Deuteration as an evolutionary tracer in massive-star formation

TL;DR

This study investigates whether deuteration ratios, used as evolutionary tracers in low-mass star formation, are applicable to high-mass star formation by analyzing N2D+ and N2H+ in massive star-forming regions.

Contribution

It demonstrates that the N2D+-to-N2H+ ratio can serve as an evolutionary indicator in high-mass star formation, similar to low-mass cases, based on observational evidence.

Findings

N2D+ abundance is highest in pre-stellar cores.

N2D+ abundance decreases during protostar formation.

N2D+ levels remain stable in ultra-compact HII regions.

Abstract

Theory predicts, and observations confirm, that the column density ratio of a molecule containing D to its counterpart containing H can be used as an evolutionary tracer in the low-mass star formation process. Since it remains unclear if the high-mass star formation process is a scaled-up version of the low-mass one, we investigated whether the relation between deuteration and evolution can be applied to the high-mass regime. With the IRAM-30m telescope, we observed rotational transitions of N2D+ and N2H+ and derived the deuterated fraction in 27 cores within massive star-forming regions understood to represent different evolutionary stages of the massive-star formation process. Results. Our results clearly indicate that the abundance of N2D+ is higher at the pre-stellar/cluster stage, then drops during the formation of the protostellar object(s) as in the low-mass regime, remaining relatively constant during the ultra-compact HII region phase. The objects with the highest fractional abundance of N2D+ are starless cores with properties very similar to typical pre-stellar cores of lower mass. The abundance of N2D+ is lower in objects with higher gas temperatures as in the low-mass case but does not seem to depend on gas turbulence. Our results indicate that the N2D+-to-N2H+ column density ratio can be used as an evolutionary indicator in both low- and high-mass star formation, and that the physical conditions influencing the abundance of deuterated species likely evolve similarly during the processes that lead to the formation of both low- and high-mass stars.