deletions | additions       diff --git a/subsubsection_Bispectrum_Bicoherence_SSRO_no__.tex b/subsubsection_Bispectrum_Bicoherence_SSRO_no__.tex  index 0fd0d7c..789a5f2 100644  --- a/subsubsection_Bispectrum_Bicoherence_SSRO_no__.tex  +++ b/subsubsection_Bispectrum_Bicoherence_SSRO_no__.tex 
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Following the analysis of Koch et al. (2015), we generate sets of randomly sampled spatial frequencies that are sampled up to half of the image size (i.e., 127 pixels). %SSRO or do you mean 2.5pc (or the equivalent half size in ''?  For each run, we compute the bicoherence of our integrated intensity maps using the randomly samples sets.   Figure 8 9  depicts the bicoherence matrices for outputs W1T2t0.2 and T2t0. The bicoherence matrix of W1T2t0.2 exhibits a clear signal on the diagonal; this is the trivial case of $k_1=k_2$. However, it exhibits little correlation elsewhere. In contrast, bicoherence maxtrix of T2t0 shows enhanced correlation for large wavenumbers (small scales). In general it contains a significant fraction of pixels above 0.5, i.e., there is fairly widespread correlation. If magnetic waves enhance correlation across scales, the wind shells may break up the volume and, thus, reduce correlation. Although shell expansion may perturb the magnetic field and excite magnetosonic waves, it is difficult to see any direct evidence of this against the initial turbulence (OA14). The comparison of the two bicohence matricies in fact seems to suggest that the shells reduce correlation perhaps by disrupting the propagation of MHD waves. \citet{burkhart10} compute the bispectrum of HI maps of the SMC. They found that the maps of HI column density exhibit more correlation compared to a turbulent Gaussian random field. They also discovered a break around $\sim 160$ parsecs, where the correlation decreases, an signature which they attribute to expanding shells. \citet{burkhart10} also demonstrate that correlation is much higher for super-Alfvenic turbulence ($\mathcal{M}_A =\sqrt{12\pi \rho} \sigma/B> 1$). The Alfven Mach numbers of our outputs range from $\sim 1-5.5$. Since the velocity dispersion, and hence the Alfvenic Mach number, increases for the strong feedback case, we would a priori expect {\it more} correlation. However, we see the opposite. This supports the conclusion that the shells suppress the free propagation of MHD waves and reduce scale coupling.