Left: projected phase-space diagram V_LOS vs. major axis distance R from the centre of M 87 out to 200 kpc for all spectroscopically confirmed PNs from Longobardi et al. (2015a); their M 87 halo PNs (red asterisks) and ICPNs (blue asterisks) are shown separately; R >  0 and R <  0 represent the northern and southern halves with respect the galaxy centre. Red open circles show four newly identified kinematic outliers (see Sect. 2.2). Black dash-dotted and black continuous lines depict the running average and running velocity dispersion independently for the M 87 south-east and north-west, computed from the 253 halo PNs. Full red circles show the robust estimate of the halo velocity dispersion following Longobardi et al. (2015a), while full black circles show the velocity dispersion values after probability-weighted removal of the crown substructure from Longobardi et al. (2015b). Both velocity dispersion profiles (red and black circles) show strong radial variation, with a steep decline at major axis distances R > 100 kpc. Green dash-dotted and green continuous lines show the running average and velocity dispersion for the combined sample of 253 halo PNs and 45 ICPNs; the inclusion of ICPNs leads to a rapidly rising velocity dispersion profile. Cyan triangles show the velocity dispersion measurements from the IFU VIRUS-P data of Murphy et al. (2011, 2014) whose outer rise near R = 700^″ (∼40 kpc) is matched by the running joint halo and ICPN velocity dispersion (green line) indicative of the contribution from the ICL. Right: zoomed-in plot in the velocity range ±1000 km s⁻¹ centred on the systemic velocity of M 87.