  Submillimeter Array 1.3mm line and continuum observations toward the young
massive star-forming region IRAS18182-1433 are presented. The data are
complemented with short-spacing CO(2-1) observations and SiO(1-0) data from the
VLA. Multiple massive outflows emanate from the mm continuum peak. The CO(2-1)
data reveal a quadrupolar outflow system consisting of two outflows inclined by
\~90 degrees. One outflow exhibits a cone-like red-shifted morphology with a
jet-like blue-shifted counterpart where a blue counter-cone can only be
tentatively identified. The SiO(1-0) data suggest the presence of a third
outflow. Analyzing the 12CO/13CO line ratios indicates decreasing CO line
opacities with increasing velocities. The other seven detected molecular
species - also high-density tracers like CH3CN, CH3OH, HCOOCH3 - are all ~1-2''
offset from the mm continuum peak, but spatially associated with a strong
molecular outflow peak and a cm emission feature indicative of a thermal jet.
This spatial displacement between the molecular lines and the mm continuum
emission could be either due to an unresolved sub-source at the position of the
cm feature, or the outflow/jet itself alters the chemistry of the core
enhancing the molecular abundances toward that region. A temperature estimate
based on the CH3CN(12_k-11_k) lines suggests temperatures of the order 150K. A
velocity analysis of the high-density tracing molecules reveals that at the
given spatial resolution none of them shows any coherent velocity structure
which would be consistent with a rotating disk. We discuss this lack of
rotation signatures and attribute it to intrinsic difficulties to
observationally isolate massive accretion disks from the surrounding dense gas
envelopes and the molecular outflows.
