The first interferometric measurements of NH$_2$D/NH$_3$ ratio in hot corinos

TL;DR

This study presents the first interferometric measurements of NH$_2$D/NH$_3$ ratios in hot corinos, revealing high deuterium fractionation and insights into nitrogen chemistry during star formation.

Contribution

It provides high-resolution observations of NH$_3$ and NH$_2$D in a protobinary system, offering new constraints on nitrogen chemistry and ice formation in star-forming regions.

Findings

NH$_3$ is sublimated in hot inner regions near protostars.

NH$_2$D/NH$_3$ ratios are as high as 0.3-1 in the observed cores.

Results suggest ammonia ice formation began in the prestellar phase.

Abstract

The nitrogen chemical evolution during star and planet formation is still not fully understood. Ammonia (NH$_3$) is a key specie in the understanding of the molecular evolution in star-forming clouds and nitrogen isotope fractionation. In this paper, we present high spatial resolution observations of multiple emission lines of NH$_3$ toward the protobinary system NGC1333 IRAS4A with Karl G. Jansky Very Large Array (VLA). We spatially resolved the binary (hereafter 4A1 and 4A2) and detected compact emission of NH$_3$ transitions with high excitation energies ($\gtrsim$100 K) from the vicinity of the protostars, indicating the NH$_3$ ice has sublimated at the inner hot region. The NH$_3$ column density is estimated to be $\sim 10^{17}-10^{18}$ cm$^{-2}$. We also detected two NH$_2$D transitions, allowing us to constrain the deuterium fractionation of ammonia. The NH$_2$D/NH$_3$ ratios are as high as $\sim 0.3-1$ in both 4A1 and 4A2. From the comparisons with the astrochemical models in the literature, the high NH$_2$D/NH$_3$ ratios suggest that the formation of NH$_3$ ices mainly started in the prestellar phase after the formation of bulk water ice finished, and that the primary nitrogen reservoir in the star-forming cloud could be atomic nitrogen (or N atoms) rather than nitrogen-bearing species such as N$_2$ and NH$_3$. The implications on the physical properties of IRAS4A cores are discussed as well.