| Abstract : | It is well known that there is a discrepancy between the observed galaxy rotation curve and the theoretical prediction, which implies the disagreement between the amount of mass inferred from the rotation curves of galaxies and the visible group in the form of stars and gas. Also, other evidence led to introduce the concept of dark matter that interacts with baryonic matter gravitationally. Since then, various Dark Matter halo profiles have been proposed, such as NFW, pseudo-isothermal (pISO), Burkert, etc. Pengfei Li et al. (2020) have studied different halo models for SPARC (Spitzer Photometry & Accurate Rotation Curves) galaxies and found that cored halo models, such as the DC14 and Burkert profiles, generally provide better fits to the rotation curves than the NFW profile. Biswas et al. (in prep) presented 3D kinematic modeling of a pilot sample of eleven galaxies from GARCIA and used Navarro-Frenk-White profile for dark matter halo. We have used the halo profile like pISO and Burket for the samples of GARCIA-I (GMRT archive atomic gas survey). Comparing these results, we can conclude which DM profiles fit best for these GARCIA galaxies. |
