Chemical Diversity in Three Massive Young Stellar Objects associated with 6.7 GHz CH$_{3}$OH Masers

Abstract: We have carried out observations in the 42$-$46 and 82$-$103 GHz bands with the Nobeyama 45-m radio telescope, and in the 338.2$-$339.2 and 348.45$-$349.45 GHz bands with the ASTE 10-m telescope toward three high-mass star-forming regions containing massive young stellar objects (MYSOs), G12.89+0.49, G16.86$-$2.16, and G28.28$-$0.36. We have detected HC${3}$N including its $^{13}$C and D isotopologues, CH${3}$OH, CH${3}$CCH, and several complex organic molecules (COMs). Combining our previous results of HC${5}$N in these sources, we compare the $N$(HC${5}$N)/$N$(CH${3}$OH) ratios in the three observed sources. The ratio in G28.28$-$0.36 is derived to be $0.091^{+0.109}_{-0.039}$, which is higher than that in G12.89+0.49 by one order of magnitude, and that in G16.86$-$2.16 by a factor of $\sim 5$. We investigate the relationship between the $N$(HC${5}$N)/$N$(CH${3}$OH) ratio and the $N$(CH${3}$CCH)/$N$(CH${3}$OH) ratio. The relationships of the two column density ratios in G28.28$-$0.36 and G16.86$-$2.16 are similar to each other, while HC${5}$N is less abundant when compared to CH${3}$CCH in G12.89+0.49. These results imply a chemical diversity in the lukewarm ($T \sim 20-30$ K) envelope around MYSOs. Besides, several spectral lines from complex organic molecules, including very-high-excitation energy lines, have been detected toward G12.89+0.49, while the line density is significantly low in G28.28$-$0.36. These results suggest that organic-poor MYSOs are surrounded by a carbon-chain-rich lukewarm envelope (G28.28$-$0.36), while organic-rich MYSOs, namely hot cores, are surrounded by a CH$_{3}$OH-rich lukewarm envelope (G12.89+0.49 and G16.86$-$2.16).