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

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

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007apj...663.1174s&link_type=abstract

The Astrophysical Journal, Volume 663, Issue 2, pp. 1174-1179.

Astronomy and Astrophysics

Astronomy

11

Ism: Molecules, Ism: Individual: Alphanumeric: Tmc-1, Ism: Individual: Alphanumeric: L1521E

Scientific paper

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 [C13CS/[13CCS abundance ratio is determined to be 4.2+/-2.3 (3 σ). The [CCS/[13CCS 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 [CCC34S/[13CCCS ratio is larger than 8.4 (3 σ). This lower limit is considerably larger than the interstellar [12C[34S/[13C[32S 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.

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