Speaker
Description
In this talk, I will present our analysis of the dark matter halos of nearby LADUMA galaxies, using high-quality HI rotation curves combined with multi-band photometry to separate the contributions of stars, gas, and dark matter to the total mass. By fitting different halo models—including NFW, pseudo-isothermal, and the more flexible generalized NFW profile—I will show how allowing the inner density slope to vary provides a clearer and more physically realistic picture of galaxy mass distributions. I will also discuss how the stellar mass component, constrained through optical and infrared imaging, influences the inferred halo structure and helps us understand whether galaxies are cuspy or core-like in their centers. Together, these results offer new insight into how baryonic processes shape dark matter halos while remaining consistent with ΛCDM expectations.
| Stream | Science or Engineering |
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