Shock-induced HCNH⁺ abundance enhancement in the heart of the starburst galaxy NGC 253 unveiled by ALCHEMI

¹ Purple Mountain Observatory, and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, 10 Yuanhua Road, Nanjing 210023, PR China
² Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
³ Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 830011 Urumqi, PR China
⁴ Univ Rennes, CNRS, IPR (Institut de Physique de Rennes) – UMR 6251, 35000 Rennes, France
⁵ Nantes Université, CNRS, CEISAM, UMR 6230, 44000 Nantes, France
⁶ National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA
⁷ Department of Astronomy, University of Virginia, PO Box 400325, 530 McCormick Road, Charlottesville, VA 22904-4325, USA
⁸ European Southern Observatory, Alonso de Córdova, 3107, Vitacura, Santiago 763-0355, Chile
⁹ Joint ALMA Observatory, Alonso de Córdova, 3107, Vitacura, Santiago 763-0355, Chile
¹⁰ National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
¹¹ Institute of Astronomy and Astrophysics, Academia Sinica, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan
¹² Department of Astronomy, School of Science, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-1855, Japan
¹³ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
¹⁴ Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, 830011 Urumqi, PR China
¹⁵ Department of Physics, Faculty of Science and Technology, Keio University, 3-14-1 Hiyoshi, Yokohama, Kanagawa 223-8522, Japan
¹⁶ Transdisciplinary Research Area (TRA) ‘Matter’/Argelander-Institut für Astronomie, University of Bonn, Bonn, Germany
¹⁷ Physics and Astronomy, University College London, London, UK
¹⁸ School of Astronomy & Space Science, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, PR China
¹⁹ Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou 311100, PR China

^★ Corresponding author; ygong@pmo.ac.cn

Received: 31 October 2024
Accepted: 26 February 2025

Abstract

Context. Understanding the chemistry of molecular clouds is pivotal to elucidate star formation and galaxy evolution. As one of the important molecular ions, HCNH⁺ plays an important role in this chemistry. Yet, its behavior and significance under extreme conditions, such as in the central molecular zones (CMZs) of external galaxies, are still largely unexplored.

Aims. We aim to reveal the physical and chemical properties of the CMZ in the starburst galaxy NGC 253 with multiple HCNH⁺ transitions to shed light on the molecule’s behavior under the extreme physical conditions of a starburst.

Methods. We employed molecular line data including results for four rotational transitions of HCNH⁺ from the ALMA Comprehensive High-resolution Extragalactic Molecular Inventory (ALCHEMI) large program to investigate underlying physical and chemical processes.

Results. Despite weak intensities, HCNH⁺ emission is widespread throughout NGC 253’s CMZ, which suggests that this molecular ion can effectively trace large-scale structures within molecular clouds. Using the quantum mechanical coupled states’ approximation, we computed rate coefficients for collisions of HCNH⁺ with para-H₂ and ortho-H₂ at kinetic temperatures up to 500 K. Using these coefficients in a non-local-thermodynamic-equilibrium (non-LTE) modeling framework and employing a Monte Carlo Markov chain analysis, we find that HCNH⁺ emission originates from regions with H₂ number densities of ∼ 10^2.80−10^3.55 cm⁻³, establishing HCNH⁺ as a tracer of low-density environments. Our analysis reveals that most of the HCNH⁺ abundances in the CMZ of NGC 253 are higher than all values reported in the Milky Way. We perform static, photodissociation region, and shock modeling, and found that recurrent shocks could potentially account for the elevated HCNH⁺ abundances observed in this CMZ.

Conclusions. We propose that the unexpectedly high HCNH⁺ abundances may result from chemical enhancement, primarily driven by the elevated gas temperatures and cosmic ray ionization rates of shocked, low-density gas in the nuclear starburst regions of NGC 253.