  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 NGC7492. 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 $\langle{v_{\rm r}}\rangle \sim 125$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 $\langle{v_{\rm r}}\rangle \sim
-110$km s$^{-1}$ that might be identified as members of the trailing wrap of
the same stream. The systemic velocity of NGC7492 set at $v_{\rm r} \sim
-177$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 $<v_{\rm r}> \sim -180$km
s$^{-1}$ might be comprised of cluster members along one of the tidal tails of
NGC7492.
