Issue |
A&A
Volume 693, January 2025
|
|
---|---|---|
Article Number | A222 | |
Number of page(s) | 11 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/202452270 | |
Published online | 20 January 2025 |
Molecular chemistry induced by a J-shock toward supernova remnant W51C
1
School of Astronomy & Space Science, Nanjing University,
163 Xianlin Avenue,
Nanjing
210023,
China
2
Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N,
allée Geoffroy Saint-Hilaire,
33615
Pessac,
France
3
Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education,
Nanjing
210023,
China
★ Corresponding author; ygchen@nju.edu.cn
Received:
17
September
2024
Accepted:
9
December
2024
Context. Shock waves from supernova remnants (SNRs) strongly affect the physical and chemical properties of molecular clouds (MCs). Shocks propagating into magnetized MCs can be classified into jump or J-shocks and continuous or C-shocks. The molecular chemistry in the re-formed molecular gas behind J-shocks is still only poorly understood. It is expected to provide a comprehensive view of the chemical feedback of SNRs and the chemical effects of J-shocks.
Aims. We conducted a W-band (71.4–89.7 GHz) observation toward a re-formed molecular clump behind a J-shock induced by SNR W51C with the Yebes 40 m radio telescope to study the molecular chemistry in the re-formed molecular gas.
Methods. Assuming local thermodynamic equilibrium (LTE), we estimated the column densities of HCO+, HCN, C2H and o-c-C3H2, and derived their abundance ratio maps with CO. The gas density was constrained by a non-LTE analysis of the HCO+ J = 1–0 line. The abundance ratios were compared with the values in typical quiescent MCs and shocked MCs, and they were also compared with the results of chemical simulations with the Paris-Durham shock code to verify and investigate the chemical effects of J-shocks.
Results. We obtained the following abundance ratios: N(HCO+)/N(CO) ~ (1.0–4.0) × 10−4, N(HCN)/N(CO) ~ (1.8–5.3) × 10−4, N(C2H)/N(CO) ~ (1.6–5.0) × 10−3, and N(o-c-C3H2)/N(CO) ~ (1.2–7.9) × 10−4. The non-LTE analysis suggests that the gas density is nH2 ≳ 104 cm−3. We find that the N(C2H)/N(CO) and N(o-c-C3H2)/N(CO) are higher than typical values in quiescent MCs and shocked MCs by 1–2 orders of magnitude, which can be qualitatively attributed to the abundant C+ and C in the earliest phase of molecular gas re-formation. The Paris-Durham shock code can reproduce, although not perfectly, the observed abundance ratios, especially the enhanced N(C2H)/N(CO) and N(c-C3H2)/N(CO), with J-shocks propagating into both nonirradiated and irradiated molecular gas with a preshock density of nH = 2 × 103 cm−3.
Key words: shock waves / ISM: abundances / ISM: clouds / ISM: molecules / ISM: supernova remnants
© The Authors 2025
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.