The chemical structure of young high-mass star-forming clumps: (I) Deuteration

Abstract

The chemical structure of high-mass star nurseries is important for a general understanding of star formation. Deuteration is a key chemical process in the earliest stages of star formation because its efficiency is sensitive to the environment. Using the IRAM-30 m telescope at 1.3--4.3 mm wavelengths, we have imaged two parsec-scale high-mass protostellar clumps (P1 and S) that show different evolutionary stages but are located in the same giant filamentary {infrared dark cloud} G28.34+0.06. Deep spectral images at subparsec resolution reveal the dust and gas physical structures of both clumps. We find that (1) the low-$J$ lines of ${\mathrm{N}}_2{\mathrm{H}}^{+}$, HCN, HNC, and $\mathrm{HC}{\mathrm{O}}^{+}$ isotopologues are subthermally excited; and (2) the deuteration of ${\mathrm{N}}_2{\mathrm{H}}^{+}$ is more efficient than that of $\mathrm{HC}{\mathrm{O}}^{+}$, HCN, and HNC by an order of magnitude. The deuterations of these species are enriched toward the chemically younger clump S compared with P1, indicating that this process favors the colder and denser environment (${\mathrm{T}}_{\mathrm{kin}}\sim 14K$, $\mathrm{N}(\mathrm{N}{\mathrm{H}}_3)\sim 9\times 10^{15}\mathrm{c}{\mathrm{m}}^{-2}$). In contrast, single deuteration of $\mathrm{N}{\mathrm{H}}_3$ is insensitive to the environmental difference between P1 and S; and (3) single deuteration of $\mathrm{C}{\mathrm{H}}_3\mathrm{OH}$ ($>10\%$) is detected toward the location where CO shows a depletion of $\sim 10$. This comparative chemical study between P1 and S links the chemical variations to the environmental differences and shows chemical similarities between the early phases of high- and low-mass star-forming regions.

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