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A massive envelope and a strong bipolar outflow are the two main structurescharacterizing the youngest protostellar systems. In order to understand thephysical properties of a bipolar outflow and the relationship with those of theenvelope, we obtained a mosaic map covering the whole bipolar outflow of theyoungest protostellar system L1157 with about $5"$ angular resolution in COJ=2-1 using the Combined Array for Research in Millimeter-wave Astronomy. Byutilizing these observations of the whole bipolar outflow, we estimate itsphysical properties and show that they are consistent with multiple jets. Wealso constrain a preferred precession direction. In addition, we observed thecentral envelope structure with $2"$ resolution in the $\lambda=1.3$ and 3 mmcontinua and various molecular lines: C$^{17}$O, C$^{18}$O, $^{13}$CO, CS, CN,N$_2$H$^+$, CH$_3$OH, H$_2$O, SO, and SO$_2$. All the CO isotopes and CS, CN,and N$_2$H$^+$ have been detected and imaged. We marginally detected thefeatures that can be interpreted as a rotating inner envelope in C$^{17}$O andC$^{18}$O and as an infalling outer envelope in N$_2$H$^+$. We also estimatedthe envelope and central protostellar masses and found that the dust opacityspectral index changes with radius.

Kinematics of the Envelope and Two Bipolar Jets in the Class 0 Protostellar System L1157