dc.description.abstract | Radial Acceleration Relation (RAR) is a relation between the baryonic, and total acceleration of a galaxy. RAR is typically measured on spiral galaxies in literature, so fewer studies have focused on elliptical galaxies. It is important to study the RAR of elliptical galaxies in order to find out whether all galaxies shift towards MOND with a constant acceleration scale. In this work, data of 1266, 4195, and 159 elliptical galaxies were selected from SDSS DR15, UPenn catalog, and ATLAS extsuperscript{3D} respectively. Each of their total accelerations were deduced from their measured velocity dispersion. Since elliptical galaxies are pressure-supported systems, the deduced acceleration depends on the model used. Hernquist model is used for the luminous (or baryonic) part of the elliptical galaxies, and also for both dark matter halo and in Modified Newtonian Dynamics (MOND). The RAR of the SDSS samples were obtained at their effective radius, while the ATLAS extsuperscript{3D} RARs were obtained at multiple binned radii. The results from different models are then compared, including the MOND characteristic acceleration scale $a_0$. A value of $a_0 = lsqSDSSao imes 10^{-10}$ $
icefrac{m}{s^2}$ was calculated from the SDSS samples, $a_0 = lsqUPao imes 10^{-10}$ $
icefrac{m}{s^2}$ from UPenn, and $a_0 = lsqAtlasao imes 10^{-10}$ $
icefrac{m}{s^2}$ from ATLAS extsuperscript{3D}. Based on the results, the elliptical galaxies seem to be a continuation of the spiral galaxies towards Newtonian Dynamics regime, but they follow a different slope. This may be due to the model dependency of elliptical galaxies. | en_US |