We study the Globular Cluster ( GC ) system of the nearby elliptical galaxy M87 using the newly available dataset with accurate kinematics provided by Strader et al .
( 2011 ) .
We find evidence for three distinct sub-populations of GCs in terms of colours , kinematics and radial profiles .
We show that a decomposition into three populations – blue , intermediate and red GCs – is statistically preferred to one with two or four populations .
The existence of three components has been suggested before , but here we are able to identify them robustly and relate them to the stellar profile .
We exploit the sub-populations to derive dynamical constraints on the mass and Dark Matter ( DM ) content of M87 out to \sim 100 kpc .
We deploy a class of global mass-estimators , developed in Paper I , obtaining mass measurements at different locations .
The DM fraction in M87 changes from \approx 0.2 at the effective radius of the stellar light ( 0.02 ^ { \circ } or 6 kpc ) to \approx 0.95 at the distance probed by the most extended , blue GCs ( 0.47 ^ { \circ } or 135 kpc ) .

We supplement this analysis with virial decompositions , which exploit the dynamical model to produce a separation into multiple components .
These yield the luminous mass as 5.5 ^ { +1.5 } _ { -2.0 } \times 10 ^ { 11 } M _ { \odot } and the dark matter within 135 kpc as 8.0 ^ { +1.0 } _ { -4.0 } \times 10 ^ { 12 } M _ { \odot } . The inner DM density behaves as \rho \sim r ^ { - \gamma } with \gamma \approx 1.6 .
This is steeper than the cosmologically preferred cusp of \rho \sim r ^ { -1 } ( Dubinski & Carlberg ; Navarro , Frenk & White ) , and may provide evidence of dark matter contraction .
Finally , we combine the GC separation into three sub-populations with the Jeans equations , obtaining information on the orbital structure of the GC system .
The centrally concentrated red GCs exhibit tangential anisotropy , consistent with the depletion of radial orbits by tidal shredding .
The most extended blue GCs have an isotropic velocity dispersion tensor in the central parts , which becomes more tangential moving outwards , consistent with adiabatic contraction of the DM halo .