Comparing Complex Chemistry in Neighboring Hot Cores: NOEMA Studies of W3(H$_{2}$O) and W3(OH)

TL;DR

This study uses NOEMA observations to compare the chemistry and structure of neighboring hot cores W3(H₂O) and W3(OH), revealing new molecules, structural features, and the influence of physical environment on star formation chemistry.

Contribution

It provides the first detailed chemical and structural comparison of two neighboring hot cores at different evolutionary stages using high-resolution interferometry.

Findings

Detection of HDO and CH₃CH₂CN in W3(OH) for the first time

Identification of extended emission possibly indicating low-velocity shocks

Construction of temperature and column density maps for key molecules

Abstract

Presented here are NOEMA interferometric observations of the neighboring hot cores W3(H$_{2}$O) and W3(OH). The presence of two star-forming cores at different evolutionary stages within the same parent cloud presents a unique opportunity to study how the physics of the source and its evolutionary stage impact the chemistry. Through spectral analysis and imaging, we identify over twenty molecules in these cores. Most notably, we have detected HDO and CH$_{3}$CH$_{2}$CN in W3(OH), which were previously not detected in this core. We have imaged the molecular emission, revealing new structural features within these sources. W3(OH) shows absorption in a "dusty cocoon" surrounded by molecular emission. These observations also reveal extended emission that is potentially indicative of a low-velocity shock. From the information obtained herein, we have constructed column density and temperature maps for methanol and compared this information to the molecular images. By comparing the spatial distribution of molecules which may be destroyed at later stages of star formation, this work demonstrates the impact of physical environment on chemistry in star-forming regions at different evolutionary stages.