Molecular globules and pillars are spectacular features , found only in the interface region between a molecular cloud and an H II -region .
Impacting far-ultraviolet ( FUV ) radiation creates photon-dominated regions ( PDRs ) on their surfaces that can be traced by typical cooling lines .
With the GREAT receiver onboard SOFIA we mapped and spectrally resolved the [ C II ] 158 \mu m atomic fine-structure line and the highly excited ^ { 12 } CO J=11 \to 10 molecular line from three objects in Cygnus X ( a pillar , a globule , and a strong IRAS source ) .
We focus here on the globule and compare our data with existing Spitzer data and recent Herschel open-time PACS data .
Extended [ C II ] emission and more compact CO-emission was found in the globule .
We ascribe this emission mainly to an internal PDR , created by a possibly embedded star-cluster with at least one early B-star .
However , external PDR emission caused by the excitation by the Cyg OB2 association can not be fully excluded .
The velocity-resolved [ C II ] emission traces the emission of PDR surfaces , possible rotation of the globule , and high-velocity outflowing gas .
The globule shows a velocity shift of \sim 2 km s ^ { -1 } with respect to the expanding H II -region , which can be understood as the residual turbulence of the molecular cloud from which the globule arose .
This scenario is compatible with recent numerical simulations that emphazise the effect of turbulence .
It is remarkable that an isolated globule shows these strong dynamical features traced by the [ C II ] -line , but it demands more observational studies to verify if there is indeed an embedded cluster of B-stars .