use new elbow plot

paper/methods_agu.tex

@@ -55,7 +55,7 @@ contains \delete{with the} $\nOsix$ the most frequent solar wind ion (heavier th
   For $q_{Fe}$  the error is calculated using error propagation for the individual densities of the charge states. The error of the individual densities are also estimated as $10$\% . For $\nO$ we based the error estimate on the individual counts per time step. In case of the $\log\nO$ charge state the relative error is limited to the $84.9$th percentile that corresponds to the upper bound of a 1$\sigma$ equivalent of the overall error. The resulting upper limit of  $\log\nO$  lies at 44.3~$\%$. This limitation is necessary due to very low counting statistics in parts of the data set which result in substantial and unrealistic errors. We decided against omitting these data points with very high statistical uncertainty, since they systematically occur in very dilute coronal hole wind which is most frequently observed during the solar activity minimum. Therefore, excluding these data points would introduce a bias into the data set by removing this specific type of coronal hole wind.  The $\colage$ is recalculated for each Monte Carlo trial from the respective randomized values of $\n$, $\vsw$, and $\T$.
 \begin{figure}
   \centering
-  \includegraphics[width = 0.9\textwidth]{figs/elbows/elbow_plot__13_new.pdf}
+  \includegraphics[width = 0.9\textwidth]{figs/elbows/elbow_plot__13.pdf}
   \caption{Convergence and cluster quality scores for different numbers of clusters. From top to bottom: the median of the mean inner cluster distance (MICD), the difference of the MICD to the next number of clusters, the Calinski-Harabasz score and the Davies-Bouldin score over the 100 trials of the full parameter combination for $k=2, \dots,13$.  The error bars are based on percentiles corresponding to a $1\sigma$ interval. The last panel shows the maximum number of iterations used by $k$-means for the respective number of clusters. 
  }
   \label{fig:elbow}