# Novel Deep Level Image State Ensemble Enhancement Method for M87 Imaging
## 3 Materials and Methods
By this point, it becomes apparent that the ISEE images vary in detail for Ln and there is an evolution of features one can gather from each generated image as reconstruction deepens. The images begin to converge to the original image while highlighting structures and changing as the process continues. When comparing the Ln ISEE and the ISEE images to the original image, a new world of information emerges from a single image. The implications of these processes for all branches of science that deal with image processing and feature extraction are broad. In Figure 5l, the vortex structure and the outburst structure are apparent in the IR dusty core. \begin{table}
\begin{tabular}{c c c c c c c} \hline \hline \(\tau_{\text{m,n}}\) & \multicolumn{5}{c}{**Image Quality Assessment Metrics ISEE**} \\ \cline{2-7} \(\mathbf{S_{m,n}}\) & **SSIM** & **PSNR** & **MSE** & **NIQE** & **BRISQUE** & **PIQE** \\ \hline Original & 1.00 & NA & NA & 8.22 & 43.38 & 100 \\ \(\tau_{1,44}\) & 0.51 & 20.33 & 603.14 & 5.91 & 37.37 & 43.54 \\ \(\tau_{2,44}\) & 0.38 & 19.34 & 757.28 & 5.97 & 42.52 & 68.82 \\ \(\tau_{3,44}\) & 0.49 & 20.61 & 564.73 & 6.08 & 42.16 & 72.28 \\ \(\tau_{4,44}\) & 0.64 & 22.46 & 369.28 & 6.50 & 42.10 & 68.71 \\ \(\tau_{5,44}\) & 0.76 & 24.50 & 369.28 & 6.73 & 41.59 & 63.23 \\ \(\tau_{6,44}\) & 0.84 & 26.58 & 143.08 & 6.86 & 35.31 & 61.16 \\ S\({}_{1,44}\) & 0.96 & 26.09 & 160.06 & 8.83 & 40.25 & 48.20 \\ S\({}_{2,44}\) & 0.83 & 21.22 & 491.38 & 7.71 & 37.49 & 47.52 \\ S\({}_{3,44}\) & 0.65 & 19.26 & 771.13 & 7.52 & 41.50 & 52.59 \\ S\({}_{4,44}\) & 0.45 & 17.80 & 1079.7 & 7.08 & 42.20 & 51.09 \\ S\({}_{5  
In the structure in Figure 71 on the dusty outer ring, there appears to be a globular mass that is in part feeding the black hole, but as it turns out when examining the overlay of the SST/HST image in Figure 2, there are dusty wisp-like structures, probably from a past ejection from the black hole, that appear to be pushing this matter outward like a bulldozer pushes dirt. So, as it is not feeding on the globular mass, it is most likely ejecting matter and energy particles. According to Table 8, the SSIM and PNSR increase for ISEE \(\tau_{\text{m},46}\) as Ln increases. The MSE decreases and NIQE shows improved quality over that of the original image and the ISED images S\({}_{\text{m},46}\). The PIQE scores are, for the most part, better than the ISEE reconstruction because of the decomposition's removal of the blue-biased glare. The glare is reintroduced in the reconstruction; however, the PIQE for the Ln ISEE images still displays improvement over that of the original image. The ISEE images for \(\tau_{m,47}\) have the highest SSIM and PSNR out of all the presented images. Figure 71 has the closest SSIM to that of the original image. The color range that it isolates has the properties to isolate the vortex, outburst, globular structures, and boundary regions for the shockwaves. \(\tau_{6,47}\) is applied to the overlay of the HST image in Figure A1a-c. The decompositional images of \(\mathrm{S}_{m,47}\) displayed in Table 9 also show a steep drop off in SSIM and PSNR as Ln increases and a rapid rise in MSE. The NIQE and PIQE increase, while the BRISQUE exhibits little variation. On the other hand, the Ln ISEE reconstructions have high SSIM, improved PNSR, and low IMSE. \(\tau_{6,47}\) has an MSE of 6.91 with an SSIM approaching 1. The NIQE and PIQE are also improved over that of the original image. [PERSON] operator uses two \(3\times 3\) kernels that are convolved with the image (A). They are given by the following equations [3]. \[G_{x}=\left[ \begin{array}{ccc}1&0&-1\\ 2&0&-2\\ 1&0&-1\end{array} \right]*A\text{ and }G_{y}=\left[ \begin{array}{ccc}1&2&1\\ 0&0&0\\ -1&-2&-1\end{array}