Abstract
The complex chemistry that occurs in star-forming regions can provide insight into the formation of prebiotic molecules at various evolutionary stages of star formation. To study this process, we present millimeter-wave interferometric observations of the neighboring hot cores W3(H2O) and W3(OH) carried out using the NOEMA interferometer. We have analyzed distributions of six molecules that account for most observed lines across both cores and have constructed physical parameter maps for rotational temperature, column density, and velocity field with corresponding uncertainties. We discuss the derived spatial distributions of these parameters in the context of the physical structure of the source. We propose the use of HCOOCH3 as a new temperature tracer in W3(H2O) and W3(OH) in addition to the more commonly used . By analyzing the physically derived parameters for each molecule across both W3(H2O) and W3(OH), the work presented herein further demonstrates the impact of physical environment on hot cores at different evolutionary stages.
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