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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 component usually dominates in the lower-J CO lines while a warmer and/or denser component dominates in the higher-J CO lines. Further work will perform involved modelling of the CO SLEDS for the BtP Galaxies, however, here we follow a very simple approach in order to estimate how much intensity remains after a simple model to the low-J emission is fit.  In order to estimate the cold component for our sample galaxies which have non-uniform J=1,2,3 coverage (i.e. some galaxies are observed in all three lines, some only in one), we fix fit  a MW fixed low-J template. This  template is  based upon the \citet{Fixsen_1999} data for the inner Milky 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. 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. Using a maximum likelihood fit over a grid with T_{kin}=10-200K, log(n(H_{2}))=2-6 and log(N(CO))=14-18, we find a best fit to the observed MW SLED with with T_{kin}= 94.6 K, log(n(H_{2}))=2.1 and log(N(CO))=16.9 cm^{-2}. We note that these parameters do not well fit at the J=1-0 line, which is underpredicted by the model. The integrated intensities we thus finally use for our low-J MW based template are listed in Table~\ref{tab1}.