Non-Gaussian assembly bias from a semi-analytic galaxy formation model

Abstract

We use $z=1$ mock galaxy catalogues produced with the semi-analytic code GALACTICUS to study the dependence of the non-Gaussian bias parameter $b_{\varphi }$ on the mass assembly history of the host halos. We generate large sets of merger trees and measure the non-Gaussian assembly bias $\Delta b_{\varphi }$ for galaxies selected by color magnitude and emission line luminosities. For galaxies selected by $g-r$ color, we find a large assembly bias consistent with the analysis of Barreira et al. (2020) based on hydro-dynamical simulations of galaxy formation. This effect arises from the fact that a larger value of the normalization amplitude ${\sigma }_8$ implies a faster mass assembly (at fixed halo mass) and, therefore, older and redder galaxies. On the contrary, for galaxies selected by their H$\alpha$ luminosity, we do not detect a significant assembly bias, at least at $z=1$ and in the halo mass range $3\times 10^{10}<M<10^{12}{M}_{\odot }$ considered here. This is presumably due to the fact that emission line strengths are mainly sensitive to the instantaneous star formation rate, which appears to depend weakly on ${\sigma }_8$ at $z=1$. This indicates that the non-Gaussian assembly bias should be less of a concern for future emission line galaxy surveys. We also investigate, for the first time, the sensitivity of the non-Gaussian assembly bias to a change in the parameters of the galaxy formation model that control the AGN and stellar feedback as well as the star formation rate. When these parameters change within a factor of two from their fiducial value, they induce variations up to order unity in the measured $\Delta b_{\varphi }$, but the overall trends with color or luminosity remain the same. However, since these results may be sensitive to the choice of galaxy formation model, it will be prudent to extend this analysis to other semi-analytic models in addition to halo mass and redshift.

arXiv comment11 pages. Comments are welcome

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