Comparison between the CCM column densities of L1489 EMC and typical CCM rich sources, normalized by the values of TMC-1 (Kaifu et al. 2004; Suzuki et al. 1992). The source names are denoted in the lower-right corner with different colors, including starless cores Serpens South 1a (Serp S1a; Li et al. 2016), L492 (Hirota & Yamamoto 2006; Hirota et al. 2009), L1521B (Suzuki et al. 1992; Hirota et al. 2004), L1498 (Suzuki et al. 1992; Kuiper et al. 1996) and L1544 (Suzuki et al. 1992) as well as WCCC source L1527 (Sakai et al. 2008). The HC₇ N column density of L1544 is derived from that of HC₅N assuming the ratio of HC_2n+1/HC_2n+3 (n = 1,2) is constant (Suzuki et al. 1992). The N(C₃S) of L1527 is deduced from column densities of C₂S and the ratioof the C₃S/C₂S (Sakai et al. 2008; Suzuki et al. 1992).