Volume 648, April 2021
|Number of page(s)||17|
|Section||Interstellar and circumstellar matter|
|Published online||20 April 2021|
Carbon-chain molecule survey toward four low-mass molecular outflow sources
Department of Astronomy, Yunnan University, Key Laboratory of Astroparticle Physics of Yunnan Province,
2 Department of Astronomy, School of Physics, Peking University, Beijing 100871, PR China
3 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, PR China
4 CAS Key Laboratory of FAST, National Astronomical Observatories, CAS, Beijing 100012, PR China
5 NAOC-UKZN Computational Astrophysics Centre (NUCAC), University of KwaZulu-Natal, Durban 4000, South Africa
6 Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, PR China
7 Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Urumqi 830011, PR China
Accepted: 5 March 2021
We performed a carbon-chain molecule (CCM) survey toward four low-mass outflow sources, IRAS 04181+2655 (I04181), HH211, L1524, and L1598, using the 13.7 m telescope at the Purple Mountain Observatory (PMO) and the 65 m Tian Ma Radio telescope at the Shanghai Observatory. We observed the following hydrocarbons (C2H, C4H, c–C3H2), HC2n+1N (n = 1, 2), CnS (n = 2, 3), and SO, HNC, N2H+. Hydrocarbons and HC3N were detected in all the sources, except for L1598, which had a marginal detection of C4H and a non-detection of HC3N (J = 2–1). HC5N and CCCS were only detected in I04181 and L1524, whereas SO was only detected in HH211. L1598 exhibits the lowest detection rate of CCMs and is generally regarded to be lacking in CCMs source. The ratio of N(HC3N/N(N2H+)) increases with evolution in low-mass star-forming cores. I04181 and L1524 are carbon-chain-rich star-forming cores that may possibly be characterized by warm carbon-chain chemistry. In I04181 and L1524, the abundant CCCS can be explained by shocked carbon-chain chemistry. In HH211, the abundant SO suggests that SO is formed by sublimated S+. In this study, we also mapped HNC, C4H, c–C3H2, and HC3N with data from the PMO. We also find that HNC and NH3 are concentrated in L1524S and L1524N, respectively. Furthermore, we discuss the chemical differences between I04181SE and I04181W. The co-evolution between linear hydrocarbon and cyanopolyynes can be seen in I04181SE.
Key words: ISM: molecules / ISM: jets and outflows / stars: low-mass / stars: protostars
© ESO 2021
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