Figure 3 - available via license: Creative Commons Attribution 4.0 International
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Ratio of the baryon density to the PDM density, ρB/ρ ph , along the radial direction on the equatorial plane, for a disc galaxy with M d = 10 11 M⊙, R d = 3.5 kpc, z d = 0.35 kpc, M b = 10 9 M⊙, and r b = 0.7 kpc. The red dashed line highlights the point at which the two densities have the same value.
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Disc galaxies represent a promising laboratory for the study of gravitational physics, including alternatives to dark matter, owing to the possibility of coupling rotation curves' dynamical data with strong gravitational lensing observations. In particular, Euclid, DES and LSST are predicted to observe hundreds of thousands of gravitational lenses....
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Context 1
... Fig. 2 we show as an example, the distribution of PDM from an edge-on and face-on point of view for a disc galaxy with M d = 10 11 M ⊙ , R d = 3.5 kpc, z d = 0.35 kpc, M b = 10 9 M ⊙ , and r b = 0.7 kpc. For the same galaxy, in Fig. 3 we show the ratio of the baryon density to the PDM density, ρ B /ρ ph , along the radial direction on the equatorial plane. From Fig. 2 we note that the resulting PDM distribution follows the same symmetries of the underlying baryonic matter, as we should expect from Eqn. (7). Moreover, we find it to be always positive definite and ...
Context 2
... B /ρ ph , along the radial direction on the equatorial plane. From Fig. 2 we note that the resulting PDM distribution follows the same symmetries of the underlying baryonic matter, as we should expect from Eqn. (7). Moreover, we find it to be always positive definite and with a shift of its peak concentration w.r.t. to the baryons. Finally, from Fig. 3 we see that the PDM overtakes the baryonic matter as the dominant "matter" component within the very core of the galaxy (below the parsec level) and at large distances from the galactic centre (i.e., approximately at 15 kpc), precisely where we would expect MOND (or DM) effects to dominate the dynamics for this type of ...
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