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\section{Description of the data}  This project uses observations by made by ALMA under project 2012.1.00762.S proposed  by Hirota et al. We used the Quality Assurance, step 2 data (QA2) downloaded from the Japanese Virtual Observatory site, which images the CO(1-0) line at $1.34\times 0.83$ arcsec resolution, corresponding to $29\times 18$ pc at the 4.5 Mpc distance of M83 \citep{Thim_2003}. The imaged data cube has a velocity resolution of 2.57 km~s$^{-1}$. With a median brightness sensitivity of $\sigma=0.89$~K per beam, the data set are ideally suited for the identification and decomposition of GMCs \citep{Rosolowsky_2006}. Through this analysis, we adopt a CO-to-H$_2$ conversion factor of X$_{\mathrm{CO}} = 2\times 10^{20}$~(K~km~s$^{-1}$)$^{-1}$~cm$^{-2}$ \cite{Bolatto_2013}. With this conversion factor, the data cube has a $1\sigma$ mass surface density sensitivity of 9.9 $M_{\odot}~\mathrm{pc}^{-2}$ and a per-beam mass sensitivity of $6\times 10^3~M_{\odot}$.  of 2.6 mm $^{12}$CO(1-0) emission from M83. $^{12}$CO is used Since the Quality Assurance data delivered  as a tracer part  ofH$_2$ and  the size, velocity line width, and luminosity of project do not include total power or short spacing data,  the GMCs can be found resulting image is affected by some negative artifacts  from when  the data \cite{Solomon_1987}. A CO-to-H$_2$ conversion factor of X$_{\mathrm{CO}} = 2\times 10^{20}$~(K~km~s$^{-1}$)$^{-1}$~cm$^{-2}$ was used cleaning process applied  toderive  the mass interferometer maps. These artifacts are most noticable toward the bright emission in the nucleus  ofH$_2$ gas. Assuming  the clouds galaxy. The data  are in virial equilibrium, a virial mass was found also likely missing flux  from the radius and velocity line width \cite{Solomon_1987}. large scale, diffuse CO emission \citep[e.g.,][]{Pety_2013}.