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Subarcsecond-resolution images of the rotational line emissions of CS andc-C$_3$H$_2$ obtained toward the low-mass protostar IRAS 04368$+$2557 in L1527with the Atacama Large Millimeter/submillimeter Array are investigated toconstrain the orientation of the outflow/envelope system. The distribution ofCS consists of an envelope component extending from north to south and a faintbutterfly-shaped outflow component. The kinematic structure of the envelope iswell reproduced by a simple ballistic model of an infalling rotating envelope.Although the envelope has a nearly edge-on configuration, the inclination angleof the rotation axis from the plane of the sky is found to be 5$^\circ$, wherewe find that the western side of the envelope faces the observer. Thisconfiguration is opposite to the direction of the large-scale ($\sim$ 10$^4$AU) outflow suggested previously from the $^{12}$CO ($J$=3$-$2) observation,and to the morphology of infrared reflection near the protostar ($\sim$ 200AU). The latter discrepancy could originate from high extinction by the outflowcavity of the western side, these discrepancies or may indicate that theoutflow axis is not parallel to the rotation axis of the envelope.Position-velocity diagrams show the accelerated outflow cavity wall, and itskinematic structure in the 2000 AU scale is explained by a standard parabolicmodel with the inclination angle derived from the analysis of the envelope. Thedifferent orientation of the outflow between the small and large scale impliesa possibility of precession of the outflow axis. The shape and the velocity ofthe outflow in the vicinity of the protostar are compared with those of otherprotostars.

Geometric and Kinematic Structure of the Outflow/Envelope System of L1527 Revealed by Subarcsecond-resolution Observation of CS