Stellar populations in the Carina region: The Galactic plane at l = 291

TL;DR

This study provides a detailed analysis of stellar populations, clusters, and the Galactic structure in the Carina region at l=291, revealing young stellar overdensities, a reddened massive star population, and insights into star formation and spiral arm placement.

Contribution

It offers the first homogeneous, multi-faceted analysis of stellar populations, clusters, and Galactic structure in the Carina region at l=291, with improved parameter estimates.

Findings

Identification of two young stellar overdensities.

Detection of a reddened massive OB star population.

Evidence of coeval star formation in key clusters.

Abstract

Previous studies of the Carina region have revealed its complexity and richness as well as a significant number of early-type stars. In many cases, these studies only concentrated on the central region or were not homogeneous. This latter aspect, in particular, is crucial because very different ages and distances for key clusters have been claimed in recent years. The aim of this work is to study in detail an area of the Galactic plane in Carina. We analyze the properties of different stellar populations and focus on a sample of open clusters and their population of YSOs and highly reddened early stars. We also studied the stellar mass distribution in these clusters and the possible scenario of their formation. Finally, we outline the Galactic spiral structure in this direction. We obtained photometric data for six young open clusters located in Carina at l = 291, and their adjacent stellar fields, which we complemented with spectroscopic observations of a few selected targets. We also culled additional information from the literature. Our results provide more reliable estimates of distances, color excesses, masses, and ages of the stellar populations in this direction. We estimate the basic parameters of the studied clusters and find that they identify two overdensities of young stellar populations. We find evidence of PMS populations inside them, with an apparent coeval stellar formation in the most conspicuous clusters. We also discuss apparent age and distance gradients in the direction NW-SE. We study the mass distributions of several clusters in the region. They consistently show a canonical IMF slope. We discover and characterise an abnormally reddened massive stellar population. Spectroscopic observations of ten stars of this latter population show that all selected targets were massive OB stars. Their location is consistent with the position of the Car-Sag spiral arm.