2023MNRAS.523.3239S

The H₂NC radical is the high-energy metastable isomer of H₂CN radical, which has been recently detected for the first time in the interstellar medium towards a handful of cold galactic sources, besides a warm galaxy in front of the PKS 1830-211 quasar. These detections have shown that the H₂CN/H₂NC isomeric ratio, likewise the HCN/HNC ratio, might increase with the kinetic temperature (T_kin), but the shortage of them in warm sources still prevents us from confirming this hypothesis and shedding light on their chemistry. In this work, we present the first detection of H₂CN and H₂NC towards a warm galactic source, the G+0.693-0.027 molecular cloud (with T_kin > 70 K), using IRAM 30-m telescope observations. We have detected multiple hyperfine components of the $N_{K_\text{a}K_\text{c}} =$ 1₀₁-0₀₀ and 2₀₂-1₀₁ transitions. We derived molecular abundances with respect to H₂ of (6.8 ± 1.3) × 10^–11 for H₂CN and of (3.1 ± 0.7) × 10^–11 for H₂NC, and an H₂CN/H₂NC abundance ratio of 2.2 ± 0.5. These detections confirm that the H₂CN/H₂NC ratio is ≳2 for sources with T_kin > 70 K, larger than the ∼1 ratios previously found in colder cores (T_kin ∼ 10 K). This isomeric ratio dependence on temperature cannot be fully explained with the currently proposed gas-phase formation and destruction pathways. Grain surface reactions, including the H₂NC → H₂CN isomerization, deserve consideration to explain the higher isomeric ratios and H₂CN abundances observed in warm sources, where the molecules can be desorbed into the gas phase through thermal and/or shock-induced mechanisms.