Shock-induced HCNH+ abundance enhancement in the heart of the starburst galaxy NGC 253 unveiled by ALCHEMI
文献类型：期刊论文
| 作者 | Gong, Y.8,9; Henkel, C.7,9 ; Bop, C. T.5,6; Mangum, J. G.10; Behrens, E.1,10; Du, F. J.8; Zhang, S. B.8; Martin, S.18,19; Menten, K. M.9; Harada, N.15,16,17
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| 刊名 | ASTRONOMY & ASTROPHYSICS
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| 出版日期 | 2025-04-01 |
| 卷号 | 696页码:A31 |
| 关键词 | ISM: clouds ISM: molecules radio lines: ISM ISM: individual objects: NGC 253 |
| ISSN号 | 0004-6361 |
| DOI | 10.1051/0004-6361/202452835 |
| 产权排序 | 3 |
| 英文摘要 | 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. |
| WOS关键词 | RAY IONIZATION RATE ; CENTRAL MOLECULAR ZONE ; STAR-FORMATION ; LINE SURVEY ; WATER-ICE ; NGC-253 ; CLOUDS ; CONSTRAINTS ; EXCITATION ; COLLISIONS |
| 资助项目 | 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研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:001457679200020 |
| 出版者 | EDP SCIENCES S A |
| 资助机构 | 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 |
| 源URL | [http://ir.xao.ac.cn/handle/45760611-7/7557]  |
| 专题 | 恒星形成与演化研究团组 |
| 通讯作者 | Gong, Y. |
| 作者单位 | 1.Univ Virginia, Dept Astron, POB 400325,530 McCormick Rd, Charlottesville, VA 22904 USA 2.Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Peoples R China 3.Zhejiang Lab, Res Ctr Intelligent Comp Platforms, Hangzhou 311100, Peoples R China 4.UCL, Phys & Astron, London, England 5.Nantes Univ, CNRS, CEISAM, UMR 6230, F-44000 Nantes, France 6.Univ Rennes, IPR Inst Phys Rennes, CNRS, UMR 6251, F-35000 Rennes, France 7.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China 8.Chinese Acad Sci, Key Lab Radio Astron, Purple Mt Observ, 10 Yuanhua Rd, Nanjing 210023, Peoples R China 9.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany 10.Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA |
| 推荐引用方式 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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