  We constructed for the first time a stellar density profile of 47 Tucanae (47
Tuc) out of $\sim$ 5.5 times its tidal radius ($r_t$) using high-quality deep
$BV$ photometry. After carefully considering the influence of photometric
errors, and Milky Way and Small Magellanic Cloud composite stellar population
contamination, we found that the cluster stellar density profile reaches a
nearly constant value from $\sim$ 1.7$r_t$ outwards, which does not depend on
the direction from the cluster's center considered. These results visibly
contrast with recent distinct theoretical predictions on the existence of tidal
tails or on a density profile that falls as $r^{-4}$ at large distances, and
with observational outcomes of a clumpy structure as well. Our results suggest
that the envelope of 47 Tuc is a halo- like nearly constant low density
structure.
