X-ray Star Clusters in the Carina Complex

TL;DR

This study analyzes the clustering of young X-ray emitting stars in the Carina complex, revealing diverse structures and star formation patterns, and highlighting the complexity of stellar distributions in this region.

Contribution

It provides a detailed mapping and characterization of star clusters and groups in Carina using X-ray data, uncovering new smaller groups and complex structures not previously identified.

Findings

Rich clusters like Trumpler 14 and 15 are centrally concentrated and complex.

Smaller, sparse groups and dispersed populations are prevalent.

No large embedded clusters were detected in the survey.

Abstract

The distribution of young stars found in the Chandra Carina Complex Project (CCCP) is examined for clustering structure. X-ray surveys are advantageous for identifying young stellar populations compared to optical and infrared surveys in suffering less contamination from nebular emission and Galactic field stars. The analysis is based on smoothed maps of a spatially complete subsample of about 3000 brighter X-ray sources classified as Carina members, and about 10,000 stars from the full CCCP sample. The principal known clusters are recovered, and some additional smaller groups are identified. No rich embedded clusters are present, although a number of sparse groups are found. The CCCP reveals considerable complexity in clustering properties. The Trumpler 14 and 15 clusters have rich stellar populations in unimodal, centrally concentrated structures several parsecs across. Non-spherical internal structure is seen, and large-scale low surface density distributions surround these rich clusters. Trumpler 16, in contrast, is comprised of several smaller clusters within a circular boundary. Collinder 228 is a third type of cluster which extends over tens of parsecs with many sparse compact groups likely arising from triggered star formation processes. A widely dispersed, but highly populous, distribution of X-ray stars across the about 50 pc CCCP mosaic supports a model of past generations of star formation in the region. Collinder 234, a group of massive stars without an associated cluster of pre-main sequence stars, may be part of this dispersed population.