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.
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 cosmological scale simulations based on the ΛCDM cosmology. Refer to the following video to know more about the EAGLE simulations:
I work on three projects that address specific scientific questions.
Project I: 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.
Project II: 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 H I flux against line of sight velocity. Despite the contrary expectation, asymmetric H I lines are the norm and in the second project I address the origin of these asymmetries. You can go through the preprint submitted on this work, or view the following seminar which describes the methodology and some earlier results:
Project III: Star formation in galaxies proceeds in dense molecular clouds, which means that the stellar activity in galaxies is primarily governed by the molecular hydrogen content in their interstellar medium. It is well established that the star formation activity of galaxies evolves with cosmic time, and so does their molecular hydrogen. However, the studies based on observed galaxies provide conflicting results on whether the molecular hydrogen content and star formation efficiency of galaxies depends on the environment where these galaxies reside in. It is also not clear whether this dependency changes as the Universe evolves. In the third project, I explore this using galaxies in cosmological hydrodynamical simulations.
You can follow my research at https://www.researchgate.net/profile/Aditya-Manuwal,
or view my LinkedIn profile at http://www.linkedin.com/in/adimanuwal .
I hope you found this interesting. Thanks for coming!
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