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Stellar bars in disk galaxies grow by losing angular momentum to theirenvironments, including the Dark Matter (DM) halo, stellar and gas disks, andinteracting satellite galaxies. This exchange of angular momentum during galaxyevolution hints at a connection between bar properties and the DM halo spin$\lambda$ -- the dimensionless form of DM angular momentum. We investigate theconnection of halo spin $\lambda$ and galaxy properties in the presence/absenceof stellar bars, using the cosmological magneto-hydrodynamic TNG50 simulationsat three redshifts $z_r=0, 0.1$ and 1. We estimate the halo spin for barred andunbarred galaxies (bar strength: $0<A_2/A_0<0.7$) at the central regions of theDM halo close to the galaxy disk and far from the disk, close to halo virialradius. At $z_r=0$, strongly barred galaxies ($A_2/A_0>0.4$) reside in DM haloshaving low spin and low specific angular momentum, while unbarred and weaklybarred galaxies ($A_2/A_0<0.2$) are hosted in high spin and high specificangular momentum halos. The inverse correlation between bar strength and halospin is surprising since previous studies show that bars transfer angularmomentum to DM halos. However, the bar strength-halo spin connection is morecomplex at higher redshift ($z_r=1$) with higher halo spin for all galaxiesthan that at $z_r=0$. Using galaxy samples across various DM halo mass ranges,we highlight the importance of sample selection in obtaining meaningfulresults. Investigating the bar--halo connection in further detail is crucialfor understanding the impact of bars on galaxy evolution models.

The stellar bar - dark matter halo connection in the TNG50 simulations