Disk galaxies at z=2 in OWLS

Simple item page
dc.creatorNavarro, Julio F.
dc.creatorSales, Laura V.
dc.creatorSchaye, Joop
dc.creatorVecchia, Claudio Dalla
dc.creatorSpringel, Volker
dc.date2009-05-21
dc.date.accessioned2026-07-07T13:17:30Z
dc.date.available2026-07-07T13:17:30Z
dc.descriptionWe use the OWLS (OverWhelmingly Large Simulations) set of cosmological Nbody/gasdynamical simulations to study the properties of simulated galaxies at z=2. We focus on the effect of supernova feedback from evolving stars on the baryonic mass and angular momentum content of galaxies that assemble at the center of 1e11-3e12 h^{-1}M_\odot halos. Our main finding is that the mass and angular momentum of such galaxies are strongly coupled, in a way that is approximately independent of feedback: varying the feedback implementation leads, in a given halo, to large variations in galaxy mass but leaves the galaxy mass-angular momentum correlation largely unaltered. In particular, the ratio between the angular momentum of a galaxy and that of its surrounding halo (j_d=J_gal/J_vir) correlates closely with the galaxy mass (expressed in units of the virial mass of the halo; m_d=M_gal/M_vir). This correlation differs substantially from the m_d=j_d assumption commonly adopted in semianalytic models of galaxy formation. We use these results to infer the sizes of disk galaxies at z=2 expected in the LCDM scenario and to interpret recent observations of extended disks at z~2 by the SINS collaboration
dc.descriptionConference Proceeding: "Galaxy Evolution: Emerging Insights and Future Challenges", November 11-14, 2008. The University of Texas at Austin. 8 pages, 7 figures
dc.identifierhttps://arxiv.org/abs/0905.3555
dc.identifierhttp://arxiv.org/abs/0905.3555
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/231132
dc.subjectCosmology and Nongalactic Astrophysics
dc.titleDisk galaxies at z=2 in OWLS
dc.typetext

Files

Collections

arXiv