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Studying Class 0 objects is very important, as it allows to characterizedynamical processes at the onset of the star formation process, and todetermine the physical mechanisms responsible for the outcome of the collapse.Observations of dense gas tracers allow the characterization of key kinematicsof the gas directly involved in the star-formation process, such as infall,outflow or rotation. This work aims at investigating the molecular linevelocity profiles of the Class 0 protostellar object B335 and attempts to putconstraints on the infall motions happening in the circumstellar gas of theobject.} Observations of C$^{17}$O (1-0), C$^{18}$O (1-0) and $^{12}CO$ (2-1)transitions are presented and the spectral profiles are analyzed at enveloperadii between 100 and 860 au. C$^{17}$O emission presents a double peaked lineprofile distributed in a complex velocity field. Both peaks present an offsetof 0.2 to 1 km s$^{-1}$ from the systemic velocity of the source in the probedarea. The optical depth of the C$^{17}$O emission has been estimated and foundto be less than 1, suggesting that the two velocity peaks trace two distinctvelocity components of the gas in the inner envelope. After discarding possiblemotions that could produce the complex velocity pattern, such as rotation andoutflow, it is concluded that infall is producing the velocity field. Becauseinside-out symmetric collapse cannot explain those observed profiles, it issuggested that those are produced by non-isotropic accretion from the envelopeinto the central source along the outflow cavity walls.

Structured velocity field in the inner envelope of B335: ALMA observations of rare CO isotopologues