SMA observations of Infrared Dark Clouds: A tale of two cores

TL;DR

This study uses high-resolution sub-millimeter observations to compare two cores within Infrared Dark Clouds, revealing different stages of high-mass star formation, from early to hot core phases.

Contribution

It provides detailed observational evidence of two distinct high-mass star-forming cores within IRDCs, highlighting their physical and chemical differences and evolutionary stages.

Findings

One core shows a hot molecular environment with complex molecules.

The other core appears in an early star-formation stage with no molecular lines.

Both cores have sufficient mass to form high-mass stars.

Abstract

We present high-angular resolution sub-millimeter continuum images and molecular line spectra obtained with the SMA toward two massive cores that lie within Infrared Dark Clouds; one actively star-forming (G034.43+00.24 MM1) and the other more quiescent (G028.53-00.25 MM1). The high-angular resolution sub-mm continuum image of G034.43+00.24 MM1 reveals a compact (~0.03 pc) and massive (~29 Msun) structure while the molecular line spectrum shows emission from numerous complex molecules. Such a rich molecular line spectrum from a compact region indicates that G034.43+00.24 MM1 contains a hot molecular core, an early stage in the formation of a high-mass protostar. Moreover, the velocity structure of its 13CO(3-2) emission indicates that this B0 protostar may be surrounded by a rotating circumstellar envelope. In contrast, the sub-mm continuum image of G028.53-00.25 MM1 reveals three compact (<0.06 pc), massive (9-21 Msun) condensations but with no lines detected in its spectrum. We suggest that the core G028.53-00.25 MM1 is in a very early stage in the high-mass star-formation process; its size and mass are sufficient to form at least one high-mass star, yet it shows no signs of localized heating. Because the combination of high velocity line wings with a large IR-mm bolometric luminosity (~100 Lsun) indicates that this core has already begun to form accreting protostars, we speculate that the condensations may be in the early phase of accretion and may eventually become high-mass protostars. We, therefore, have found the possible existence of two high-mass star-forming cores; one in a very early phase of star-formation and one in the later hot core phase. Together the properties of these two cores support the idea that the earliest stages of high-mass star-formation occur within IRDCs.