Four more galaxies (NGC 5033, NGC 6674, NGC 5055, NGC 1090) were studied with NFDG methods in a recent paper, in relation to the so-called External Field Effect (EFE). While the NFDG theory does not imply the EFE, these four galaxies were modeled like the previous three galaxies and perfect fits to the galactic rotation curves were produced.
We start with NGC 5033, an inclined spiral galaxy. It is located about 38-60 million light-years away, in the constellation Canes Venatici. This galaxy has a very bright central nucleus and a relatively faint disk extending outward in space. NFDG results for NGC 5033 are shown below: the top panel shows the variable dimension D as a function of the radial distance R, computed with NFDG models. This dimension decreases from D=3.0-3.5 at smaller radial distances to D=2.4-2.5 at larger distances. This is typical NFDG behavior for galactic structures with a strong spherically-symmetric bulge, plus a dominating stellar disk. Bottom panel: NFDG galactic rotation curves compared with SPARC data. There is perfect agreement between the main NFDG curve (red-solid) and the experimental data.
The second galaxy is NGC 6674, a barred spiral galaxy in the constellation Hercules. This galaxy also has a strong central bulge component and a dominant stellar disk at larger distances. NFDG results for NGC 6674 are shown below: the top panel shows the variable dimension D as a function of the radial distance R, computed with NFDG models. This dimension decreases from D=3.0 at smaller radial distances to D=2.3-2.4 at larger distances. Again, this is typical NFDG behavior for galactic structures with a strong spherically-symmetric bulge, plus a dominating stellar disk. Bottom panel: NFDG galactic rotation curves compared with SPARC data. There is perfect agreement between the main NFDG curve (red-solid) and the experimental data.
The third galaxy is NGC 5055, a spiral galaxy in the constellation Canes Venatici, also known as Messier 63, or the Sunflower galaxy. This galaxy does not have a central bulge componenent, but just a dominant stellar disk and gas components. NFDG results for NGC 5055 are shown below: the top panel shows the variable dimension D as a function of the radial distance R, computed with NFDG models. This dimension decreases from D=3.0-3.1 at smaller radial distances to D=2.4-2.5 at larger distances. Bottom panel: NFDG galactic rotation curves compared with SPARC data. There is perfect agreement between the main NFDG curve (red-solid) and the experimental data.
The fourth galaxy is NGC 1090, 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 shown below: the top panel shows the variable dimension D as a function of the radial distance R, computed with NFDG models. This dimension decreases from D=3.0-3.4 at smaller radial distances to D=2.1-2.2 at larger distances. Bottom panel: NFDG galactic rotation curves compared with SPARC data. There is perfect agreement between the main NFDG curve (red-solid) and the experimental data.
