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The Chamaeleon molecular cloud complex is one of the nearest star-formingsites encompassing three molecular clouds with a different star-formationhistory, from quiescent (Cha III) to actively forming stars (Cha II), andreaching the end of star-formation (Cha I). To charactize its large-scalestructure, we derived column density and temperature maps using PACS and SPIREobservations from the Herschel Gould Belt Survey, and applied several tools,such as filament tracing, power-spectra, \Delta-variance, and probabilitydistribution functions of column density (PDFs), to derive physical properties.The column density maps reveal a different morphological appearance for thethree clouds, with a ridge-like structure for Cha I, a clump-dominated regimefor Cha II, and an intricate filamentary network for Cha III. The filamentwidth is measured to be around 0.12\pm0.04 pc in the three clouds, and thefilaments found to be gravitationally unstable in Cha I and II, but mostlysubcritical in Cha III. Faint filaments (striations) are prominent in Cha Ishowing a preferred alignment with the large-scale magnetic field. The PDFs ofall regions show a lognormal distribution at low column densities. For higherdensities, the PDF of Cha I shows a turnover indicative of an extended higherdensity component, culminating with a power-law tail. Cha II shows a power-lawtail with a slope characteristic of gravity. The PDF of Cha III can be best fitby a single lognormal. The turbulence properties of the three regions are foundto be similar, pointing towards a scenario where the clouds are impacted bylarge-scale processes. The magnetic field could possibly play an important rolefor the star-formation efficiency in the Chamaeleon clouds if proven that itcan effectively channel material on Cha I, and possibly Cha II, but probablyless efficiently on the quiescent Cha III cloud.

Herschel's view of the large-scale structure in the Chamaeleon dark clouds