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FDG RESULTS FOR NGC 1090

NGC 1090 is a barred spiral galaxy in the constellation Cetus. This galaxy also has a dominant stellar disk and a less strong gas component. NFDG results for NGC 1090 are described in the figure below: the top panel shows the variable dimension D(R) (red-solid curve) computed with the main NFDG model, and the new mass-dimension function Dm(R) (blue-dashed curve), computed with the NFDG field equation. Both dimensions decrease from D=2.7-3.0 at lower radial distances, to D=2.0-2.2 at larger distances. This is typical NFDG behavior for galactic structures dominated by an axially-symmetric stellar disk component. Bottom panel: NFDG galactic rotation curves compared with SPARC data. There is perfect agreement between the main NFDG D(R) curve (red-solid) and the experimental data. This shows that, if this galaxy behaves as a fractal structure whose dimension D follows the red-solid curve in the top panel, then the resulting NFDG circular velocity curve in the bottom panel (red-solid) will perfectly fit the experimental data, without any need of dark matter. The NFDG Dm(R) curve (blue-dashed) is less effective in fitting the experimental data, but is still a reasonably good fit.

A disk-dominated galaxy, such as NGC 1090, is characterized by a fractional dimension which is very close to D=2. This is due to the axially-symmetric, flattened-disk shape of this galaxy (see also similar galaxies in the NFDG catalog). The gas component is less important for this galaxy. See my fifth paper for a full discussion of this galaxy.

NFDG analysis of NGC 1090. Top panel: variable space dimension D(R) (red-solid curve) and mass-dimension Dm(R) (blue-dashed curve). Bottom panel: NFDG rotation curves (circular velocity vs. radial distance) compared to the original SPARC data. Also shown: MOND (RAR) fit and Newtonian predictions.