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We study the mass distribution and kinematics of the giant elliptical galaxyM87 (NGC 4486) using discrete chemo-dynamical, axisymmetric Jeans equationmodelling. Our catalogue comprises 894 globular clusters (GCs) extending to aprojected radius of $\sim 430$ kpc with line-of-sight velocities and colours,and Multi Unit Spectroscopic Explorer (MUSE) integral field unit data withinthe central $2.4$ kpc of the main galaxy. The gravitational potential for ourmodels is a combination of a luminous matter potential with a varyingmass-to-light ratio for the main galaxy, a supermassive black hole and a darkmatter (DM) potential with a cusped or cored DM halo. The best-fitting modelswith either a cusped or a cored DM halo show no significant differences andboth are acceptable. We obtain a total mass of $(2.16 \pm 0.38) \times 10^{13}M_{\odot}$ within $\sim$ 400 kpc. By including the stellar mass-to-light ratiogradient, the DM fraction increases from $\sim$ 26 percent (with no gradient)to $\sim$ 73 percent within $1\,R_e^{\rm maj}$ (major axis of half-lightisophote, 14.2 kpc), and from $\sim$ 84 percent to $\sim$ 94 percent within$5\,R_e^{\rm maj}$ (71.2 kpc). Red GCs have moderate rotation with $V_{\rmmax}/\sigma \sim$ 0.4, and blue GCs have weak rotation with $V_{\rm max}/\sigma\sim$ 0.1. Red GCs have tangential velocity dispersion anisotropy, while blueGCs are consistent with being nearly isotropic. Our results suggest that redGCs are more likely to be born in-situ, while blue GCs are more likely to beaccreted.

A discrete chemo-dynamical model of M87's globular clusters: Kinematics extending to ~ 400 kpc