  We discovered new high-velocity components of H$_2$O maser emission in one of
the "water fountain" sources, IRAS~18286$-$0959, which has been monitored using
the Nobeyama 45 m telescope in the new FLASHING (Finest Legacy Acquisitions of
SiO- and H$_2$O-maser Ignitions by Nobeyama Generation) project since 2018
December. The maser spectra show new, extremely high expansion velocities
($>$200~km~s$^{-1}$ projected in the line of sight) components, some of which
are located symmetrically in the spectrum with respect to the systemic
velocity. They were also mapped with KaVA (KVN and VERA Combined Array) in 2019
March. We located some of these maser components closer to the central stellar
system than other high velocity components (50--200~km~s$^{-1}$) that have been
confirmed to be associated with the known bipolar outflow. The new components
would flash in the fast collimated jet at a speed over 300~km~s$^{-1}$ (soon)
after 2011 when they had not been detected. The fastest of the new components
seem to indicate rapid deceleration in these spectra, however our present
monitoring is still too sparse to unambiguously confirm it (up to
50~km~s$^{-1}$yr$^{-1}$) and too short to reveal their terminal expansion
velocity, which will be equal to the expansion velocity that has been observed
($v_{\rm exp}\sim$120~km~s$^{-1}$). Future occurrences of such extreme velocity
components may provide a good opportunity to investigate possible recurrent
outflow ignitions. Thus sculpture of the parental envelope will be traced by
the dense gas that is entrained by the fast jet and exhibits spectacular
distributions of the relatively stable maser features.
