Toward a Physical Understanding of Galaxy-Halo Alignment

Abstract

We investigate the alignment of galaxy and halo orientations using the TNG300-1 hydrodynamical simulation. Our analysis reveals that the distribution of the 2D misalignment angle ${\theta }_{2D}$ can be well described by a truncated shifted exponential (TSE) distribution with only {\textit{one}} free parameter across different redshifts and galaxy/halo properties. We demonstrate that the galaxy-ellipticity (GI) correlations of galaxies can be reproduced by perturbing halo orientations with the obtained ${\theta }_{2D}$ distribution, with only a small bias ($<3^{\circ }$) possibly arising from unaccounted couplings between ${\theta }_{2D}$ and other factors. We find that both the 2D and 3D misalignment angles ${\theta }_{2D}$ and ${\theta }_{3D}$ decrease with ex situ stellar mass fraction $F_{\mathrm{acc}}$, halo mass $M_{\mathrm{vir}}$ and stellar mass $M_{\ast }$, while increasing with disk-to-total stellar mass fraction $F_{\mathrm{disk}}$ and redshift. These dependences are in good agreement with our recent observational study based on the BOSS galaxy samples. Our results suggest that $F_{\mathrm{acc}}$ is a key factor in determining the galaxy-halo alignment. Grouping galaxies by $F_{\mathrm{acc}}$ nearly eliminates the dependence of ${\theta }_{3D}$ on $M_{\mathrm{vir}}$ for all three principle axes, and also reduces the redshift dependence. For ${\theta }_{2D}$, we find a more significant redshift dependence than for ${\theta }_{3D}$ even after controlling $F_{\mathrm{acc}}$, which may be attributed to the evolution of galaxy and halo shapes. Our findings present a valuable model for observational studies and enhance our understanding of galaxy-halo alignment.

19 pages, 12 figures, Published in ApJ

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