${}^{13}$C isotopic fractionation of HC${}_3$N in two starless cores: L1521B and L134N (L183)

Abstract

We observed the $J=5-4$ rotational lines of the normal species and three ${}^{13}$C isotopologues of HC${}_3$N at the 45 GHz band toward two low-mass starless cores, L1521B and L134N (L183), using the Nobeyama 45 m radio telescope in order to study the main formation pathways of HC${}_3$N in each core. The abundance ratios of the three ${}^{13}$C isotopologues in L1521B are derived to be [H${}^{13}$CCCN]:[HC${}^{13}$CCN]:[HCC${}^{13}$CN] = 0.98 (+- 0.14) : 1.00 : 1.52 (+- 0.16) (1 sigma). The fractionation pattern is consistent with that at the cyanopolyyne peak in Taurus Molecular Cloud-1. This fractionation pattern suggests that the main formation pathway of HC${}_3$N is the neutral-neutral reaction between C${}_2$H${}_2$ and CN. On the other hand, their abundance ratios in L134N are found to be [H${}^{13}$CCCN]:[HC${}^{13}$CCN]:[HCC${}^{13}$CN]= 1.5 (+- 0.2) : 1.0 : 2.1 (+- 0.4) (1 sigma), which are different from those in L1521B. From this fractionation pattern, we propose that the reaction between HNC and CCH is a possible main formation pathway of HC${}_3$N in L134N. We find out that the main formation pathways of the same molecule are not common even in the similar physical conditions. We discuss the possible factors to make a difference in fractionation pattern between L134N and L1521B/TMC-1.

arXiv commentAccepted for publication in ApJ, 11pages, 4 figures, 2 tables

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