Subscribe to the gold package and get unlimited access to Shamra Academy
Register a new userInvestigating Dark Matter and MOND Models with Galactic Rotation Curve Data: Analysing the Gas-Dominated Galaxies
71
0
0.0
(
0
)
Authors
Jonas Petersen
Ask ChatGPT about the research
No Arabic abstract
In this study the geometry of gas dominated galaxies in the SPARC database is analyzed in a normalized $(g_{bar},g_{obs})$-space ($g2$-space), where $g_{obs}$ is the observed centripetal acceleration and $g_{bar}$ is the centripetal acceleration as obtained from the observed baryonic matter via Newtonian dynamics. The normalization of $g2$-space significantly reduce the effect of both random and systematic uncertainties as well as enable a comparison of the geometries of different galaxies. Analyzing the gas-dominated galaxies (as opposed to other galaxies) further suppress the impact of the mass to light ratios. It is found that the overall geometry of the gas dominated galaxies in SPARC is consistent with a rightward curving geometry in the normalized $g2$-space (characterized by $r_{obs}>r_{bar}$, where $r_{bar}=arg max_r[g_{bar}(r)]$ and $r_{obs}=arg max_r[g_{obs}(r)]$). This is in contrast to the overall geometry of all galaxies in SPARC which best approximates a geometry curing nowhere in normalized $g2$-space (characterized by $r_{obs}=r_{bar}$) with a slight inclination toward a rightward curving geometry. The geometry of the gas dominated galaxies not only indicate the true (independent of mass to light ratios to leading order) geometry of data in $g2$-space (which can be used to infer properties on the solution to the missing mass problem) but also - when compared to the geometry of all galaxies - indicate the underlying radial dependence of the disk mass to light ratio.
rate research
Read More
We study geometries of galactic rotation curves from Dark Matter (DM) and Modified Newtonian Dynamics (MOND) models in $(g_{rm bar},g_{rm tot})$-space ($g2$-space) where $g_{rm tot}$ is the total centripetal acceleration of matter in the galaxies and $g_{rm bar}$ is that due to the baryonic (visible) matter assuming Newtonian gravity. The $g2$-space geometries of the models and data from the SPARC database are classified and compared in a rescaled $hat{g}2$-space that reduces systematic uncertainties on galaxy distance, inclination angle and variations in mass to light ratios. We find that MOND modified inertia models, frequently used to fit rotation curve data, are disfavoured at more than 5$sigma$ independent of model details. The Bekenstein-Milgrom formulation of MOND modified gravity compares better with data in the analytic approximation we use. However a quantitative comparison with data is beyond the scope of the paper due to this approximation. NFW DM profiles only agree with a minority of galactic rotation curves. Improved measurements of rotation curves, in particular at radii below the maximum of the total and the baryonic accelerations of the curves are very important in discriminating models aiming to explain the missing mass problem on galactic scales.
Dark Matter (DM) and Modified Newtonian Dynamics (MOND) models of rotationally supported galaxies lead to curves with different geometries in $(g_{N},g_{tot})$-space ($g2$-space). Here $g_{tot}$ is the total acceleration and $g_{N}$ is the acceleration as obtained from the baryonic matter via Newtonian dynamics. In MOND modified inertia (MI) models the curves in $g2$-space are closed with zero area and so curve segments at radii $rgeq r_{N}$ (large radii) and $r< r_{N}$ (small radii) coincide, where $r_{N}$ is the radius where $g_N$ is greatest. In DM models with cored density profiles where $g_{tot}$ is also zero at the galactic centre, the curves are again closed, but the area of the closed curves are in general non-zero because the curve segments at radii $rgeq r_{N}$ and $r<r_{N}$ do not coincide. Finally in DM models with cuspy density profiles such as the NFW profile where $g_{tot}$ is formally non-zero at the galactic origin the curves are open, and again the curve segments at radii $rgeq r_{N}$ and $r< r_{N}$ do not coincide. We develop a test of whether data at small and large radii coincide and investigate rotation curves from the SPARC database in order to discriminate between the above geometries. Due to loosely quantified systematic uncertainties we do not underline the result of the test, but instead conclude that the test illustrates the relevance of this type of analysis and demonstrate the ability to discriminate between the considered DM and MI models in this way.
The Modified Newtonian Dynamics (MOND) paradigm generically predicts that the external gravitational field in which a system is embedded can produce effects on its internal dynamics. In this communication, we first show that this External Field Effect can significantly improve some galactic rotation curves fits by decreasing the predicted velocities of the external part of the rotation curves. In modified gravi
Mass models of 15 nearby dwarf and spiral galaxies are presented. The galaxies are selected to be homogeneous in terms of the method used to determine their distances, the sampling of their rotation curves (RCs) and the mass-to-light ratio (M/L) of their stellar contributions, which will minimize the uncertainties on the mass model results. Those RCs are modeled using the MOdified Newtonian Dynamics (MOND) prescription and the observationally motivated pseudo-isothermal (ISO) dark matter (DM) halo density distribution. For the MOND models with fixed (M/L), better fits are obtained when the constant a$_{0}$ is allowed to vary, giving a mean value of (1.13 $pm$ 0.50) $times$ 10$^{-8}$ cm s$^{-2}$, compared to the standard value of 1.21 $times$ 10$^{-8}$ cm s$^{-2}$. Even with a$_{0}$ as a free parameter, MOND provides acceptable fits (reduced $chi^{2}_{r}$ $<$ 2) for only 60% (9/15) of the sample. The data suggest that galaxies with higher central surface brightnesses tend to favor higher values of the constant a$_{0}$. This poses a serious challenge to MOND since a$_{0}$ should be a universal constant. For the DM models, our results confirm that the DM halo surface density of ISO models is nearly constant at $ rho_{0} R_{C} sim 120 M_{odot} pc^{-2}$. This means that if the (M/L) is determined by stellar population models, ISO DM models are left with only one free parameter, the DM halo central surface density.
We review the~current status of the~study of rotation curve (RC) of the~Milky Way, and~present a~unified RC from the~Galactic Center to the galacto-centric distance of about 100 kpc. The~RC is used to directly calculate the~distribution of the~surface mass density (SMD). We then propose a~method to derive the~distribution of dark matter (DM) density in the~in the~Milky Way using the~SMD distribution. The~best-fit dark halo profile yielded a local DM density of $rho_odot = 0.36pm 0.02$ GeV/cc. We also review the~estimations of the~local DM density in the~last decade, and~show that the~value is converging to a~value at $rho_odot=0.39pm 0.09$ GeV/cc.
Log in to be able to interact and post comments
comments
Fetching comments
Sign in to be able to follow your search criteria
