Star clusters in the Sh2-132 complex: clues about the connection between embedded and open clusters

TL;DR

This study investigates the evolutionary connection between embedded and open star clusters in the Sh2-132 complex, revealing new clusters and evidence of dynamical transition from embedded to open clusters using infrared data.

Contribution

It provides new insights into the embedded-open cluster evolution, discovering four clusters and evidence of early dynamical evolution in the Sh2-132 region.

Findings

Discovery of four new clusters, including one deeply embedded.

Evidence of dynamical transition from embedded to open clusters.

Identification of a cluster related to a Wolf-Rayet star.

Abstract

Embedded clusters are formed in molecular clouds where massive stars can produce HII regions. The detailed embedded-open cluster evolutionary connection as well as the origin of associations are yet to be unveiled. There appears to be a high infant mortality rate among embedded clusters and the few survivors evolve to open clusters. We study the colour-magnitude diagrams and structure of the star clusters related to the Sh2-132 HII region using the 2MASS database. Cluster fundamental and structural parameters are determined via MS and PMS isochrones and stellar radial density profiles. We report the discovery of four clusters. One of them is projected a few diameters away from the optical cluster Teutsch\,127 and appears to be deeply embedded, seen only in the infrared. Evidence is found that we are witnessing the dynamical transition from an embedded to an open cluster. An additional cluster is also close to Teutsch\,127 and might be associated with a bow-shock. We also study the CMD and structure of the open cluster Berkeley\,94 in Sh2-132 and a new cluster which is projected in the outskirts of the complex. Finally, we searched for star clusters around the two known Wolf-Rayet stars in the complex. One of them appears to be related to a compact cluster. Finally, the present analyses suggest early dynamical evolution for young star clusters.