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The star-forming region W5 is a major part of the Cassiopeia OB6 association.Its internal structure and kinematics may provide hints of the star formationprocess in this region. Here, we present a kinematic study of young stars in W5using the Gaia data and our radial velocity data. A total 490 out of 2,000young stars are confirmed as members. Their spatial distribution shows that W5is highly substructured. We identify a total of eight groups using the k-meansclustering algorithm. There are three dense groups in the cavities of H IIbubbles, and the other five sparse groups are distributed at the ridge of thebubbles. The three dense groups have almost the same ages (5 Myr) and show apattern of expansion. The scale of their expansion is not large enough toaccount for the overall structure of W5. The three northern groups are, infact, 3 Myr younger than the dense groups, which indicates the independent starformation events. Only one group of them shows the signature of feedback-drivenstar formation as its members move away from the eastern dense group. The othertwo groups might have formed in a spontaneous way. On the other hand, theproperties of two southern groups are not understood as those of a coevalpopulation. Their origins can be explained by dynamical ejection of stars andmultiple star formation. Our results suggest that the substructures in W5formed through multiple star-forming events in a giant molecular cloud.

the astronomical journal

The kinematics of young stellar population in the W5 region of the  Cassiopeia OB6 association: implication on the formation process of stellar  associations