Characterization of molecular outflows at core-scale in the massive clump AGAL G345.0029-0.224

TL;DR

This study uses high-resolution ALMA data to analyze molecular outflows at the core scale in a high-mass star-forming region, revealing multiple hot cores with outflow activity and clarifying their role in massive star formation.

Contribution

It provides a detailed characterization of molecular outflows at the core scale in a high-mass clump, addressing discrepancies between clump-scale and core-scale outflow observations.

Findings

Multiple hot cores with outflows identified

Outflow activity linked to individual cores

Clarification of outflow contributions at core scale

Abstract

High-mass stars, with their powerful winds and intense radiation fields, are fundamental in regulating galactic dynamics and evolution; however, despite their great relevance, the mechanisms involved in their formation are still not fully understood. In this context, molecular outflows, which are essential for removing angular momentum and allowing accretion onto the central object, are a crucial phenomenon for characterizing their formation. Previous studies reveal a discrepancy in the masses of outflows associated with high-mass clumps between works conducted at the clump scale ($\sim$ pc) and those at the core scale ($\sim$ subpc). This suggests that the high-mass outflow activity observed at the clump scale might be the result of the contribution from several lower-mass outflows linked to individual molecular cores. This work presents a study of the molecular gas toward a high-mass clump associated with an Extended Green Object (EGO). EGOs are indicators of jets associated with high-mass protostars. Employing high angular resolution data from the Atacama Large Millimeter/submillimeter Array (ALMA), the presence of several hot cores with outflow activity was observed in the source. A characterization of the outflows at the core scale is presented within the context of the physical parameters of the molecular clumps.