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Paper: Disk Galaxies at z=2 in OWLS
Volume: 419, Galaxy Evolution: Emerging Insights and Future Challenges
Page: 10
Authors: Navarro, J. F.; Sales, L. V.; OWLS team
Abstract: We 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 feedback from evolving stars on the baryonic mass and angular momentum content of galaxies that assemble at the center of 1011–1012 h-1Msun 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 strength 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 (jd = Jgal / Jvir) correlates closely with the galaxy mass (expressed in units of the virial mass of the halo; md = Mgal / Mvir). This correlation differs substantially from the md = jd 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.
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