We have derived from VIMOS spectroscopy the radial velocities for a sample of 71 stars selected from CFHT/Megacam photometry around the Galactic globular cluster NGC 7492 .
In the resulting velocity distribution , it is possible to distinguish two relevant non-Galactic kinematic components along the same line of sight : a group of stars at \langle { v _ { r } } \rangle \sim 125 km s ^ { -1 } which is compatible with the velocity of the old leading arm of the Sagittarius tidal stream , and a larger number of objects at \langle { v _ { r } } \rangle \sim - 110 km s ^ { -1 } that might be identified as members of the trailing wrap of the same stream .
The systemic velocity of NGC 7492 set at v _ { r } \sim - 177 km s ^ { -1 } differs significantly from that of both components , thus our results confirm that this cluster is not one of the globular clusters deposited by the Sagittarius dwarf spheroidal in the Galactic halo , even if it is immersed in the stream .
A group of stars with < v _ { r } > \sim - 180 km s ^ { -1 } might be comprised of cluster members along one of the tidal tails of NGC 7492 .