Evolution of Chemistry in the envelope of HOt CorinoS (ECHOS)

II. The puzzling chemistry of isomers as revealed by the HNCS/HSCN ratio

¹ Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014 Madrid, Spain
² Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France
³ Centro de Astrobiología (CAB), INTA-CSIC, Carretera de Ajalvir Km. 4, Torrejón de Ardoz, 28850 Madrid, Spain
⁴ Max-Planck-Institut für extraterrestrische Physik, 85748 Garching, Germany
⁵ Physikalish-Meteorologisches Observatorium Davos und Weltstrahlungszentrum (PMOD/WRC), Dorfstrasse 33, 7260 Davos Dorf, Switzerland
⁶ Institut de Ciències de l’Espai (ICE, CSIC), Can Magrans s/n, 08193 Bellaterra, Barcelona, Spain
⁷ Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
⁸ Departamento de Estadística e Investigación Operativa, Facultad de Ciencias Matemáticas, Universidad Complutense de Madrid, Spain
⁹ Joint Center for Ultraviolet Astronomy, Universidad Complutense de Madrid, Avda Puerta de Hierro s/n, 28040, Madrid, Spain

^★ Corresponding author; g.esplugues@oan.es

Received: 16 August 2024
Accepted: 19 October 2024

Abstract

Context. The observational detection of some metastable isomers in the interstellar medium with abundances comparable to those of the most stable isomer, or even when the stable isomer is not detected, highlights the importance of non-equilibrium chemistry. This challenges our understanding of the interstellar chemistry and shows the need to study isomeric forms of molecular species to constrain chemical processes occurring in the interstellar medium.

Aims. Our goal is to study the chemistry of isomers through the sulphur isomer pair HNCS and HSCN, since HSCN has been observed in regions where its stable isomer has not been detected, and the observed HNCS/HSCN ratio seems to significantly vary from cold to warm regions.

Methods. We used the Nautilus time-dependent gas-grain chemical code to model the formation and destruction paths of HNCS and HSCN in different astrochemical scenarios, as well as the time evolution of the HNCS/HSCN ratio. We also analysed the influence of the environmental conditions on their chemical abundances.

Results. We present an observational detection of the metastable isomer HSCN in the Class I object B1-a (N=(1.1±0.6)×10¹² cm⁻²), but not of the stable isomer HNCS, despite HNCS lying 3200 K lower in energy than HSCN. Our theoretical results show an HNCS/HSCN ratio sensitive to the gas temperature and the evolutionary time, with the highest values obtained at early stages (t≲10⁴ yr) and low (T_g≲20 K) temperatures. A more detailed analysis also shows that the main mechanism forming HNCS in young (t<10⁵ yr) and cold (T_g=10 K) objects at moderate-low densities (n_H≤10⁵ cm⁻³) is a grain surface reaction (the chemical desorption reaction N_solid+HCS_solid→HNCS), unlike previous predictions that suggest only gas-phase chemistry for its formation. However, for the formation of its metastable isomer HSCN, over the same time range and physical conditions, we find that both surface and gas-phase reactions (through the ion H₂NCS⁺) play important roles. In warmer (T_g≥50 K) regions, the formation of this isomer pair is only dominated by gas-phase chemistry through the ions H₂NCS⁺ (mainly at low densities) and HNCSH⁺ (mainly at high densities).

Conclusions. The results suggest a different efficiency of the isomerisation processes depending on the source temperature. The progressive decrease of HNCS/HSCN with gas temperature at early evolutionary times derived from our theoretical results indicates that this ratio may be used as a tracer of cold young objects. This work also demonstrates the key role of grain surface chemistry in the formation of the isomer pair HNCS and HSCN in cold regions, as well as the importance of the ions H₂NCS⁺ and HNCSH⁺ in warm/hot regions. Since most of the interstellar regions where HSCN is detected are cold regions (starless cores, Class 0/I objects), a larger sample including sources characterised by high temperatures (e.g. hot cores) are needed to corroborate the theoretical results.