The APOSTLE simulations: solutions to the Local Group's cosmic puzzles
Till Sawala (1, 2), Carlos S. Frenk (1), Azadeh Fattahi (3), Julio, F. Navarro (3, 4), Richard G. Bower (1), Robert A. Crain (5), Claudio, Dalla Vecchia (6, 7), Michelle Furlong (1), John. C. Helly (1), Adrian, Jenkins (1), Kyle A. Oman (2) Matthieu Schaller (1), Joop Schaye (8)

TL;DR
The APOSTLE simulations successfully replicate key observed properties of the Local Group, addressing longstanding cosmic structure formation puzzles within the b1bcCDM framework through detailed hydrodynamic modeling.
Contribution
This work introduces the APOSTLE suite of hydrodynamic simulations that match Local Group observations and resolve issues like the missing satellites and planes of satellites problems.
Findings
Simulations match observed satellite galaxy abundance.
Reproduce the stellar mass-velocity dispersion relation.
Provide new estimates for MW dwarf spheroidals' halo velocities.
Abstract
The Local Group of 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" ({\Lambda}CDM) model: there are far fewer satellite galaxies than substructures in cold dark matter halos (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 twelve volumes selected to match the kinematics of the Local Group (LG) members. Applying the Eagle code to the LG…
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