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dc.contributor.authorZhao, Hongsheng
dc.contributor.authorFamaey, Benoit
dc.contributor.authorLüghausen, Fabian
dc.contributor.authorKroupa, Pavel
dc.date.accessioned2014-01-14T12:31:07Z
dc.date.available2014-01-14T12:31:07Z
dc.date.issued2013-09
dc.identifier.citationZhao , H , Famaey , B , Lüghausen , F & Kroupa , P 2013 , ' Local Group timing in Milgromian dynamics : A past Milky Way-Andromeda encounter at z >0.8 ' Astronomy & Astrophysics , vol. 557 , L3 . DOI: 10.1051/0004-6361/201321879en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 70763615
dc.identifier.otherPURE UUID: 78b500ea-6c4e-4793-9e05-163a247f68c8
dc.identifier.otherArXiv: http://arxiv.org/abs/1306.6628v2
dc.identifier.otherScopus: 2-s2.0-84882435158
dc.identifier.urihttp://hdl.handle.net/10023/4365
dc.description4 pages, 2 figures, published in Astronomy and Astrophysicsen
dc.description.abstractContext: Local Group (LG) timing is one of the first historical probes of the so-called missing mass problem. Whilst modern cosmological probes indicate that pure baryonic dynamics is not sufficient on the largest scales, nearby galaxies and small galaxy groups persistently obey Milgrom’s MOND law, which implies that dynamics at small scales is possibly entirely predicted by the baryons. Aims: Here, we investigate LG timing in this context of Milgromian dynamics. Methods: We used the latest measured proper motions and radial velocities for Andromeda and the Magellanic clouds, and we integrated their orbits backwards by making use of the Milgromian two-body equation of motion. Results: With the currently measured proper motions and radial velocity of M31, we find that MOND would imply that the Milky Way (MW) and M31 first moved apart via Hubble expansion after birth, but then necessarily were attracted again by the Milgromian gravitational attraction, and had a past fly-by encounter before coming to their present positions. This encounter would most probably have happened 7 to 11 Gyr ago (0.8 < z < 3). The absence of a dark matter halo and its associated dynamical friction is necessary for such a close encounter not to have triggered a merger. Observational arguments which could exclude or favour such a past encounter would thus be very important in order to falsify or vindicate Milgromian dynamics on the scale of the LG. Interestingly, the closest approach of the encounter is small enough (<55 kpc) to have had severe consequences on the disc dynamics, including perhaps thick disc formation, and on the satellite systems of both galaxies. The ages of the satellite galaxies and of the young halo globular clusters, all of which form the vast polar structure around the MW, are consistent with these objects having been born during this encounter.en
dc.format.extent4en
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2013, ESO. A&A 557, L3 (2013). Reproduced with permission from the publishers.en
dc.subjectGalaxiesen
dc.subjectLocal Group (LG)en
dc.subjectGalaxy evolutionen
dc.subjectGalaxy gravitationen
dc.titleLocal Group timing in Milgromian dynamics : A past Milky Way-Andromeda encounter at z>0.8en
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201321879
dc.description.statusPeer revieweden


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