Sawala, Till and Frenk, Carlos S. and Fattahi, Azadeh and Navarro, Julio F. and Bower, Richard G. and Crain, Robert A. and Dalla Vecchia, Claudio and Furlong, Michelle and Helly, John. C. and Jenkins, Adrian and Oman, Kyle A. and Schaller, Matthieu and Schaye, Joop and Theuns, Tom and Trayford, James and White, Simon D. M. (2016) 'The APOSTLE simulations : solutions to the Local Group's cosmic puzzles.', Monthly notices of the Royal Astronomical Society., 457 (2). pp. 1931-1943.
The Local Group galaxies offer some of the most discriminating tests of models of cosmic structure formation. For example, observations of the Milky Way (MW) and Andromeda satellite populations appear to be in disagreement with N-body simulations of the ‘lambda cold dark matter’ (ΛCDM) model: there are far fewer satellite galaxies than substructures in CDM haloes (the ‘missing satellites’ problem); dwarf galaxies seem to avoid the most massive substructures (the ‘too-big-to-fail’ problem); and the brightest satellites appear to orbit their host galaxies on a thin plane (the ‘planes of satellites’ problem). Here we present results from APOSTLE (A Project Of Simulating The Local Environment), a suite of cosmological hydrodynamic simulations of 12 volumes selected to match the kinematics of the Local Group (LG) members. Applying the EAGLE code to the LG environment, we find that our simulations match the observed abundance of LG galaxies, including the satellite galaxies of the MW and Andromeda. Due to changes to the structure of haloes and the evolution in the LG environment, the simulations reproduce the observed relation between stellar mass and velocity dispersion of individual dwarf spheroidal galaxies without necessitating the formation of cores in their dark matter profiles. Satellite systems form with a range of spatial anisotropies, including one similar to the MWs, confirming that such a configuration is not unexpected in ΛCDM. Finally, based on the observed velocity dispersion, size, and stellar mass, we provide estimates of the maximum circular velocity for the haloes of nine MW dwarf spheroidals.
|Keywords:||Galaxies: evolution, Galaxies: formation, Cosmology: theory.|
|Full text:||(VoR) Version of Record|
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|Publisher Web site:||http://dx.doi.org/10.1093/mnras/stw145|
|Publisher statement:||This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||16 January 2016|
|Date deposited:||23 February 2016|
|Date of first online publication:||05 February 2016|
|Date first made open access:||23 February 2016|
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