Millimetric and sub-millimetric observations of IRAS 05327+3404 "Holoea" in M36

TL;DR

This study uses millimeter and sub-millimeter observations to analyze the properties and outflows of the young stellar object IRAS 05327+3404 'Holoea', revealing its complex structure and evolutionary stages.

Contribution

It provides detailed molecular line observations of Holoea, identifying two main outflows and suggesting different evolutionary stages for the associated sources.

Findings

Detected two continuum emission peaks at 1.1-mm.

Identified two main molecular outflows with different orientations.

SMM 1 likely in an earlier evolutionary stage than SMM 2.

Abstract

The transition between the proto-star, Class I, and the pre-main sequence star, Class II, phases is still one of the most uncertain, and important, stages in the knowledge of the process of formation of an individual star, because it is the stage that determines the final mass of the star. We observed the YSO "Holoea", associated with IRAS 05327+3404, which was classified as an object in transition between the Class I and Class II phases with several unusual properties, and appears to be surrounded by large amounts of circumstellar material. We used the SMA and BIMA telescopes at millimeter and sub-millimeter wavelengths to observe the dust continuum emission and the CO (1-0) and (2-1), HCO+ (1-0) and (3-2), and HCN (1-0) transitions in the region around IRAS 05327+3404. We detected two continuum emission peaks at 1.1-mm: SMM 1, the sub-mm counterpart of IRAS 05327+3404, and SMM 2, ~6 arcsec to the West. The emissions of the three molecules show marked differences. The CO emission near the systemic velocity is filtered out by the telescopes, and CO mostly traces the high-velocity gas. The HCO+ and HCN emissions are more centrally concentrated around the central parts of the region, and show several intensity peaks coincident with the sub-mm continuum peaks. We identify two main molecular outflows: a bipolar outflow in an E-W direction that would be powered by SMM 1 and another one in a NE direction, which we associate with SMM 2. We propose that the SMM sources are probably Class I objects, with SMM 1 in an earlier evolutionary stage.