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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 720268.0, MPI für Astronomie / Publikationen_mpia
The stellar spheroid, the disk, and the dynamics of the cosmic web
Authors:Domínguez-Tenreiro, R.; Obreja, A.; Brook, C. B.; Martínez-Serrano, F. J.; Stinson, G.; Serna, A.
Date of Publication (YYYY-MM-DD):2015
Title of Journal:The Astrophysical Journal Letters
Volume:800
Start Page:id. L30 (5 pp)
Audience:Not Specified
Abstract / Description:Models of the advanced stages of gravitational instability predict that baryons that form the stellar populations of current galaxies at z = 0 displayed a web-like structure at high z, as part of the cosmic web (CW). We explore details of these predictions using cosmological hydrodynamical simulations. When the stellar populations of the spheroid and disk components of simulated late-type galaxies are traced back separately to high zs we found CW-like structures where spheroid progenitors are more evolved than disk progenitors. The distinction between the corresponding stellar populations, as driven by their specific angular momentum content j, can be explained in terms of the CW evolution, extended to two processes occurring at lower z. First, the spheroid progenitors strongly lose j at collapse, which contrasts with the insignificant j loss of the disk progenitors. The second is related to the lack of alignment, at assembly, between the spheroid-to-be material and the already settled proto-disk, in contrast to the alignment of disk-to-be material, in some cases resulting from circumgalactic, disk-induced gravitational torques. The different final outcomes of these low-z processes have their origins in the different initial conditions driven by the CW dynamics.
Free Keywords:cosmology: theory; galaxies: formation; methods: numerical
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X
URL:http://cdsads.u-strasbg.fr/abs/2015ApJ...800L..30D
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