It is found that the halo substructures significantly affect the galaxy velocity field. Based on the fractal geometry of the halo, this self-consistent model predicts an NFW-like rotation curve and a scale free power spectrum of the rotation velocity fluctuations....
We show that where the amplitude of the rotation curve is comparable to the characteristic velocities of the interstellar turbulence, pressure support may lead to underestimates of the mass density of the underlying dark matter halo and the inner slope of its density profile. These effects may be...
The rotation curve data for spiral galaxies are consistent with the dark matter distributed in their halo. This dark halo constitutes much of the galaxy’s total mass. All baryonic matter (stars, star clusters, ISM, etc.) are held together by the gravitational potential of this dark matter ha...
The Disk and Dark Halo Mass of the Barred Galaxy NGC 4123. II. Fluid-Dynamical Models We report a dynamical determination of the separate contributions of disk and dark halo masses to the rotation curve of a spiral galaxy. We use fluid-dynam... JA Sellwood,BJ Weiner,TB Williams - 《Astr...
Although questionable with regard to other measurements of the shape of disc galaxy gravitational potentials, this model can accommodate a scenario in which the gravitational mass distribution, as measured via the rotation curve, is confined to a thin plane without requiring a dark matter halo or ...
We present a simple scenario where the formation of galactic bulges was regulated by the dark halo gravity and regulates the growth of the central supermassive black hole. Assuming the angular momentum is low, we suggest that bulges form in a runaway collapse due to the "gravothermal" instabi...
We explore empirical constraints on the statistical relationship between the radial size of galaxies and the radius of their host dark matter halos from z\sim 0.1 z\sim 0.1 --3 using the GAMA and CANDELS surveys. We map dark matter halo mass to galaxy stellar mass using relationships from ab...
The ?attening of the Galactic rotation curve begins in the range 1 < r/kpc < 10, hence the solution (3’) ? ? most likely describes the Galaxy’s halo. This may be veri?ed by calculating the rotational curves in our model. We know already from the estimate (4) that our model ...
The effect of halo substructures on galaxy rotation curves is investigated in this paper using a simple model of dark matter clustering. A dark matter halo density profile is developed based only on the scale free nature of clustering that leads to a statistically self-similar distribution of the...
The non-circular streaming motions in barred galaxies are sensitive to the mass of the bar and can be used to lift the degeneracy between disk and dark matter halo encountered when fitting axisymmetric rotation curves of disk galaxies. In this paper, we present photometric and kinematic ...