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Determining the dark matter content of dwarfs and dwarfs spheroidal galaxies in the local group cluster using the CAS parameters

In this paper, we will discuss the CAS parameters (concentration, asymmetry and clumpiness) which are used to determine the non-parametric structures of dwarf samples to calculate the dark matter masses of dwarfs and dwarfs spheroidal galaxies in the Local Group Cluster. Dwarf galaxies are the most numerous galaxies in our Universe and the Milky Way is surrounded by dozens of them. Measuring the dark matter content of dwarf galaxies has mainly been carried out using kinematic measures of individual stars in Local Group systems. However, if the galaxy is perturbed by tides, the assumption that it is in virial equilibrium will be incorrect. A new method which was introduced by Samantha J. Penny et al. (2008) for measuring the dark matter content of dwarf Ellipticals in the Perseus Cluster is based on the radius of the dwarf, the projected distance of the dwarf from the cluster centre and the total mass of the cluster interior to it. We will present this new method and use it to determine the dark matter content of dwarfs and dwarfs spheroidal galaxies in the Local Group. We will also describe our new method in determining Dark Matter Halos content in Galaxy Clusters.