  Recently, Carraro (2005) drew attention to the remarkable star cluster
Whiting 1 by showing that it lies about 40 kpc from the Sun and is therefore
unquestionably a member of the Galactic halo (b=-60.6 deg.). Its CMD indicated
that Whiting 1 is very young (5 Gyrs) for a globular cluster. It is very likely
that Whiting 1 originated in a dwarf galaxy that has since been disrupted by
the Milky Way. Deep CCD photometry in the BVI pass-bands obtained with the VLT
is used to improve the quality of the CMD and to determine the cluster's
luminosity function and surface density profile. High-resolution spectrograms
obtained with Magellan are used to measure the cluster's radial velocity and to
place limits on its possible metallicity. The measurements of distance and
radial velocity are used to test the cluster's membership in the stellar
streams from the Sgr dSph. From our CMD of Whiting 1, we derive new estimates
for the cluster's age (6.5 Gyrs), metallicity ([Fe/H]=-0.65), and distance
(29.4 kpc). From echelle spectrograms of three stars, we obtain -130.6 km/s for
the cluster's radial velocity and show from measurements of two infra-red CaII
lines that the [Fe/H] of the cluster probably lies in the range -1.1 to -0.4.
We demonstrate that the position of Whiting 1 on the sky, its distance from the
Sun, and its radial velocity are identical to within the errors of both the
theoretical predictions of the trailing stream of stars from the Sgr dSph
galaxy and the previous observations of the M giant stars that delineate the
streams. With the addition of Whiting 1, there is now strong evidence that 6
globular clusters formed within the Sgr dSph.
