| dc.contributor.author | Cunnama, D. | |
| dc.contributor.author | Power, C. | |
| dc.contributor.author | Elahi, P. J. | |
| dc.date.accessioned | 2021-02-15T07:50:23Z | |
| dc.date.available | 2021-02-15T07:50:23Z | |
| dc.date.issued | 2019 | |
| dc.identifier.citation | Cunnama, D. et al. (2019). NIFTY galaxy cluster simulations – VI. The dynamical imprint of substructure on gaseous cluster outskirts. Monthly Notices of the Royal Astronomical Society, 491(3), 3923–3936 | en_US |
| dc.identifier.issn | 1365-2966 | |
| dc.identifier.uri | https://doi.org/10.1093/mnras/stz3176 | |
| dc.identifier.uri | http://hdl.handle.net/10566/5916 | |
| dc.description.abstract | Galaxy cluster outskirts mark the transition region from the mildly non-linear cosmic web to the highly non-linear, virialized, cluster interior. It is in this transition region that the intracluster medium (ICM) begins to influence the properties of accreting galaxies and groups, as ram pressure impacts a galaxy’s cold gas content and subsequent star formation rate. Conversely, the thermodynamical properties of the ICM in this transition region should also feel the influence of accreting substructure (i.e. galaxies and groups), whose passage can drive shocks. | en_US |
| dc.language.iso | en | en_US |
| dc.publisher | Oxford University Press | en_US |
| dc.relation.ispartofseries | .; | |
| dc.subject | Methods: numerical | en_US |
| dc.subject | Galaxies: clusters: general | en_US |
| dc.subject | Galaxies: evolution | en_US |
| dc.subject | Galaxies: formation | en_US |
| dc.subject | Cosmology: theory | en_US |
| dc.title | NIFTY galaxy cluster simulations – VI. The dynamical imprint of substructure on gaseous cluster outskirts | en_US |
| dc.type | Article | en_US |
