Making a step forward, we here include also the contribution from a dark matter halo in order to see whether this helps in fitting the rotation curve data. As a test case, we consider a sample of spiral galaxies with smooth baryon matter distribution and well-measured circular velocity ...
at which the stars are too faint to determine the rotation curve. TheM/Lratio is close to 30, about the same as that found for the Galaxy. In order to place this result in context, it is necessary to describe the process whereby the rotation curves are determined for extragalactic systems...
We welcome this particular side of their communication as it helps stimulating the effort towards the adoption of better statistical methods in galaxy rotation curves, an effort to which we contributed with Rodrigues {\\it et al.}~2018 (hereafter R18). Indeed, R18 was the first work that, ...
The theory of many-body gravity is now shown to be able to explain the rotation curves of the Milky Way and the M31 (Andromeda) galaxies, to a fair extent. The radial acceleration relation (RAR) for 63 galaxies, with their galactic masses spanning three orders of magnitude, has been ...
Into Astro 42: Galaxy Rotation Curves The LCDM cosmology is widely regarded by the scientific community nowadays as the leading model for the universe. Specifically, in order to explain the discrepancy in galaxy rotation curves, it assumes the existence of dark matter halos around each and every ...
The Luminous Convolution Model (LCM) is an empirical formula, based on a heuristic convolution of Relativistic transformations, which makes it possible to predict the observed rotation curves of a broad class of spiral galaxies from luminous matter alone. Since the LCM is independent of distance ...
The M/L ratio is close to 30, about the same as that found for the Galaxy. In order to place this result in context, it is necessary to describe the process whereby the rotation curves are determined for extragalactic systems. First, one can assume that the disk is radially supported by...
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Using the multiplicity of solutions for the projectable case of the covariant extension of Ho?ava-Lifshitz gravity, we show that an appropriate choice for the auxiliary field allows for an effective description of galaxy rotation curves. This description is based on static and spherically symmetric ...
Rotation curves constrain a galaxy's underlying mass density profile, under the assumption that the observed rotation produces a centripetal force that exactly balances the inward force of gravity. However, most rotation curves are measured using emission lines from gas, which can experience additional...