Characterization of Line Ratio Variations in Orion A

Abstract Here we use a new method to study the correlation between different molecular emission lines in star-forming molecular dust clouds. This method is applied to maps from the Line Emission as a Tool for Galaxy Observations project ( 12 CO, 13 CO, C 18 O, N 2 H + , CCH, HCN, and CN) in Orion A. Our data shows the correlation properties change within dust clouds in Orion A, suggesting that the physical properties change as well. We are preparing our code and data to be publicly accessible in an online repository.