Details

Autor(en) / Beteiligte

• Sawala, Till
• Frenk, Carlos S
• Fattahi, Azadeh
• Navarro, Julio F
• Bower, Richard G
• Crain, Robert A
• Vecchia, Claudio Dalla
• Furlong, Michelle
• Helly, John. C
• Jenkins, Adrian
• Oman, Kyle A
• Schaller, Matthieu
• Schaye, Joop
• Theuns, Tom
• Trayford, James
• White, Simon D. M

Titel

The APOSTLE simulations: solutions to the Local Group's cosmic puzzles

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2016-04, Vol.457 (2), p.1931-1943

Ort / Verlag

London: Oxford University Press

Erscheinungsjahr

2016

Quelle

Alma/SFX Local Collection

Beschreibungen/Notizen

• 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.