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dc.contributor.authorBanik, Indranil
dc.contributor.authorZhao, Hongsheng
dc.date.accessioned2016-06-24T12:30:03Z
dc.date.available2016-06-24T12:30:03Z
dc.date.issued2016-06-21
dc.identifier.citationBanik , I & Zhao , H 2016 , ' Dynamical history of the Local Group in ΛCDM ' , Monthly Notices of the Royal Astronomical Society , vol. 459 , no. 2 , pp. 2237-2261 . https://doi.org/10.1093/mnras/stw787en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 243626072
dc.identifier.otherPURE UUID: 71475df8-43ed-4e59-9129-3b0da67c90ae
dc.identifier.otherScopus: 84974605008
dc.identifier.otherORCID: /0000-0002-4123-7325/work/29616903
dc.identifier.otherWOS: 000377471200081
dc.identifier.urihttp://hdl.handle.net/10023/9045
dc.descriptionIB is supported by a Science and Technology Facilities Council studentship.en
dc.description.abstractThe positions and velocities of galaxies in the Local Group (LG) measure the gravitational field within it. This is mostly due to the Milky Way (MW) and Andromeda (M31). We constrain their masses using distance and radial velocity (RV) measurements of 32 LG galaxies. To do this, we follow the trajectories of many simulated particles starting on a pure Hubble flow at redshift 9. For each observed galaxy, we obtain a trajectory which today is at the same position. Its final velocity is the model prediction for the velocity of that galaxy. Unlike previous simulations based on spherical symmetry, ours are axisymmetric and include gravity from Centaurus A. We find the total LG mass is 4.33+0.37 -0.32 × 1012M⊙, with 0.14 ± 0.07 of this being in the MW. We approximately account for IC 342, M81, the Great Attractor and the Large Magellanic Cloud. No plausible set of initial conditions yields a good match to the RVs of our sample of LG galaxies. Observed RVs systematically exceed those predicted by the best-fitting Lambda Cold Dark Matter (ΛCDM) model, with a typical disagreement of 45.1+7.0 -5.7 km s-1 and a maximum of 110 ± 13 km s-1 for DDO 99. Interactions between LG dwarf galaxies cannot easily explain this. One possibility is a past close flyby of the MW and M31. This arises in some modified gravity theories but not in ΛCDM. Gravitational slingshot encounters of material in the LG with either of these massive fast-moving galaxies could plausibly explain why some non-satellite LG galaxies are moving away from us even faster than a pure Hubble flow.
dc.format.extent25
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1093/mnras/stw787en
dc.subjectMethods: data analysisen
dc.subjectMethods: numericalen
dc.subjectGalaxy: kinematics and dynamicsen
dc.subjectGalaxies: groups: localen
dc.subjectLocal group: cosmological parametersen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectAstronomy and Astrophysicsen
dc.subjectNDASen
dc.subjectBDCen
dc.subjectR2Cen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleDynamical history of the Local Group in ΛCDMen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stw787
dc.description.statusPeer revieweden


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