  Aims: Investigation of the dense gas, the outflows and the continuum emission
from the massive twin cores NGC6334I and I(N) at high spatial resolution.
Methods: We imaged the region with the Australia Telescope Compact Array (ATCA)
at 3.4mm wavelength in continuum as well as CH3CN(5_K-4_K) and HCN(1-0)
spectral line emission. Results: While the continuum emission in NGC6334I
mainly traces the UCHII region, toward NGC6334I(N) we detect line emission from
four of the previously identified dust continuum condensations that are of
protostellar or pre-stellar nature. The CH3CN(5_K-4_K) lines are detected in
all K-components up to energies of 128K above ground toward two protostellar
condensations in both regions. We find line-width increasing with increasing K
for all sources, which indicates a higher degree of internal motions closer to
the central protostars. Toward the main mm and CH3CN source in NGC6334I we
identify a velocity gradient approximately perpendicular to the large-scale
molecular outflow. This may be interpreted as a signature of an accretion disk,
although other scenarios, e.g., an unresolved double source, could produce a
similar signature as well. No comparable signature is found toward any of the
other sources. HCN does not trace the dense gas well but it is dominated by the
molecular outflows. While the outflow in NGC6334I exhibits a normal Hubble-law
like velocity structure, the data indicate a precessing outflow close to the
plane of the sky for NGC6334I(N). Furthermore, we observe a wide (~15.4km/s)
HCN absorption line, much broader than the previously observed CH3OH and NH3
absorption lines. Several explanations for the difference are discussed.
