  We use CARMA 3mm continuum and molecular lines (NH2D, N2H+, HCO+, HCN and CS)
at ~1000 au resolution to characterize the structure and kinematics of the
envelope surrounding the deeply embedded first core candidate Per-Bolo 58. The
line profile of the observed species shows two distinct peaks separated by
0.4-0.6 km/s, most likely arising from two different optically thin velocity
components rather than the product of self-absorption in an optically thick
line. The two velocity components, each with a mass of ~0.5-0.6 Msun, overlap
spatially at the position of the continuum emission, and produce a general
gradient along the outflow direction. We investigate whether these observations
are consistent with infall in a turbulent and magnetized envelope. We compare
the morphology and spectra of the N2H+(1-0) with synthetic observations of an
MHD simulation that considers the collapse of an isolated core that is
initially perturbed with a turbulent field. The proposed model matches the data
in the production of two velocity components, traced by the isolated hyperfine
line of the N2H+(1-0) spectra and shows a general agreement in morphology and
velocity field. We also use large maps of the region to compare the kinematics
of the core with that of the surrounding large-scale filamentary structure and
find that accretion from the large-scale filament could also explain the
complex kinematics exhibited by this young dense core.
