  We investigate the nature of the recently catalogued star cluster candidate
FSR584, which is projected in the direction of the molecular cloud W3 and may
be the nearest globular cluster to the Sun. 2MASS CMDs, the stellar radial
density profile, and proper motions are employed to derive fundamental and
structural parameters. The CMD morphology and the radial density profile show
that FSR584 is an old star cluster. With proper motions, the properties of
FSR584 are consistent with a metal-poor globular cluster with a well-defined
turnoff and evidence of a blue horizontal-branch. FSR584 might be a
Palomar-like halo globular cluster that is moving towards the Galactic plane.
The distance from the Sun is approx 1.4kpc, and it is located at approx 1kpc
outside the Solar circle. The radial density profile is characterized by a core
radius of rc=0.3+/-0.1 pc. However, we cannot exclude the possibility of an old
open cluster. Near-infrared photometry coupled to proper motions support the
scenario where FSR584 is a new globular cluster in the Galaxy. The absorption
is A_V=9.2+/-0.6$, which makes it a limiting object in the optical and explains
why it has so far been overlooked
