Time evolution of o-H₂D⁺, N₂D⁺, and N₂H⁺ during the high-mass star formation process

¹ INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
² INAF, Istituto di Radioastronomia – Italian node of the ALMA Regional Centre (It-ARC), Via Gobetti 101, 40129 Bologna, Italy
³ Chemistry Department, Sapienza University of Rome, P.le A. Moro, 00185 Rome, Italy
⁴ Departamento de Astronomía, Facultad Ciencias Físicas y Matemáticas, Universidad de Concepción, Av. Esteban Iturra s/n Barrio Universitario, Casilla 160, Concepción, Chile
⁵ Centre for Astrochemical Studies, Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching bei München, Germany
⁶ Max-Planck-Institut für Radioastronomie, Auf dem Hügel, 69, 53121 Bonn, Germany
⁷ Centre for Astrophysics and Planetary Science, University of Kent, Canterbury CT2 7NH, UK
⁸ INAF, Istituto di Radioastronomia, Via Gobetti 101, 40129 Bologna, Italy
⁹ Instituto de Radioastronomía y Astrofísica UNAM, Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán, Mexico

^★ Corresponding author; giovanni.sabatini@inaf.it

Received: 25 July 2024
Accepted: 13 November 2024

Abstract

Context. Deuterium fractionation is a well-established evolutionary tracer in low-mass star formation, but its applicability to the high-mass regime remains an open question. In this context, the abundances and ratios of different deuterated species have often been proposed as reliable evolutionary indicators for different stages of the high-mass star formation process.

Aims. In this study, we investigate the role of N₂H+ and key deuterated molecules (o-H₂D⁺ and N₂D⁺) as tracers of the different stages of the high-mass star formation process. We assess whether their abundance ratios can serve as reliable evolutionary indicators.

Methods. We conducted APEX observations of o-H₂D⁺ (1₁₀–1₁₁), N₂H⁺ (4−3), and N₂D⁺ (3−2) in a sample of 40 high-mass clumps at different evolutionary stages, selected from the ATLASGAL survey. Molecular column densities and abundances relative to H₂, X, were derived through spectral line modelling, both under local thermodynamic equilibrium (LTE) and non-LTE conditions.

Results. The o-H₂D⁺ column densities show the smallest deviation from LTE conditions when derived under non-LTE assumptions. In contrast, N₂H⁺ shows the largest discrepancy between the column densities derived from LTE and non-LTE. In all the cases discussed, we found that X(o-H₂D⁺) decreases more significantly with each respective evolutionary stage than in the case of X(N₂D⁺); whereas X(N₂H⁺) increases slightly. Therefore, the validity of the X(o-H₂D⁺)/X(N₂D⁺) ratio as a reliable evolutionary indicator, recently proposed as a promising tracer of the different evolutionary stages, was not observed for this sample. While the deuteration fraction derived from N₂D⁺ and N₂H⁺ clearly decreases with clump evolution, the interpretation of this trend is complex, given the different distribution of the two tracers.

Conclusions. Our results suggest that a careful consideration of the observational biases and beam-dilution effects are crucial for an accurate interpretation of the evolution of the deuteration process during the high-mass star formation process.