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We present the first Herschel PACS and SPIRE results of the Vela C molecularcomplex in the far-infrared and submillimetre regimes at 70, 160, 250, 350, and500 um, spanning the peak of emission of cold prestellar or protostellar cores.Column density and multi-resolution analysis (MRA) differentiates the Vela Ccomplex into five distinct sub-regions. Each sub-region displays differences intheir column density and temperature probability distribution functions (PDFs),in particular, the PDFs of the `Centre-Ridge' and `South-Nest' sub-regionsappear in stark contrast to each other. The Centre-Ridge displays a bimodaltemperature PDF representative of hot gas surrounding the HII region RCW 36 andthe cold neighbouring filaments, whilst the South-Nest is dominated by coldfilamentary structure. The column density PDF of the Centre-Ridge is flatterthan the South-Nest, with a high column density tail, consistent with formationthrough large-scale flows, and regulation by self-gravity. At small tointermediate scales MRA indicates the Centre-Ridge to be twice as concentratedas the South-Nest, whilst on larger scales, a greater portion of the gas in theSouth-Nest is dominated by turbulence than in the Centre-Ridge. In Vela C,high-mass stars appear to be preferentially forming in ridges, i.e., dominanthigh column density filaments.

Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites