  We present 0.9 mm continuum and CO (3-2) line emission observations retrieved
from the Atacama Large Millimeter/submillimeter Array (ALMA) archive toward the
high-mass star formation region IRAS 16076-5134. We identify fourteen dense
cores with masses between 0.3 to 22 M$_{\odot}$. We find an ensemble of
filament-like CO (3-2) ejections from -62 to +83 km s$^{-1}$ that appear to
arise radially from a common central position, close to the dense core MM8. The
ensemble of filaments, has a quasi-isotropic distribution in the plane of the
sky. The radial velocity of several filaments follow a linear velocity
gradient, incresing from a common origin. Considering the whole ensemble of
filaments, we estimate its total mass to be 138 and 216 M$_{\odot}$ from its CO
emission, for 70 K and 140 K respectively. Also, assuming a constant velocity
expansion of the filaments (of 83 km s$^{-1}$) we estimate the dynamical age of
the outflowing material (3500 years), its momentum (~10$^{4}$ M$_{\odot}$ km
s$^{-1}$) and its kinetic energy (~10$^{48-49}$ erg). The morphology and
kinematics presented by the filaments suggest the presence of a dispersal
outflow with explosive characteristics in IRAS 16076-5134. In addition, we make
a raw estimate of the lower limit of the frequency rate of the explosive
dispersal outflows in the Galaxy (one every 110 years) considering constant
star formation rate and efficiency with respect to the galactocentric radius of
the Galaxy. This may imply a comparable rate of dispersal outflows and
supernovae (approximately one every 50 years), which may be important for the
energy budget of the Interstellar Medium and the link between dispersal
outflows and high-mass star formation.
