http://arxiv.org/abs/1711.00856
According to the hierarchical model of galaxy formation underlying our current understanding of cosmology, the Milky Way (MW) has continued to accrete smaller-sized dwarf galaxies since its formation. Remnants of this process surround the MW as debris streams and satellite galaxies, and provide information that is complementary to studies of the Galaxy itself. The satellite system thus has the potential to teach us about the formation and evolution of the MW. Can the existence of a narrow, co-rotating plane of satellite galaxies (the Vast Polar Structure, VPOS) put constraints on our Galaxy’s properties? Are such satellite galaxy planes more narrow around less massive hosts, more abundant around more concentrated hosts, more kinematically coherent around more early-forming halos? To address such questions, we have looked for correlations between properties of satellite galaxy planes fitted to cosmological simulations in the ELVIS suite and properties of their host dark matter halos, while accounting for realistic observational biases such as the obscuration by the disk of the MW. We find no evidence for strong correlations that would allow conclusions on the host halo properties from the mere existence of the VPOS around our Galaxy.
M. Pawlowski
Mon, 6 Nov 17
28/53
Comments: 4 pages, 4 figures, to appear in the proceedings of the SF2A meeting 2017
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