The spatial distribution of the Milky Way and Andromeda satellite galaxies

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dc.creatorMetz, M.
dc.creatorKroupa, P.
dc.creatorJerjen, H.
dc.date2006-10-31
dc.date.accessioned2026-07-07T11:00:04Z
dc.date.available2026-07-07T11:00:04Z
dc.descriptionThere are two fundamentally different physical origins of faint satellite galaxies: cosmological sub-structures that contain shining baryons and the fragmentation of gas-rich tidal arms thrown out from interacting galaxies during hierarchical structure formation. The latter tidal-dwarf galaxies (TDG) may form populations with correlated orbital angular momenta about their host galaxies. The existence of TDGs is a stringent necessity because they arise as a result of fundamental physical principals. We determine the significance of the apparent disc-like distribution of Milky Way (MW) satellite galaxies. The distribution of the MW satellites is found to be inconsistent with an isotropic or prolate DM sub-structure distribution at a 99.5 per cent level including the recently discovered UMa and CVn dwarf spheroidal galaxies. The distribution is extremely oblate and inclined by about $88\degr$ with respect to the the MW disc. We also apply the methods to Andromeda's (M31) satellite galaxies using two recently published data-sets. It can not be excluded that the whole population of M31 companions is drawn randomly from an isotropic parent distribution. However, two subsamples of Andromeda satellites are identified which have disc-like features. [abbreviated]
dc.description14 figures, 6 tables; acc. for pub. in MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0610933
dc.identifierhttp://arxiv.org/abs/astro-ph/0610933
dc.identifierMon.Not.Roy.Astron.Soc.374:1125-1145,2007
dc.identifierdoi:10.1111/j.1365-2966.2006.11228.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/187610
dc.subjectAstrophysics
dc.titleThe spatial distribution of the Milky Way and Andromeda satellite galaxies
dc.typetext

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