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\textit{Oh, an empty article!} \section{Introduction}
Star formation of all mass occurs in molecular clouds. In particular, they are almost exclusively formed in giant molecular clouds (GMCs) with cloud mass >10 M_⨀ [1]. The formation and distribution of molecular clouds then impacts galactic structure and evolution by influencing the formation and distribution of stars [1]. Adamo et al. (2015) studied the distribution of star clusters in M83, a spiral galaxy 4.5 Mpc away. M83 has been extensively analyzed in this regard, but with the fullest to date catalog of clusters Adamo et al. (2015) found the initial cluster mass function followed a power law with slope -2 and had a truncation on the high-mass end that decreased with distance from the center of the galaxy. It is suggested that the galactic environment limits the formation of high mass clusters, possibly due to the limit on the formation of high mass molecular clouds [2]. We are looking at the mass distribution of molecular clouds in M83 to see if the same function is shown as in the stellar clusters.
\section{Description of the data}
This project uses observations by ALMA of 2.6 mm 12CO(1-0) emission from M83. 12CO is used as a tracer of H2 and the size, velocity line width, and luminosity of the GMCs can be found from the data [3]. A CO-to-H2 conversion factor of XCO = 2 "×" 1020 K km s-1 cm2 was used to derive the mass of H2 gas. Assuming the clouds are in virial equilibrium, a virial mass was found from the radius and velocity line width [3].
\section{Analysis}
Analysis
We examined the GMC properties as in Solomon et al. (1987). M83 clouds exhibit similar relationships for velocity line width to radius, which confirms our assumption of the clouds being in virial equilibrium. As well, the virial mass to luminous mass and luminous mass to radius relationships are also consistent with previous findings. We then binned the clouds by equal surface area on the disk as in Adamo et al. (2015), and for each bin examined the cumulative mass function:
\begin{center} $N(>M)=\int^\infty_M \frac{dN}{dM}dM=\frac{\beta M_\odot}{\alpha+1}\left(\frac{M}{M_\odot}\right)^\alpha
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