Dust in and around galaxies: dust in cluster environments and its impact on gas cooling
Name
1811.05477.pdf
Description
Accepted version
Size
5.94 MB
Format
Unknown
Checksum (MD5)
e6d6e1188756f66e6aba76dd51c264a9
Author(s)
Vogelsberger, Mark
McKinnon, Ryan Michael
O’Neil, Stephanie
Marinacci, Federico
Torrey, Paul A.
Kannan, Rahul
Date Issued
2019
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Version
Author's final manuscript
Abstract
© 2019 The Author(s). 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 {200, M ·}, 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 reradiation of collisionally deposited electron energies. Adopting a rather low thermal sputtering rate, we find, consistent with observations, a present-day overall dust-to-gas ratio of ∼2 × 10-5, a total dust mass of {M · }, and a dust mass fraction of ∼3 × 10-6. The typical thermal sputtering time-scales 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 } 1\, {\rm Mpc}, by factors of a few. 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.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
Terms of Use
Creative Commons Attribution-Noncommercial-Share Alike
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1093/MNRAS/STZ1644
