Rotating Filament in Orion B: Do Cores Inherit Their Angular Momentum from Their Parent Filament?

Angular momentum is one of the most important physical quantities that governs star formation. The initial angular a core may be responsible for its fragmentation, and can have an influence on size protoplanetary disk. To understand how cores obtain their momentum, it to study filaments where they form. While theoretical studies filament rotation been explored, there exist very few observational measurements specific in star-forming filaments. We present high-resolution N2D+ ALMA observations LBS 23 (HH24-HH26) region Orion B, which provide reliable filament. find total (4 × 1020 cm2 s?1), dependence with radius (j(r) ? r1.83), ratio rotational energy gravitational (?rot ? 0.04) comparable those observed rotating sizes similar our width (?0.04 pc) other regions. Our profile consistent acquired from ambient turbulence simulations show host develop simultaneously due multi-scale growth nonlinear perturbation generated by turbulence.