Unveiling the gas phase H₂NCO radical: Laboratory rotational spectroscopy and interstellar searches in the direction of IRAS 16293-2422

¹ Université Paris-Saclay, CNRS, Institut des Sciences Moléculaires d’Orsay, 91405 Orsay, France
e-mail: marie-aline.martin@universite-paris-saclay.fr
² Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, UT3-PS, CNRS, CNES, 9 av. du Colonel Roche, 31028 Toulouse Cedex 4, France
³ Université Bordeaux, CNRS, Institut des Sciences Moléculaires, 33400 Talence, France
⁴ Niels Bohr Institute, University of Copenhagen, Øster Voldgade 5–7, 1350 Copenhagen K., Denmark

Received: 23 February 2024
Accepted: 7 May 2024

Abstract

Context. The carbamoyl radical (H₂NCO) is believed to play a central role in the ice-grain chemistry of crucial interstellar complex organic molecules such as formamide and acetamide. Yet, little is known about this radical, which remains elusive in laboratory gasphase experiments.

Aims. In order to enable interstellar searches of H₂NCO, we have undertaken a mandatory laboratory characterisation of its pure rotational spectrum.

Methods. We report the gas-phase laboratory detection of H₂NCO, produced by H-atom abstraction from formamide, using pure rotational spectroscopy at millimetre and submillimetre wavelengths. Millimetre-wave data were acquired using chirped-pulse Fourier-transform spectroscopy, while submillimetre-wave ones were obtained using Zeeman-modulated spectroscopy. Experimental measurements were guided by quantum-chemical calculations at the ωB97X-D/cc-pVQZ level of theory. Interstellar searches for the radical have been undertaken in the Protostellar Interferometric Line Survey (PILS) towards the solar-type protostar IRAS 16293-2422.

Results. From the assignment and fit of experimental transitions up to 660 GHz, reliable spectroscopic parameters for H₂NCO in its ground vibrational state have been derived, enabling accurate spectral predictions. No transitions of the radical were detected in the PILS survey. The inferred upper limit shows that the H₂NCO abundance is at least 60 times below that of formamide and 160 times below that of HNCO in this source; a value that is in agreement with predictions from a physico-chemical model of this young protostar.