diff --git a/Section_Results.tex b/Section_Results.tex
index eb736a3..8d3a7b1 100644
--- a/Section_Results.tex
+++ b/Section_Results.tex
@@ -37,13 +37,6 @@ \section{Results}
 	\end{center}
 \end{figure}
 
-Fig.~\ref{fig:cosmology-params-all} displays the marginal posterior distributions for an extended set of cosmological parameters.  
-We find that the allowed range for the linear galaxy bias,  $b_1$, in each redshift bin (lower two rows), is almost halved with the addition of the weak lensing data. 
-This constraint does not arise, however, from the sensitivity of the galaxy-galaxy lensing observable to galaxy bias (shown to be relatively weak in the CS+GGL contours). 
-Instead, in this analysis, it is a result of the degeneracy breaking in the $\sigma_8$-$\Omega_{\rm m}$ plane, tightening constraints on $\sigma_8$ which, for galaxy clustering, is degenerate with galaxy bias. 
-The improved constraints on galaxy bias do not, however, fold through to improved constraints on $h$, which the weak lensing data adds very little information to. 
-
-
 \begin{figure*}
 	\begin{center}
 		\includegraphics[width=\textwidth]{Parameter_Plots/cosmology/omegam_sigma8_s8_ns_h_a_baryon_a_ia_b1l_b1h_blind_C}
@@ -52,6 +45,12 @@ \section{Results}
 	\end{center}
 \end{figure*}
 
+Fig.~\ref{fig:cosmology-params-all} displays the marginal posterior distributions for an extended set of cosmological parameters.  
+We find that the allowed range for the linear galaxy bias,  $b_1$, in each redshift bin (lower two rows), is almost halved with the addition of the weak lensing data. 
+This constraint does not arise, however, from the sensitivity of the galaxy-galaxy lensing observable to galaxy bias (shown to be relatively weak in the CS+GGL contours). 
+Instead, in this analysis, it is a result of the degeneracy breaking in the $\sigma_8$-$\Omega_{\rm m}$ plane, tightening constraints on $\sigma_8$ which, for galaxy clustering, is degenerate with galaxy bias. 
+The improved constraints on galaxy bias do not, however, fold through to improved constraints on $h$, which the weak lensing data adds very little information to. 
+
 \begin{table*}
 	\begin{center}
 		\caption{The goodness-of-fit of the flat $\Lambda$CDM cosmological model to each of the single and joint probe combinations with cosmic shear, galaxy clustering and galaxy-galaxy lensing (GGL).}