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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 theenvelope surrounding the deeply embedded first core candidate Per-Bolo 58. Theline profile of the observed species shows two distinct peaks separated by0.4-0.6 km/s, most likely arising from two different optically thin velocitycomponents rather than the product of self-absorption in an optically thickline. The two velocity components, each with a mass of ~0.5-0.6 Msun, overlapspatially at the position of the continuum emission, and produce a generalgradient along the outflow direction. We investigate whether these observationsare consistent with infall in a turbulent and magnetized envelope. We comparethe morphology and spectra of the N2H+(1-0) with synthetic observations of anMHD simulation that considers the collapse of an isolated core that isinitially perturbed with a turbulent field. The proposed model matches the datain the production of two velocity components, traced by the isolated hyperfineline of the N2H+(1-0) spectra and shows a general agreement in morphology andvelocity field. We also use large maps of the region to compare the kinematicsof the core with that of the surrounding large-scale filamentary structure andfind that accretion from the large-scale filament could also explain thecomplex kinematics exhibited by this young dense core.

A turbulent origin for the complex envelope kinematics in the young low-mass core Per-Bolo 58