  The internal velocity structure within dense gaseous cores plays a crucial
role in providing the initial conditions for star formation in molecular
clouds. However, the kinematic properties of dense gas at core scales (~0.01 -
0.1 pc) has not been extensively characterized because of instrument
limitations until the unique capabilities of GBT-Argus became available. The
ongoing GBT-Argus Large Program, Dynamics in Star-forming Cores (DiSCo) thus
aims to investigate the origin and distribution of angular momenta of
star-forming cores. DiSCo will survey all starless cores and Class 0
protostellar cores in the Perseus molecular complex down to ~0.01 pc scales
with < 0.05 km/s velocity resolution using the dense gas tracer N$_2$H$^+$.
Here, we present the first datasets from DiSCo toward the B1 and NGC 1333
regions in Perseus. Our results suggest that a dense core's internal velocity
structure has little correlation with other core-scale properties, indicating
these gas motions may be originated externally from cloud-scale turbulence.
These first datasets also reaffirm the ability of GBT-Argus for studying dense
core velocity structure and provided an empirical basis for future studies that
address the angular momentum problem with a statistically broad sample.
