Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-16553
Debattista, V P; Moore, B; Quinn, T; Kazantzidis, S; Maas, R; Mayer, L; Read , J; Stadel, J (2008). The causes of halo shape changes induced by cooling baryons: Disks versus substructures. Astrophysical Journal, 681(2):1076-1088.
PDF (Accepted manuscript, Version 2)
PDF (Accepted manuscript, Version 1)
Cold dark matter cosmogony predicts triaxial dark matter halos, whereas observations find quite round halos. This is most likely due to the condensation of baryons leading to rounder halos. We examine the halo phase space distribution basis for such shape changes. Triaxial halos are supported by box orbits, which pass arbitrarily close to the density center. The decrease in triaxiality caused by baryons is thought to be due to the scattering of these orbits. We test this hypothesis with simulations of disks grown inside triaxial halos. After the disks are grown we check whether the phase space structure has changed by evaporating the disks and comparing the initial and final states. While the halos are substantially rounder when the disk is at full mass, their final shape after the disk is evaporated is not much different from the initial. Likewise, the halo becomes (more) radially anisotropic when the disk is grown, but the final anisotropy is consistent with the initial. Only if the baryons are unreasonably compact or massive does the halo change irreversibly. We show that the character of individual orbits is not generally changed by the growing mass. Thus, the central condensation of baryons does not destroy enough box orbits to cause the shape change. Rather, box orbits merely become rounder along with the global potential. However, if angular momentum is transferred to the halo, either via satellites or via bars, a large irreversible change in the halo distribution occurs. The ability of satellites to alter the phase space distribution of the halo is of particular concern to galaxy formation simulations since halo triaxiality can profoundly influence the evolution of disks.
|Item Type:||Journal Article, refereed, original work|
|Communities & Collections:||07 Faculty of Science > Institute of Theoretical Physics|
|Deposited On:||10 Mar 2009 17:59|
|Last Modified:||28 Nov 2013 00:41|
|Publisher:||Institute of Physics Publishing|
|Citations:||Web of Science®. Times cited: 69|
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