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Massive stars have a strong impact on their local environments. However, howstellar feedback regulates star formation is still under debate. In thiscontext, we studied the chemical properties of 80 dense cores in the Orionmolecular cloud complex composed of the Orion A (39 cores), B (26 cores), andlambda Orionis (15 cores) clouds using multiple molecular line data taken withthe Korean Very Long Baseline Interferometry Network (KVN) 21-m telescopes. Thelambda Orionis cloud has an H ii bubble surrounding the O-type star lambda Ori,and hence it is exposed to the ultraviolet (UV) radiation field of the massivestar. The abundances of C2H and HCN, which are sensitive to UV radiation,appear to be higher in the cores in the lambda Orionis cloud than those in theOrion A and B clouds, while the HDCO to H2CO abundance ratios show an oppositetrend, indicating a warmer condition in the lambda Orionis cloud. The detectionrates of dense gas tracers such as the N2H+, HCO+, and H13CO+ lines are alsolower in the lambda Orionis cloud. These chemical properties imply that thecores in the lambda Orionis cloud are heated by UV photons from lambda Ori.Furthermore, the cores in the lambda Orionis cloud do not show anystatistically significant excess in the infall signature of HCO+ (1 - 0),unlike the Orion A and B clouds. Our results support the idea that feedbackfrom massive stars impacts star formation in a negative way by heating andevaporating dense materials, as in the lambda Orionis cloud.

Planck Cold Clumps in the lambda Orionis Complex. III. A chemical probe of stellar feedback on cores in the lambda Orionis cloud