# Dark Matter Halo Spin of the Dwarf Galaxy UGC 5288: Insights from Observations, N-body and Cosmological Simulations

**Authors:** Sioree Ansar, Sandeep K Kataria, Mousumi Das  
**arXiv:** [2307.09952](https://arxiv.org/abs/2307.09952)  
**Date:** 2023-07-19  
**Summary page:** https://www.summarizepaper.com/en/paper/2307.09952v1/

## Key points

- Researchers focus on determining the angular momentum of dark matter (DM) halos in galaxies
- Study investigates the dimensionless halo spin of a gas-rich dwarf barred galaxy called UGC5288
- Hybrid method combining observations and modeling techniques is used to estimate the halo spin
- Forward modeling based on observations is done to determine various properties of the galaxy disk
- HI rotation curve is utilized to constrain the DM halo density profile
- Bar properties are used to identify models that represent the observed baryonic disk
- Comparison with TNG50 simulations validates the findings, showing reasonable alignment with median spin profiles of UGC5288 analogues
- Novel approach for estimating DM halo angular momentum by combining observational data with N-Body/SPH simulations
- Findings contribute to understanding dark matter distribution and its impact on galactic dynamics.

## Summary

In this study, researchers focus on the challenging task of determining the angular momentum of dark matter (DM) halos in galaxies. Specifically, they investigate the dimensionless halo spin of a gas-rich dwarf barred galaxy called UGC5288 using N-Body/SPH simulations. To estimate the halo spin, the team employs a hybrid method that combines observations and modeling techniques. The researchers begin by forward modeling various properties of the galaxy disk based on observations. These properties include stellar and gas mass, surface densities, disk scalelengths, bar length, and bar ellipticity. By utilizing the HI rotation curve, they are able to constrain the DM halo density profile. Additionally, they use information about the bar properties to identify models that best represent the observed baryonic disk. To validate their findings, the team compares the halo spin profile obtained from their simulated models with those of similar mass dwarf galaxy analogues in TNG50 simulations. The results show that while there are uncertainties due to evolutionary history of DM halos, their model's halo spin profile aligns reasonably well with median spin profiles of UGC5288 analogues in TNG50 simulations. Overall, this study presents a novel approach for estimating DM halo angular momentum in galaxies by combining observational data with N-Body/SPH simulations. The findings contribute to our understanding of dark matter distribution and its impact on galactic dynamics.