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In order to characterise the cloud structures responsible for the formationof high-mass stars, we present Herschel observations of the DR21 environment.Maps of the column density and dust temperature unveil the structure of theDR21 ridge and several connected filaments. The ridge has column densitieslarger than 1e23/cm^2 over a region of 2.3 pc^2. It shows substructured columndensity profiles and branching into two major filaments in the north. Themasses in the studied filaments range between 130 and 1400 Msun whereas themass in the ridge is 15000 Msun. The accretion of these filaments onto the DR21ridge, suggested by a previous molecular line study, could provide a continuousmass inflow to the ridge. In contrast to the striations seen in e.g., theTaurus region, these filaments are gravitationally unstable and form cores andprotostars. These cores formed in the filaments potentially fall into theridge. Both inflow and collisions of cores could be important to drive theobserved high-mass star formation. The evolutionary gradient of star formationrunning from DR21 in the south to the northern branching is traced bydecreasing dust temperature. This evolution and the ridge structure can beexplained by two main filamentary components of the ridge that merged first inthe south.

The spine of the swan: A Herschel study of the DR21 ridge and filaments in Cygnus X