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Observations indicate that molecular clouds are strongly magnetized, and thatmagnetic fields influence the formation of stars. A key observation supportingthe conclusion that molecular clouds are significantly magnetized is that theorientation of their internal structure is closely related to that of themagnetic field. At low column densities the structure aligns parallel with thefield, whereas at higher column densities, the gas structure is typicallyoriented perpendicular to magnetic fields, with a transition at visualextinctions $A_V\gtrsim{}3~\rm{}mag$. Here we use far-infrared polarimetricobservations from the HAWC+ polarimeter on SOFIA to report the discovery of afurther transition in relative orientation, i.e., a return to parallelalignment at $A_V\gtrsim{}21~\rm{}mag$ in parts of the Serpens South cloud.This transition appears to be caused by gas flow and indicates that magneticsupercriticality sets in near $A_V\gtrsim{}21~\rm{}mag$, allowing gravitationalcollapse and star cluster formation to occur even in the presence of relativelystrong magnetic fields.

Magnetized filamentary gas flows feeding the young embedded cluster in Serpens South