MASS ACCRETION FLOWS IN THE HIGH-MASS STAR FORMING COMPLEX NGC6334.

The formation of high-mass stars is one of the major topics of astrophysical research, in particular the process of accretion from largescale clouds down to small-scale cores. We have selected the nearby, filamentary, high-mass star forming complex NGC6334 to study the gas velocity at different scales and probe the infall rates onto the protostellar cores embedded in the NGC6334-I and I(N) clusters. This study makes use of single-dish and interferometric submillimeter observations, complemented with 3D numerical non-LTE radiative transfer modeling. We measure a mass accretion rate of 10-5Mʘ yr-1 throughout the filament increasing up to 10-3Mʘ yr-1 towards the densest regions where high-mass stars are forming. At smaller scales, our 3D model is consistent with accretion rates of 10-3Mʘ yr-1 towards the clusters, and 10-4Mʘ yr-1 onto the protostars. [ABSTRACT FROM AUTHOR]