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We investigate the relationship between turbulence and feedback in the OrionA molecular cloud using maps of $^{12}$CO(1-0), $^{13}$CO(1-0) andC$^{18}$O(1-0) from the CARMA-NRO Orion survey. We compare gas statistics withthe impact of feedback in different parts of the cloud to test whether feedbackchanges the structure and kinematics of molecular gas. We use principalcomponent analysis, the spectral correlation function, and the spatial powerspectrum to characterize the cloud. We quantify the impact of feedback withmomentum injection rates of protostellar outflows and wind-blown shells as wellas the surface density of young stars. We find no correlation between shells oroutflows and any of the gas statistics. However, we find a significantanti-correlation between young star surface density and the slope of the$^{12}$CO spectral correlation function, suggesting that feedback may influencethis statistic. While calculating the principal components, we find peaks inthe covariance matrix of our molecular line maps offset by 1-3 km s$^{-1}$toward several regions of the cloud which may be produced by feedback. Wecompare these results to predictions from molecular cloud simulations.

The CARMA-NRO Orion Survey: Statistical Signatures of Feedback in the Orion A Molecular Cloud