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tokens: (UCD-C group; see Section 3.1.2 ) include two groups with v r > 400 km s −1 and v r 400 km s −1 . The mean radial velocity of the other UCDs with v r > 400 km s −1 ( = 977 km s −1 ) is lower than those of the dwarfs with v r > 400 km s −1 and the M87 UCDs. The mean radial velocity of the other UCDs with v r 400 km s −1 is −117 km s −1 . Figure 13. (a) Radial velocities of GCs and dwarfs as a function of galactocentric distance from M87. The filled circles, open circles, and crosses represent the IGCs, M87 GCs, and dwarfs in the survey region (Kim et al. 2014 ), respectively. The small and large open circles represent the M87 GCs in Strader et al. ( 2011 ) and in this study, respectively. The dashed horizontal line indicates v r = 400 km s −1 , where a dip in the radial velocity distribution can be seen (see Figure 12 ). (b) Mean radial velocity of GCs and dwarfs in each radial bin as a function of galactocentric distance from M87. The symbols are the same as in (a). We divided the IGCs and dwarfs into two groups according to their radial velocities: v r > 400 km s −1 and v r 400 km s −1 . The vertical error bars indicate the root mean square velocities of the objects in each bin. Figure 14. (a) Radial velocities of UCDs and dwarf galaxies as a function of galactocentric distance from M87. The open squares, filled squares, and crosses represent the UCDs in the M87 region, the UCDs not in the M87 region, and the dwarfs in the survey region, respectively. The small and large open squares represent the UCDs in Zhang et al. ( 2015 ) and in this study, respectively. (b) Mean radial velocity of UCDs and dwarfs in each radial bin as a function of galactocentric distance from M87. The symbols are the same as in (a). We divided the dwarfs into two groups according to their radial velocities: v r > 400 km s −1 and v r 400 km s −1 . The vertical error bars indicate the root mean square velocities of the objects in each bin. Figure 15 shows the radial velocity dispersion profiles of the GCs and UCDs. The radial velocity dispersion of the GCs, UCDs, and dwarfs in each radial bin as well as its error is calculated following the formula in Pryor Meylan ( 1993 ). We use the IGCs, UCDs, and dwarfs with v r > 400 km s −1 that are not probably affected by infalling populations to derive the velocity dispersion for each tracer. The radial velocity dispersion of the combined M87 GCs is almost constant at 333 km s −1 . The radial velocity dispersion of the IGCs is similar to that of the GCs in M87 ( σ = 314 km s −1 ). Both are much lower than the radial velocity dispersion of dwarfs in the same survey region ( σ = 608 km s −1 ) and that of ICPNe superposed on the M87 region ( σ = 881 km s −1 ; Longobardi et al. 2015 ). Strader et al. ( 2011 ) suggested that the stellar halo of M87 is not truncated at R GC ∼ 30′, which is different from the result from the planetary nebulae (PNe) of M87 (Doherty et al. 2009 ). Our results are consistent with Strader et al. ( 2011 );