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

doi:10.1051/0004-6361/202452835

	Shock-induced HCNH⁺ abundance enhancement in the heart of the starburst galaxy NGC 253 unveiled by ALCHEMI
	Gong, Y.1,2; Henkel, C.2,3 ; Bop, C. T.4,5; Mangum, J. G.6; Behrens, E.6,7; Du, F. J.1; Zhang, S. B.1; Martin, S.8,9; Menten, K. M.2; Harada, N.10,11,12; Bouvier, M.13; Tang, X. D.3,14 ; Tanaka, K.15; Viti, S.13,16,17; Yan, Y. T.2; Yang, W.18; Mao, R. Q.1; Quan, D. H.19
	2025-04-01
Source Publication	ASTRONOMY & ASTROPHYSICS
ISSN	0004-6361
Volume	696 Pages:A31
Contribution Rank	3
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-H-2 and ortho-H(2 )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 H-2 number densities of similar to 102.80-10(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.
Keyword	ISM: clouds ISM: molecules radio lines: ISM ISM: individual objects: NGC 253
DOI	10.1051/0004-6361/202452835
Indexed By	SCI
Language	英语
WOS Keyword	RAY IONIZATION RATE ; CENTRAL MOLECULAR ZONE ; STAR-FORMATION ; LINE SURVEY ; WATER-ICE ; NGC-253 ; CLOUDS ; CONSTRAINTS ; EXCITATION ; COLLISIONS
Funding Project	the Strategic Priority Research Program of the Chinese Academy of Sciences[XDB0800301] ; Strategic Priority Research Program of the Chinese Academy of Sciences[2025PVA0048] ; Chinese Academy of Sciences President's International Fellowship Initiative[811363] ; Chinese Academy of Sciences President's International Fellowship Initiative[A0110413001] ; European Research Council[2023YFA1608002] ; National Key R&D Program of China[12041305] ; NSFC[MOPPEX 833460] ; European Research Council (ERC)[xbzg-zdsys-202212] ; Chinese Academy of Sciences (CAS) Light of West China Program[2022TSY- CLJ0005] ; Tianshan Talent Program of Xinjiang Uygur Autonomous Region[2022D01E06] ; Natural Science Foundation of Xinjiang Uygur Autonomous Region[12403027] ; National Natural Science Foundation of China[2024M751376] ; China Postdoctoral Science Foundation[2024ZB347] ; Jiangsu Funding Programme for Excellent Postdoctoral Talent ; Observatoire des Sciences de l'Univers de Grenoble (OSUG)[2018.1.00162] ; ALMA
WOS Research Area	Astronomy & Astrophysics
WOS Subject	Astronomy & Astrophysics
WOS ID	WOS:001457679200020
Publisher	EDP SCIENCES S A
Funding Organization	the Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Chinese Academy of Sciences President's International Fellowship Initiative ; European Research Council ; National Key R&D Program of China ; NSFC ; European Research Council (ERC) ; Chinese Academy of Sciences (CAS) Light of West China Program ; Tianshan Talent Program of Xinjiang Uygur Autonomous Region ; Natural Science Foundation of Xinjiang Uygur Autonomous Region ; National Natural Science Foundation of China ; China Postdoctoral Science Foundation ; Jiangsu Funding Programme for Excellent Postdoctoral Talent ; Observatoire des Sciences de l'Univers de Grenoble (OSUG) ; ALMA
Citation statistics
Document Type	期刊论文
Identifier	http://ir.xao.ac.cn/handle/45760611-7/7558
Collection	射电天文研究室_恒星形成与演化研究团组
Corresponding Author	Gong, Y.
Affiliation	1.Chinese Acad Sci, Key Lab Radio Astron, Purple Mt Observ, 10 Yuanhua Rd, Nanjing 210023, Peoples R China 2.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany 3.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China 4.Univ Rennes, IPR Inst Phys Rennes, CNRS, UMR 6251, F-35000 Rennes, France 5.Nantes Univ, CNRS, CEISAM, UMR 6230, F-44000 Nantes, France 6.Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA 7.Univ Virginia, Dept Astron, POB 400325,530 McCormick Rd, Charlottesville, VA 22904 USA 8.European Southern Observ, Alonso de Cordova 3107, Santiago 7630355, Vitacura, Chile 9.Joint ALMA Observ, Alonso de Cordova 3107, Santiago 7630355, Vitacura, Chile 10.Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan 11.Acad Sinica, Inst Astron & Astrophys, 11F AS NTU Astron-Math Bldg,1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan 12.Grad Univ Adv Studies SOKENDAI, Sch Sci, Dept Astron, 2-21-1 Osawa, Mitaka, Tokyo 1811855, Japan 13.Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands 14.Chinese Acad Sci, Key Lab Radio Astron, Urumqi 830011, Peoples R China 15.Keio Univ, Fac Sci & Technol, Dept Phys, 3-14-1 Hiyoshi, Yokohama, Kanagawa 2238522, Japan 16.Univ Bonn, Transdisciplinary Res Area TRA Matter Argelander I, Bonn, Germany 17.UCL, Phys & Astron, London, England 18.Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Peoples R China 19.Zhejiang Lab, Res Ctr Intelligent Comp Platforms, Hangzhou 311100, Peoples R China
Recommended Citation GB/T 7714	Gong, Y.,Henkel, C.,Bop, C. T.,et al. Shock-induced HCNH⁺ abundance enhancement in the heart of the starburst galaxy NGC 253 unveiled by ALCHEMI[J]. ASTRONOMY & ASTROPHYSICS,2025,696:A31.
APA	Gong, Y..,Henkel, C..,Bop, C. T..,Mangum, J. G..,Behrens, E..,...&Quan, D. H..(2025).Shock-induced HCNH⁺ abundance enhancement in the heart of the starburst galaxy NGC 253 unveiled by ALCHEMI.ASTRONOMY & ASTROPHYSICS,696,A31.
MLA	Gong, Y.,et al."Shock-induced HCNH⁺ abundance enhancement in the heart of the starburst galaxy NGC 253 unveiled by ALCHEMI".ASTRONOMY & ASTROPHYSICS 696(2025):A31.

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