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A growing body of evidence indicates that the formation of filaments ininterstellar clouds is a key component of the star formation process. In thispaper, we present new Herschel PACS and SPIRE observations of the B59 and Stemregions in the Pipe Nebula complex, revealing a rich, organized network offilaments. The asymmetric column density profiles observed for severalfilaments, along with the bow-like edge of B59, indicates that the Pipe Nebulais being compressed from its western side, most likely by the winds from thenearby Sco OB2 association. We suggest that this compressive flow hascontributed to the formation of some of the observed filamentary structures. InB59, the only region of the entire Pipe complex showing star formationactivity, the same compressive flow has likely enhanced the initial columndensity of the clump, allowing it to become globally gravitationally unstable.Although more speculative, we propose that gravity has also been responsiblefor shaping the converging filamentary pattern observed in B59. While thequestion of the relative impact of large-scale compression and gravity remainsopen in B59, large-scale compression appears to be a plausible mechanism forthe initial formation of filamentary structures in the rest of the complex

The Pipe Nebula as seen with Herschel: Formation of filamentary structures by large-scale compression ?