  We present the first spectroscopic observations of the very metal-poor Milky
Way globular cluster ESO280-SC06. Using spectra acquired with the 2dF/AAOmega
spectrograph on the Anglo-Australian Telescope, we have identified 13 members
of the cluster, and estimate from their infrared calcium triplet lines that the
cluster has a metallicity of $\mathrm{[Fe/H]}=-2.48\substack{+0.06 \\ -0.11}$.
This would make it the most metal-poor globular cluster known in the Milky Way.
This result was verified with comparisons to three other metal-poor globular
clusters that had been observed and analyzed in the same manner. We also
present new photometry of the cluster from EFOSC2 and SkyMapper and confirm
that the cluster is located $22.9\pm2.1$ kpc from the Sun and $15.2\pm2.1$ kpc
from the Galactic centre, and has a radial velocity of $92.5\substack{+2.4 \\
-1.6}$ km s$^{-1}$. These new data finds the cluster to have a radius about
half that previously estimated, and we find that the cluster has a dynamical
mass of the cluster of $(12\pm2)\times10^3$ solar masses. Unfortunately, we
lack reliable proper motions to fully characterize its orbit about the Galaxy.
Intriguingly, the photometry suggests that the cluster lacks a well-populated
horizontal branch, something that has not been observed in a cluster so ancient
or metal-poor.
