We present radial velocity and metallicity measurements for the far-southern Galactic globular cluster IC 4499 .
We selected several hundred target red giant stars in and around the cluster from the 2MASS point source catalog , and obtained spectra at the near-infrared calcium triplet using the AAOmega spectrograph .
Observations of giants in globular clusters M4 , M22 , and M68 were taken to provide radial velocity and metallicity comparison objects .
Based on velocity data we conclude that 43 of our targets are cluster members , by far the largest sample of IC 4499 giants spectroscopically studied .
We determine the mean heliocentric radial velocity of the cluster to be 31.5 \pm 0.4 km/s , and find the most likely central velocity dispersion to be 2.5 \pm 0.5 km/s .
This leads to a dynamical mass estimate for the cluster of 93 \pm 37 \times 10 ^ { 3 } M _ { \odot } .
We are sensitive to cluster rotation down to an amplitude of \approx 1 km/s , but no evidence for cluster rotation is seen .
The cluster metallicity is found to be [ Fe/H ] = - 1.52 \pm 0.12 on the Carretta-Gratton scale ; this is in agreement with some earlier estimates but carries significantly higher precision .
The radial velocity of the cluster , previously highly uncertain , is consistent with membership in the Monoceros tidal stream as proposed by Peñarrubia and co-workers , but also with a halo origin .
The horizontal branch morphology of the cluster is slightly redder than average for its metallicity , but it is likely not unusually young compared to other clusters of the halo .
The new constraints on the cluster kinematics and metallicity may give insight into its extremely high specific frequency of RR Lyrae stars .