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tokens: an arc and IRS 3 a jet. IRS 3 also exhibits 3–6 cm emission which indicates shock ionization due to the interaction between the jet from IRS 3 and the surrounding gas (Young et al. 2009 ). Finally, in the outflow source L1251A, a collimated molecular outflow was detected with CO J = 2 − 1 line observation by Lee et al. ( 2010 ). The dynamical timescale of this outflow is 5.2 × 10 4 yr assuming an inclination angle of 70° (Lee et al. 2010 ). Spitzer IRAC observations revealed four infrared sources IRS 1–IRS 4. The driving source is IRS 3, a Class 0 object. From this object, a collimated long infrared jet originated. Our observed position is 12 arcsec east and 9 arcsec south to IRS 3 (see Fig. A1 ). The detected strong Spitzer IRAC observations revealed a jet with a bipolar structure extending from north to south though IRS 3. The jet may originate from a paraboloidal shock (Lee et al. 2010 ). About the N-bearing species in these outflows, the average values of x(HC 3 N)/x(HC 5 N) and x(HC 5 N)/x(HC 7 N) are 6.8 and 4.6 respectively, which are both larger than those of the Lup I starless cores and the WCCC source Lup I-1, showing that the abundance of N-bearing species decreases faster with carbon length in these outflows than in starless cores and WCCC sources. The ratio of x(HC 3 N)/x(HC 5 N) is somewhat lower than the median value (8.7) of 16 low-mass protostars detected by Law et al. ( 2018 ). Table 7 shows that in the starless cores, x(C 3 S) is two or more times lower than x(HC 7 N). The x(C 3 S) in the WCCC source Lup I-1 is also three times less than x(HC 7 N). While in the other three outflow sources the x(C 3 S) are 2–5 times of the x(HC 7 N). These results demonstrate that the x(C 3 S)/x(HC 7 N) values for the three outflows are larger than those of starless cores and the WCCC source almost one order of magnitude higher than their average value. 4.3.2 Chemical mechanism of Group JS sources The abnormal high abundance of C 3 S compared with those of nitrogen-bearing CCMs in JS sources has not been seen before. Previous studies revealed that the column densities of C 2 S have good positive correlation with those of HC 3 N and HC 5 N in quiescent dark cores (Suzuki et al. 1992 ). The column densities of C 3 S are 3–5 times lower than those of C 2 S (Suzuki et al. 1992 ; Fuente et al. 1990 ). High C 2 S and C 3 S abundances were found towards Taurus dark clouds, and there is still a good correlation between column densities of C 2 S and HC 5 N. In star formation regions, S-bearing CCMs were at best only marginally detected (Suzuki et al. 1992 ), indicating that the results of our three outflow sources are unusual. WCCC theory was a possible explanation for the large hydrocarbon abundances such as C 4 H and C 6 H present in L1251A (Cordiner et al. 2011 ). However, WCCC cannot explain the abundances of C 3 S in the three outflow sources, since the relative intensities of N- and S-bearing molecules in WCCC sources are close to those in