  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(H$_2$O) 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 HCOOCH$_3$ as a new temperature
tracer in W3(H$_2$O) and W3(OH) in addition to the more commonly used CH$_3$CN.
By analyzing the physically-derived parameters for each molecule across both
W3(H$_2$O) and W3(OH), the work presented herein further demonstrates the
impact of physical environment on hot cores at different evolutionary stages.
