The embedded clusters DBS 77, 78, 102, and 160-161 and their link with the interstellar medium

TL;DR

This study investigates the properties and interstellar medium interactions of embedded clusters DBS 77, 78, 102, 160, and 161 in the Milky Way's fourth quadrant using multi-wavelength data, revealing their physical parameters and link to surrounding HII regions and HI bubbles.

Contribution

It provides new detailed physical parameters of these clusters and demonstrates their connection with interstellar structures like HI bubbles and HII regions.

Findings

Estimated clusters' reddening, distance, age, and initial mass function.

Identified the HI bubble associated with DBS 160-161 clusters.

Demonstrated the energy from massive stars can create surrounding HI bubbles.

Abstract

Aims. We report a study of the global properties of some embedded clusters placed in the fourth quadrant of the Milky Way to clarify some issues related with their location into the Galaxy and their stellar formation processes. Methods. We performed BVI photometric observations in the region of DBS 77, 78, 102, 160, and 161 clusters and infrared spectroscopy in DBS 77 region. They were complemented with JHK data from VVV survey combined with 2MASS catalogue, and used mid-infrared information from GLIMPSE catalogue. We also searched for HI data from SGPS and PMN radio surveys, and previous spectroscopic stellar classification. The spectroscopic and photometric information allowed us to estimate the spectral classification of the brightest stars of each studied region. On the other hand, we used the radio data to investigate the interstellar material parameters and the continuum sources probably associated with the respective stellar components. Results. We estimated the basic physical parameters of the clusters (reddening, distance, age, and initial mass function). We searched for HII regions located near to the studied clusters and we analyzed the possible link between them. In the particular case of DBS 160-161 clusters, we identified the HI bubble B332.5-0.1-42 located around them. We found that the mechanical energy injected to the interstellar medium by the more massive stars of this couple of clusters was enough to generate the bubble.