  Located at less than 2pc away, Luhman16AB (WISE.J104915.57-531906.1) is the
closest pair of brown dwarfs and third closest `stellar' system to Earth. An
exoplanet candidate in the Luhman16 binary system was reported in 2017 based on
a weak astrometric signature in the analysis of 12 HST epochs. An additional
epoch collected in 2018 and re-analysis of the data with more advanced methods
further increased the significance level of the candidate, consistent with a
Neptune-mass exoplanet orbiting one of the Luhman16 brown dwarf components. We
report the joint analysis of these previous data together with two new
astrometric HST epochs we obtained to confirm or disprove this astrometric
signature. Our new analysis rules out presence of a planet orbiting one
component of the Luhman16AB system for masses M > 1.5 M_Nep (Neptune masses)
and periods between 400 and 5000 days. However, the presence of third bodies
with masses M < 3 M_Nep and periods between 2 and 400 days (~1.1yrs) can not be
excluded. Our measurements make significant improvements to the
characterization of this sub-stellar binary, including its mass-ratio
0.8305+/-0.0006, individual component masses 35.4+/-0.2 M_Jup and 29.4+/-0.2
M_Jup (Jupiter masses), and parallax distance 1.9960pc +/- 50AU. Comparison of
the masses and luminosities of Luhman16AB to several evolutionary models shows
persistent discrepancies in the ages of the two components, but strengthens the
case that this system is a member of the 510+/-95 Myr Oceanus Moving Group.
