Nami Sakai et al. 2007 ApJ 663 1174 doi:10.1086/518595
Nami Sakai1, Masafumi Ikeda1, Masaru Morita1, Takeshi Sakai2, Shuro Takano3, Yoshihiro Osamura4 and Satoshi Yamamoto1
Show affiliationsThe 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
/
abundance ratio is determined to be 4.2 ± 2.3 (3 σ). The
/
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
/
ratio is larger than 8.4 (3 σ). This lower limit is considerably larger than the interstellar
/
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.
Issue 2 (2007 July 10)
Received 2007 January 16, accepted for publication 2007 April 2
Nami Sakai et al. 2007 ApJ 663 1174
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