Chemical Abundance Gradients of Organic Molecules within a Protostellar Disk

Abstract

Observations of low-mass protostellar systems show evidence of rich, complex organic chemistry. Their low luminosity, however, makes determining abundance distributions of complex organic molecules within the water snowline challenging. However, the excitation conditions sampled by differing molecular distributions may produce substantive changes in the resulting emission. Thus, molecular excitation may recover spatial information from spatially unresolved data. By analyzing spatially unresolved NOrthern Extended Millimeter Array observations of CH _3 OH and CH _3 CN, we aim to determine if CH _3 OH and CH _3 CN are distributed differently in the protostellar disk around HOPS-370, a highly luminous intermediate-mass protostar. Rotational diagram analysis of CH _3 OH and CH _3 CN yields rotational temperatures of 198 ± 1.2 K and 448 ± 19 K, respectively, suggesting the two molecules have different spatial distributions. Source-specific 3D LTE radiative transfer models are used to constrain the spatial distribution of CH _3 OH and CH _3 CN within the disk. A uniform distribution with an abundance of 4 × 10 ^−8 reproduces the CH _3 OH observations. In contrast, the spatial distribution of CH _3 CN needs to be either more compact (within ∼120 au versus ∼240 au for CH _3 OH) or exhibit a factor of ≳15 increase in abundance in the inner ∼55 au. A possible explanation for the difference in spatial abundance distributions of CH _3 OH and CH _3 CN is carbon-grain sublimation.

Keywords

• Astrochemistry
• Protostars
• Circumstellar disks
• Radiative transfer simulations