We have resolved for the first time the radial and vertical structure of the almost edge-on envelope/disk system of the low-mass Class 0 protostar L1527 .
For that , we have used ALMA observations with a spatial resolution of 0.25 ^ { \prime \prime } \times 0.13 ^ { \prime \prime } and 0.37 ^ { \prime \prime } \times 0.23 ^ { \prime \prime } at 0.8 mm and 1.2 mm , respectively .
The L1527 dust continuum emission has a deconvolved size of 78 au \times 21 au , and shows a flared disk-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 toward 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 which 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 disk winds .