http://arxiv.org/abs/2109.05723
We have conducted mapping observations toward the n3 and n5 positions in the NGC\,2264-D cluster-forming region with the Atacama Compact Array (ACA) of the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 3. Observations with 10000 au scale beam reveal the chemical composition at the clump scale. The spatial distributions of the observed low upper-state-energy lines of CH${3}$OH are similar to those of CS and SO, and the HC${3}$N emission seems to be predominantly associated with clumps containing young stellar objects. The turbulent gas induced by the star formation activities produces large-scale shock regions in NGC\,2264-D, which are traced by the CH${3}$OH, CS and SO emissions. We derive the HC${3}$N, CH${3}$CN, and CH${3}$CHO abundances with respect to CH${3}$OH. Compared to the n5 field, the n3 field is farther (in projected apparent distance) from the neighboring NGC\,2264-C, yet the chemical composition in the n3 field tends to be similar to that of the protostellar candidate CMM3 in NGC\,2264-C. The HC${3}$N/CH${3}$OH ratios in the n3 field are higher than those in the n5 field. We find an anti-correlation between the HC${3}$N/CH${3}$OH ratio and their excitation temperatures. The low HC${3}$N/CH$_{3}$OH abundance ratio at the n5 field implies that the n5 field is an environment with more active star formation compared with the n3 field.
K. Taniguchi, A. Plunkett, T. Shimoikura, et. al.
Tue, 14 Sep 21
42/88
Comments: 16 pages, 10 figures, 6 tables, Accepted by Publications of the Astronomical Society of Japan (PASJ)
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