Orientation Of Late-type Galaxies Within Their Dark Matter Halos

Astronomy and Astrophysics – Astronomy

Scientific paper

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Scientific paper

We investigate relatively isolated late-type host galaxies and their satellites using the Sloan Digital Sky Survey (SDSS) and the LCDM Millennium Run Simulation (MRS). Late-type galaxies are believed to be embedded within dark matter halos that extend far beyond their optical radius, but the orientation of the luminous galaxy within the halo is poorly constrained. Pure dark matter simulations (e.g., the MRS) do not contain any information about the orientation of the galaxies, so it is necessary to make assumptions about how the galaxies could be oriented. The structure and dynamics of late-type galaxies are dominated by their angular momentum, and their most pronounced feature is the rotationally supported disk. By creating a disk within a simulated dark matter halo it is possible to create an artificial image of a luminous galaxy. The question becomes how to orient the disk relative to the dark matter halo so that it matches observed data. Here we investigate how the locations of the satellites around isolated late-type hosts in the MRS compare to similar data from the SDSS. To do this we create artificial luminous disks within the dark matter halos of the MRS hosts. The disks are oriented perpendicular to the angular momentum vectors of the halos, computed at different stages of the merging history of the host galaxies. We find that the locations of the satellites around blue SDSS hosts and blue MRS hosts are scale dependent, being found preferentially close to the major axes of their hosts when they are nearby to the hosts. At large radii the satellites of MRS hosts are isotropically distributed, while in the SDSS the satellites show a weak preference for being found close to the minor axes of their hosts.

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