Vertical structure of the transition zone from infalling rotating envelope to disc in the Class 0 protostar, IRAS 04368+2557

We have resolved for the first time the radial and vertical structures of the almost edge-on. envelope/disc system of the low-mass Class 0 protostar L1527. For that, we have usedAtacama Large Millimetre/submillimetre Array (ALMA) observations with a spatial resolution of 0.25 x 0.13 arcsec² and 0.37 x 0.23 arcsec² at 0.8 and 1.2 mm, respectively. The L1527 dust continuum emission has a deconvolved size of 78 x 21 au², and shows a flared disc-like structure. A thin infalling-rotating envelope is seen in the CCH emission outward of about 150 au, and its thickness is increased by a factor of 2 inward of it. This radius lies between the centrifugal radius (200 au) and the centrifugal barrier of the infalling-rotating envelope (100 au). The gas stagnates in front of the centrifugal barrier and moves towards vertical directions. SO emission is concentrated around and inside the centrifugal barrier. The rotation speed of the SO emitting gas is found to be decelerated around the centrifugal barrier. A part of the angular momentum could be extracted by the gas that moves away from the mid-plane around the centrifugal barrier. If this is the case, the centrifugal barrier would be related to the launching mechanism of low-velocity outflows, such as disc winds.