A near IR imaging survey of intermediate and high-mass young stellar outflow candidates

TL;DR

This near-infrared imaging survey of intermediate and high-mass young stellar outflow candidates reveals prevalent H_2 emission and collimated outflows, supporting disk accretion as a key star formation mechanism up to late O types.

Contribution

The study provides new detections of H_2 emission features and outflows, linking molecular outflows with jet-driven mechanisms and identifying young stellar objects responsible for these outflows.

Findings

76% of objects show H_2 emission

50% or more exhibit aligned H_2 features suggesting collimated outflows

Most outflows are jet-driven and associated with early evolutionary stages

Abstract

We have carried out a near-infrared imaging survey of luminous young stellar outflow candidates using the United Kingdom Infrared Telescope. Observations were obtained in the broad band K (2.2 mu) and through narrow band filters at the wavelengths of H_2 v=1--0 S(1) (2.1218 mu) and Br gamma (2.166 mu) lines. Fifty regions were imaged with a field of view of 2.2 X 2.2 arcmin^2. Several young embedded clusters are unveiled in our near-infrared images. 76% of the objects exhibit H_2 emission and 50% or more of the objects exhibit aligned H_2 emission features suggesting collimated outflows, many of which are new detections. These observations suggest that disk accretion is probably the leading mechanism in the formation of stars, at least up to late O spectral types. The young stellar objects responsible for many of these outflows are positively identified in our images based on their locations with respect to the outflow lobes, 2MASS colours and association with MSX, IRAS, millimetre and radio sources. The close association of molecular outflows detected in CO with the H_2 emission features produced by shock excitation by jets from the young stellar objects suggests that the outflows from these objects are jet-driven. Towards strong radio emitting sources, H_2 jets were either not detected or were weak when detected, implying that most of the accretion happens in the pre-UCHII phase; accretion and outflows are probably weak when the YSO has advanced to its UCHII stage.