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Date and Time of the Query: 2019-05-26 T18:33:49 PDT
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For refcode 2013MNRAS.435.1928P:
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Copyright by Royal Astronomical Society. 2013MNRAS.435.1928P Dwarf galaxy planes: the discovery of symmetric structures in the Local Group Pawlowski, Marcel S.; Kroupa, Pavel; Jerjen, Helmut Abstract. Both major galaxies in the Local Group (LG) are surrounded by thin planes of mostly co-orbiting satellite galaxies, the vast polar structure (VPOS) around the Milky Way (MW) and the Great Plane of Andromeda (GPoA) around M31. We summarize the current knowledge concerning these structures and compare their relative orientations by re-determining their properties in a common coordinate system. The existence of similar, coherent structures around both major LG galaxies motivates an investigation of the distribution of the more distant non-satellite galaxies in the LG. This results in the discovery of two planes (diameters of 1-2 Mpc) which contain almost all nearby non-satellite galaxies. The two LG planes are surprisingly symmetric. They are inclined by only 20^degree^ relative to the galactic disc of M31, are similarly thin (heights of ~60 kpc) and have near-to-identical offsets from the MW and from M31. They are inclined relative to each other by 35^degree^. Comparing the plane orientations with each other and with additional features reveals indications for an intimate connection between the VPOS and the GPoA. They are both polar with respect to the MW, have similar orbital directions and are inclined by about 45^degree^+/-7^degree^ relative to each other. The Magellanic Stream approximately aligns with the VPOS and the GPoA, but also shares its projected position and line-of-sight velocity trend with a part of the dominating structure of non-satellite dwarf galaxies. In addition, the recent proper motion measurement of M31 indicates a prograde orbit of the MW-M31 system, the VPOS and the GPoA. The alignment with other features such as the Supergalactic Plane and the overdensity in hypervelocity stars are discussed as well. We end with a short summary of the currently proposed scenarios trying to explain the LG galaxy structures as either originating from cosmological structures or from tidal debris of a past galaxy encounter. We emphasize that there currently exists no full detailed model which satisfactorily explains the existence of the thin symmetric LG planes. Key words: Galaxy: halo, galaxies: dwarf, galaxies: individual: M31, galaxies: kinematics and dynamics, Local Group, Magellanic Clouds
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