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dc.contributor.authorRichardson, Mark L. A.
dc.contributor.authorScannapieco, E.
dc.contributor.authorDevriendt, J.
dc.contributor.authorSlyz, A.
dc.contributor.authorThacker, Robert J.
dc.contributor.authorDubois, Y.
dc.contributor.authorWurster, J.
dc.contributor.authorSilk, J.
dc.date.accessioned2019-10-22T10:30:05Z
dc.date.available2019-10-22T10:30:05Z
dc.date.issued2016-07-10
dc.identifier.citationRichardson , M L A , Scannapieco , E , Devriendt , J , Slyz , A , Thacker , R J , Dubois , Y , Wurster , J & Silk , J 2016 , ' Comparing simulations of AGN feedback ' , Astrophysical Journal , vol. 825 , no. 2 , 83 , pp. 1-26 . https://doi.org/10.3847/0004-637X/825/2/83en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 262149924
dc.identifier.otherPURE UUID: 85006aa4-e717-4d92-b89b-1eadb4106d6d
dc.identifier.otherBibtex: Richardson+2016
dc.identifier.otherScopus: 84978372397
dc.identifier.otherORCID: /0000-0003-0688-5332/work/63716925
dc.identifier.urihttp://hdl.handle.net/10023/18737
dc.description.abstractWe perform adaptive mesh refinement (AMR) and smoothed particle hydrodynamics (SPH) cosmological zoom simulations of a region around a forming galaxy cluster, comparing the ability of the methods to handle successively more complex baryonic physics. In the simplest, non-radiative case, the two methods are in good agreement with each other, but the SPH simulations generate central cores with slightly lower entropies and virial shocks at slightly larger radii, consistent with what has been seen in previous studies. The inclusion of radiative cooling, star formation, and stellar feedback leads to much larger differences between the two methods. Most dramatically, at z=5, rapid cooling in the AMR case moves the accretion shock to well within the virial radius, while this shock remains near the virial radius in the SPH case, due to excess heating, coupled with poorer capturing of the shock width. On the other hand, the addition of feedback from active galactic nuclei (AGNs) to the simulations results in much better agreement between the methods. For our AGN model, both simulations display halo gas entropies of 100 keV cm2, similar decrements in the star formation rate, and a drop in the halo baryon content of roughly 30%. This is consistent with the AGN growth being self-regulated, regardless of the numerical method. However, the simulations with AGN feedback continue to differ in aspects that are not self-regulated, such that in SPH a larger volume of gas is impacted by feedback, and the cluster still has a lower entropy central core.
dc.format.extent26
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rightsCopyright © 2016 American Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at http://dx.doi.org/10.3847/0004-637X/825/2/83en
dc.subjectGalaxies: activeen
dc.subjectGalaxies: clusters: generalen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: halosen
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleComparing simulations of AGN feedbacken
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/0004-637X/825/2/83
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1605.03589en


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