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We present observations of the 1.3 mm continuum emission toward hub-N andhub-S of the infrared dark cloud G14.225-0.506 carried out with theSubmillimeter Array, together with observations of the dust emission at 870 and350 microns obtained with APEX and CSO telescopes. The large scale dustemission of both hubs consists of a single peaked clump elongated in thedirection of the associated filament. At small scales, the SMA images revealthat both hubs fragment into several dust condensations. The fragmentationlevel was assessed under the same conditions and we found that hub-N presents 4fragments while hub-S is more fragmented, with 13 fragments identified. Westudied the density structure by means of a simultaneous fit of the radialintensity profile at 870 and 350 microns and the spectral energy distributionadopting a Plummer-like function to describe the density structure. Theparameters inferred from the model are remarkably similar in both hubs,suggesting that density structure could not be responsible in determining thefragmentation level. We estimated several physical parameters such as the levelof turbulence and the magnetic field strength, and we found no significantdifferences between these hubs. The Jeans analysis indicates that the observedfragmentation is more consistent with thermal Jeans fragmentation compared witha scenario that turbulent support is included. The lower fragmentation levelobserved in hub-N could be explained in terms of stronger UV radiation effectsfrom a nearby HII region, evolutionary effects, and/or stronger magnetic fieldsat small scales, a scenario that should be further investigated.

What is controlling the fragmentation process in the Infrared Dark Cloud G14.225-0.506? Differet level of fragmentation in twin hubs