Speaker
Description
Galaxy properties trace the local environment differently. Investigating this correlation provides valuable insights into the importance of considering environmental effects in galaxy formation and evolution models. With the SIMBA cosmological hydrodynamical simulation and observational data, we analyse galaxy clustering as a function of colour, specific star formation rate and age. The clustering is measured with the projected galaxy two-point correlation function $w_p(r_p)$. For a better comparison with observations, we refer to a previous study using BOSS (Baryon Oscillation Spectroscopic Survey) data. Our results agree with the literature at small scales up to $r_p \sim 3\;h^{-1}$Mpc, at $z=0.5$: redder, more quenched and older galaxies cluster more strongly. They are more likely to be found in dense environments. This small-scale galaxy clustering dependence on galaxy properties is mainly due to the small size of the simulation box. At larger scales, the clustering of dark matter haloes significantly influences galaxy clustering. Due to poorly matched data, we do not obtain the clustering powers of the BOSS analysis. Nevertheless, our results still show the expected trends. A larger simulation volume would be necessary for more accurate galaxy clustering measurements.
| Stream | Science |
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