Galaxies in our universe are known to be surrounded by near-spherical halos of dark matter that have a radially decreasing density profile. It has been decades since the evidence for dark matter began to pour in, but it is still not clear what it is or how does it relate to properties of galaxies. I am working under the supervision of Dr. Aaron Ludlow, Dr. Aaron Robotham and Dr. Chris Power on studies aimed at exploring how the properties of galaxies relate to that of the surrounding dark matter halos.
Dynamical state of a dark matter halo refers to the measure of how far away is the dark matter halo from an equilibrium (or relaxed) state. The first project examines whether and how are the dynamical state of dark matter halos and observable properties of galaxies correlated. The 21 cm emission from neutral hydrogen atoms (H I) in galaxies carries combined information about the galaxy dynamics and gas mass distribution. H I line is the representation of 21-cm emission from galaxies in the HI-flux and line-of-sight velocity space. Despite the contrary expectation, asymmetric H I lines are the norm and in the second project I explore the origin of these asymmetries.
Since the interactions between dark matter and baryons are non-linear by nature, we need to model the involved astrophysical processes self-consistently in order to explore this interplay. We use data from the EAGLE suite of hydrodynamical simulations for these projects which are based on the ΛCDM cosmology. Refer to the following video to know more about EAGLE:
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