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We study the dynamics of the giant elliptical galaxy M87 from the central tothe outermost regions with the made-to-measure (M2M) method. We use a newcatalogue of 922 globular cluster line-of- sight velocities extending to aprojected radius of 180 kpc (equivalent to 25 M87 effective radii), and SAURONintegral field unit data within the central 2.4 kpc. 263 globular clusters,mainly located beyond 40 kpc, are newly observed by the Next Generation VirgoSurvey (NGVS). For the M2M modelling, the gravitational potential is taken as acombination of a luminous matter potential with a constant stellarmass-to-light ratio and a dark matter potential modelled as a logarithmicpotential. Our best dynamical model returns a stellar mass-to-light ratio inthe I band of M/LI = 6.0(+ -0.3) M_sun/L_sun with a dark matter potential scalevelocity of 591(+ -50) km/s and scale radius of 42(+ -10) kpc. We determine thetotal mass of M87 within 180 kpc to be (1.5 + - 0.2) 10^13 M_sun. The masswithin 40 kpc is smaller than previous estimates determined using globularcluster kinematics that did not extend beyond 45 kpc. With our new globularcluster velocities at much larger radii, we see that globular clusters around40 kpc show an anomalously large velocity dispersion which affected previousresults. The mass we derived is in good agreement with that inferred from ROSATX-ray observation out to 180 kpc. Within 30 kpc our mass is also consistentwith that inferred from Chandra and XMM-Newton X-ray observations, while within120 kpc it is about 20% smaller. The model velocity dispersion anisotropy betaparameter for the globular clusters in M87 is small, varying from -0.2 at thecentre to 0.2 at 40 kpc, and gradually decreasing to zero at 120 kpc.

The Next Generation Virgo cluster Survey. V. modelling the dynamics of M87 with the Made-to-Measure method