Determining the Dark Matter Content of Dwarfs and Dwarfs Spheroidal Galaxies in the Local Group Cluster using the CAS Parameters Ungku Ferwani Salwa Ungku Ibrahim 1,2,* , Zamri Zainal Abidin 1 , Norsiah Hashim 1,2 , Mohd Shaiful Rizal Hassan 1 , Zety Sharizat Hamidi 3 and Zainol Abidin Ibrahim 1 1 Department of Physics, Faculty of Science, University of Malaya, 50603 Kuala Lumpur, Malaysia 2 Center for Foundation Studies in Science, University of Malaya, 50603 Kuala Lumpur, Malaysia 3 Faculty of Applied Sciences, Universiti Teknologi MARA, UiTM S.Alam, Selangor, Malaysia *uferwanis@um.edu.my Abstract—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. Keywords-Cosmology, Dark Matter, Radio Astronomy INTRODUCTION By introducing new parameter, known as CAS parameter [1], one can determined the non-parametric structures of dwarf galaxy sample. The CAS parameters are useful for characterizing the structural properties of galaxies using model-independent measurements. We need to review how galaxy structure correlates with physical properties of galaxies in determining the galaxy morphology- redshift relationship. Technically speaking, galaxy morphology correlates with galaxy properties such as luminosities, environment and mass-to-light ratio. Some quantitative measurements of galaxy structure correlates hardly with physical properties but it is impossible to describe all. The light concentration of an evolved stellar population was first to be discovered relates with its luminosity, stellar mass and scale. While the concentration of a galaxy’s light profile correlates with its stellar mass, absolute magnitude and size, in a sense revealing the past formation history of a galaxy, there are several indicators in the structures of galaxies ongoing galaxy formation. For instant, recently it has been shown that the clumpiness of the galaxy’s light distribution correlates with the amount and the location of star formation. The clumpiness is measured by quantifying the fraction of galaxy’s light in the rest-frame B-band in high spatial frequency structures. The ratio between the amount of light in these high spatial frequency structures and total light gives a measure of clumpiness, or star formation. There is also strong relationship between the dynamical state of a galaxy and the presence of a merger. Generally, merging galaxies are asymmetric, while non-mergers are not. This has been shown in numerous ways, including empirical methods and the correlation of internal HI dynamics and asymmetries of stellar distributions. The study of hydrogen line spectral in the 21 cm background is becoming one of the most exciting fields in astrophysics and vast quantity of high profile instruments are being built and designed at present day. Most of these instruments general purpose and are designed to detect neutral hydrogen (HI) in galaxies at around redshifts of 1 or 4 from the epoch of reionization out to redshifts of 10 and beyond. However, the understanding of neutral hydrogen at low redshifts is also of interest and the project we propose will contribute to this area and allow us to build up experience for future studies using these more powerful instruments. Computing the mass (and accurate redshifts) of low redshift galaxy clusters is the main objective of the proposed instrument and this will provide a useful resource for the wider- community especially in Malaysia since it will be the first research- based radio astronomical instrument ever to be built in the country. Onset of the epoch of reionization might be possible to detect using redshifted 2l cm emission. It has been noted also that the spin-temperature prior to reionization can be observed in Cosmic Microwave Background (CMB) at very low frequencies (~ 30-50 MHz) enabling accurate determination of important cosmological parameters. The motivation of this work is however takes a different approach. Mapping of the large-scale structure, after the Proceeding of the 2011 IEEE International Conference on Space Science and Communication (IconSpace) 12-13 July 2011, Penang, Malaysia 978-1-4577-0564-9/11/$26.00 ©2011 IEEE 182