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Production Pathways of CCS and CCCS Inferred from Their 13C Isotopic Species

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Nami Sakai1, Masafumi Ikeda1, Masaru Morita1, Takeshi Sakai2, Shuro Takano3, Yoshihiro Osamura4 and Satoshi Yamamoto1

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The rotational spectral lines (JN = 32-21 and JN = 21-10) of 13CCS and C13CS have been observed toward a cold dark cloud, TMC-1. The strongest hyperfine component lines of 13CCS and C13CS (JN = 21-10, F = 5/2-3/2) have successfully been detected. The img1.gif / img2.gif abundance ratio is determined to be 4.2 ± 2.3 (3 σ). The img3.gif / img2.gif ratio is evaluated to be 230 ± 130 (3 σ), and hence, 13CCS is found to be significantly diluted. Such a difference between the 13CCS and C13CS abundances is also found in L1521E, which is a very young core with rich carbon-chain molecules. Therefore, the anomaly is not specific to TMC-1, but seems to be common for the CCS-rich clouds. Furthermore, we have also observed the J = 4-3 transition of 13CCCS and CCC34S in TMC-1 and L1521E and have found that the img4.gif / img5.gif ratio is larger than 8.4 (3 σ). This lower limit is considerably larger than the interstellar img6.gif img7.gif / img8.gif img9.gif ratio of 3, indicating that 13CCCS is diluted as in the case of 13CCS. These results give us strong constraints on the main pathways to produce CCS and CCCS.


Subject headings

ISM: molecules; ISM: individual (TMC-1, L1521E)


Dates

Issue 2 (2007 July 10)

Received 2007 January 16, accepted for publication 2007 April 2



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