  Asteroids of size larger than 0.15 km generally do not have periods smaller
than 2.2 hours, a limit known as cohesionless spin barrier. This barrier can be
explained by the cohesionless rubble-pile structure model. There are few
exceptions to this <<rule>>, called LSFRs (Large Super-Fast Rotators), as
(455213) 2001 OE84, (335433) 2005 UW163 and 2011 XA3. The near-Earth asteroid
(436724) 2011 UW158 was followed by an international team of optical and radar
observers in 2015 during the flyby with Earth. It was discovered that this NEA
is a new candidate LSFR. With the collected lightcurves from optical
observations we are able to obtain the amplitude-phase relationship, sideral
rotation period ($PS = 0.610752 \pm 0.000001$ h), a unique spin axis solution
with ecliptic coordinates $ \lambda = 290^{\circ} \pm 3^{\circ}$, $\beta =
39^{\circ} \pm 2^{\circ}$ and the asteroid 3D model. This model is in
qualitative agreement with the results from radar observations.
