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Observations of molecular clouds reveal a complex structure, with gas anddust often arranged in filamentary rather than spherical geometries. Theassociations of pre- and proto- stellar cores with the filaments suggest adirect link with the process of star formation. Any study of the properties ofsuch filaments requires a representative samples from different enviroments andso an unbiased detection method. We developed such an approach using theHessian matrix of a surface-brightness distribution to identify filaments anddetermine their physical and morphological properties. After testing the methodon simulated, but realistic filaments, we apply the algorithms tocolumn-density maps computed from Herschel observations of the Galactic Planeobtained by the Hi-GAL project. We identified ~500 filaments, in the longituderange of l=216.5 to l=225.5, with lengths from ~1 pc up to ~30 pc and widthsbetween 0.1 pc and 2.5 pc. Average column densities are between 10^20 cm^-2 and10^22 cm^-2. Filaments include the majority of dense material with N_H_2 >6x10^21cm^-2. We find that the pre- and proto-stellar compact sources alreadyidentified in the same region are mostly associated with filaments. However,surface densities in excess of the expected critical values for high-mass starformation are only found on the filaments, indicating that these structures arenecessary to channel material into the clumps. Furthermore, we analyze thegravitational stability of filaments and discuss their relationship with starformation.

astrophysical journal/the astrophysical journal

The identification of filaments on far infrared and submillimiter  images. Morphology, physical conditions and relation with star formation of  filamentary structure