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Herschel surveys of Galactic clouds support a paradigm for low-mass starformation in which dense filaments play a crucial role. The detailedfragmentation properties of star-forming filaments remain poorly understood,however, and the validity of the filament paradigm in the high-mass regime isstill unclear. To investigate the density/velocity structure of the filament inthe high-mass star-forming region NGC6334, we conducted ALMA observations inthe 3mm continuum and the N2H+(1-0) line at ~3arcsec resolution. The filamentwas detected in both tracers. We identified 26 cores at 3mm and 5velocity-coherent fiber-like features in N2H+ within the filament. The typicallength of, and velocity difference between, the fiber-like features of theNGC6334 filament are reminiscent of the properties for the fibers of thelow-mass star-forming filament B211/B213. Only 2 or 3 of the 5velocity-coherent features are well aligned with the filament and may representgenuine, fiber sub-structures. The core mass distribution has a peak at~10Msun. They can be divided into 7 groups of cores, closely associated withArTeMiS clumps. The projected separation between cores and the projectedspacing between clumps are roughly consistent with the effective Jeans lengthin the filament and a physical scale of about 4 times the filament width,respectively, suggesting a bimodal filament fragmentation process. Despitebeing one order of magnitude denser and more massive than the B211/B213filament, the NGC6334 filament has a similar density/velocity structure. Thedifference is that the cores in NGC6334 appear to be an order of magnitudedenser and more massive than the cores in Taurus. This suggests that densefilaments may evolve and fragment in a similar manner in low- and high-massstar-forming regions, and that the filament paradigm may hold in theintermediate-mass (if not high-mass) star formation regime.

Probing fragmentation and velocity sub-structure in the massive NGC 6334 filament with ALMA