Structure and kinematics of the Taurus region

We apply a hierarchical clustering algorithm for partitioning the stars in our sample into groups (i.e., clusters) that are associated with the various molecular clouds of the complex, and derive the distance and spatial velocity of individual stars and their corresponding molecular clouds.

We show that the molecular clouds are located at different distances and confirm the existence of important depth effects in this region reported in previous studies. For example, we find that the L~1495 molecular cloud is located at d=129.9^+0.4^_-0.3_pc, while the filamentary structure connected to it (in the plane of the sky) is at d=160.0^+1.2^_-1.2_pc. We report B215 and L1558 as the closest (d=128.5^+1.6^_-1.6_pc) and most remote (d=198.1^+2.5^_-2.5_pc) substructures of the complex, respectively.