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Angular momentum is one of the most important physical quantities that governstar formation. The initial angular momentum of a core may be responsible forits fragmentation and can have an influence on the size of the protoplanetarydisk. To understand how cores obtain their initial angular momentum, it isimportant to study the angular momentum of filaments where they form. Whiletheoretical studies on filament rotation have been explored, there exist veryfew observational measurements of the specific angular momentum in star-formingfilaments. We present high-resolution N2D+ ALMA observations of the LBS 23(HH24-HH26) region in Orion B, which provide one of the most reliablemeasurements of the specific angular momentum in a star-forming filament. Wefind the total specific angular momentum ($4 \times 10^{20} cm^2s^{-1}$), thedependence of the specific angular momentum with radius (j(r) $\proptor^{1.83}$), and the ratio of rotational energy to gravitational energy($\beta_{rot} \sim 0.04$) comparable to those observed in rotating cores withsizes similar to our filament width ($\sim$ 0.04 pc) in other star-formingregions. Our filament angular momentum profile is consistent with rotationacquired from ambient turbulence and with simulations that show cores and theirhost filaments develop simultaneously due to the multi-scale growth ofnonlinear perturbation generated by turbulence.

Rotating filament in Orion B: Do cores inherit their angular momentum from their parent filament?