cooling. The additional infrared cooling
changes the overall cooling rate in the outer parts of the cluster, beyond
$sim 500,{rm kpc}$, by $10% – 100%$. This results in noticeable changes of
the entropy, temperature, and density profiles of cluster gas once dust
formation is included. The emitted dust infrared emission due to dust cooling
is consistent with observational constraints reaching a total bolometric IR
cooling luminosity of about $L_{rm IR, cool} sim 2times 10^{10},{rm
L}_odot$. We conclude that dust can survive sufficiently long in the
intracluster medium to reach a small but significant abundance with
implications for the thermodynamic properties of the cluster.

Simulating the dust content of galaxies and their surrounding gas is
challenging due to the wide range of physical processes affecting the dust
evolution. Here we present cosmological hydrodynamical simulations of a cluster
of galaxies, $M_text{200,crit}=6 times 10^{14},{rm M}odot$, including a
novel dust model for the moving mesh code Arepo. This model includes dust
production, growth, supernova-shock-driven destruction, ion-collision-driven
thermal sputtering, and high temperature dust cooling through far infrared
re-radiation of collisionally deposited electron energies. Consistent with
observations we predict a present-day overall dust-to-gas ratio of $sim
2times 10^{-5}$, a total dust mass of $sim 2times 10^9,{rm M}odot$ and a
dust mass fraction of $sim 3times 10^{-6}$. The typical thermal sputtering
timescales within $sim 100,{rm kpc}$ are around $sim 10,{rm Myr}$, and
increase towards the outer parts of the cluster to $sim 10^3,{rm Myr}$ at a
cluster-centric distance of $1,{rm Mpc}$. The condensation of gas phase
metals into dust grains reduces high temperature metal-line cooling, but also
leads to additional dust infrared cooling. The additional infrared cooling
changes the overall cooling rate in the outer parts of the cluster, beyond
$sim 500,{rm kpc}$, by $10% – 100%$. This results in noticeable changes of
the entropy, temperature, and density profiles of cluster gas once dust
formation is included. The emitted dust infrared emission due to dust cooling
is consistent with observational constraints reaching a total bolometric IR
cooling luminosity of about $L_{rm IR, cool} sim 2times 10^{10},{rm
L}_odot$. We conclude that dust can survive sufficiently long in the
intracluster medium to reach a small but significant abundance with
implications for the thermodynamic properties of the cluster.

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