Complex organic molecules (COMs), the building blocks of life, have been extensively detected under various physical conditions, from quiescent clouds to star-forming regions. They therefore serve as excellent tracers of the local physical and chemical properties of these environments. Proper models that are capable of grasping the formation and destruction of COMs are crucial to understanding observations. However, given that distinct COMs can be detected from different locations and at varying times, we improved UCLCHEM -- a gas-grain chemical code -- to a 1D, time-dependent model tailored to protostars. In this update, we examine two stages of a protostar, the prestellar and heating stages, incorporating a simple radiative mechanism for both the internal and external radiation fields of the cloud. This approach relies on the key assumption that the dust and gas temperatures are completely coupled. Ultimately, we implemented an updated version of our model to interpret observations obtained through both single-dish and interferometry under varying conditions, including a SgrB2(N1) hot core, massive Galactic clumps, and a hot core in Orion. We show that our model can reproduce these observations well. We highlight that some COMs are positioned at a higher temperature in the envelope, and others at a lower temperature, which could potentially leading to misinterpretations when using a single-point model. In the case of SgrB2(N1), the best model indicates that the cosmic-ray ionisation rate significantly exceeds the value typically used for the standard interstellar medium. Our model is as an efficient computational tool that will be particularly useful for gaining better insights into COM observations.
Tram et al. (2026) studied this question.