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\subsection{Simple CO decomposition}  Many studies to date have found it necessary to decompose CO SLEDs into at least two components (cite some). One (cooler) component usually dominates in the lower-J CO lines while a warmer component dominates in the higher-J CO lines. Further work will do more involved modelling of the CO SLEDS for the BtP Galaxies, however, here we follow a very simple approach in order to estimate a first order cold/warm decomposition.  In order to estimate the cold component for our sample galaxies which have non-uniform J=1,2,3 coverage, coverage (i.e. some galaxies are observed in all three lines, some only in one),  we fix a MW template based upon the \citet{Fixsen_1999} data for the inner Milky Way. Way from the COBE Far Infrared Absolute Spectrophotometer (FIRAS).  However, the J=1 line was not robustly detected by FIRAS. \citet{Yoda_2010} determine a Milky Way J=2 to J=1 ratio based on their J=2 data with the AMANOGAWA telescope and the matched-resolution J=1 data from \citep{Dame_2001}. We thus substitue in a value based upon this observed J=2 to J=1 ratio.  suspect and we substitute the Amanogawa line for it. Furthermore, instead of using the raw data as a template, we fit a RADEX model in order to smooth out irregularities in the template SLED that are just due to meaurement error. We find a best-fit RADEX model to the MW SLED of x, x, x.