Abstract
We use spectroscopic data for similar to 6000 red giant branch stars in the Small Magellanic Cloud (SMC), together with proper motion data from Gaia Early Data Release 3, to build a mass model of the SMC. We test our Jeans mass modelling method ( BINULATOR + GRAVSPHERE) on mock data for an SMC-like dwarf undergoing severe tidal disruption, showing that we are able to successfully remove tidally unbound interlopers, recovering the dark matter density and stellar velocity anisotropy profiles within our 95 percent confidence intervals. We then apply our method to real SMC data, finding that the stars of the cleaned sample are isotropic at all radii (at 95 per cent confidence) and that the inner dark matter density profile is dense, rho DM(150 pc ) = 1 . 58(-0.58)(+0.80) x 10(8) M-circle dot kpc(-3), consistent with a A cold dark matter cusp. Our model gives a new estimate of the SMC's total mass within 3 kpc (M-tot <= 3 kpc) of 2.29 +/- 0.46 x 10(9) M-circle dot. We also derive an astrophysical 'J-factor' of 18.99 +/- 0.16 GeV2 cm(-5) and a ' D-factor' of 18.73 +/- 0.04 GeV2 cm(-5), making the SMC a promising target for dark matter annihilation and decay searches. Finally, we combine our findings with literature measurements to test models in which dark matter is 'heated up' by baryonic effects. We find good qualitative agreement with the Di Cintio et al. model but we deviate from the Lazar et al. model at high M & lowast;/M-200 > 10(-2). We provide a new, analytical, density profile that reproduces dark matter heating behaviour over the range 10(-4) < M-& lowast;/M-200 < 10(-1).