Received YYY; in original form ZZZ'
title: 'Dynamical modelling of dwarf-spheroidal galaxies using Gaussian-process emulation'
---

\[firstpage\]

galaxies: dwarf – galaxies: kinematics and dynamics – methods: statistical

INTRODUCTION
============

In the $\Lambda$CDM model of cosmology, galaxies form by *hierachical growth*, with large galaxies being formed by the agglomeration of smaller ones. Of particular interest are the dwarf-spheroidal (dSph) galaxies that orbit the Milky Way, the dark-matter haloes of which are the smallest dark matter-dominated structures observed, and which are likely to be relics of the earliest stages of galaxy formation. These galaxies are still not fully understood. Although dark matter-only $N$-body simulations of halo-formation using $\Lambda$CDM cosmology predict cusps in the dark-matter density profile of the dSphs (i.e. they predict that density is inversely proportional to radius for small radii), the literature on the modelling of observed dSphs contains claims of both cusps and cores (i.e. it contains claims that density may be constant for small radii) ([@battaglia_kinematic_2008], [@strigari_kinematics_2010], [@breddels_model_2013], and [@read_case_2018]). Either the $\Lambda$CDM model fails at small scales and requires modification ([@ludlow_2016; @lovell_2014]), or dSphs evolve over their lifetimes, under the influence of baryonic feedback. For example, it has been shown that supernova-driven flattening may turn dark-matter cusps 